BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Event reconstruction performance with new retro-reflector based de signs for water Cherenkov detectors DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15718@indico.ific.uv.es DESCRIPTION:Speakers: Lukas Berns (Tokyo Institute of Technology)\nWe have proposed the possibility of a cost-efficient way to improve the detector performance for water Cherenkov detectors\, by reflecting the usually lost light falling between photo-detectors onto the other side of the tank wit h retro-reflectors. Using a detector simulation based on optical measureme nts of retro-reflectors\, we developed a convolutional neural network base d reconstruction algorithm. Here we report on the reconstruction performan ce for ring events in the energy scale expected for atmospheric and accele rator neutrinos under various candidate detector configurations.\n\nhttps: //indico.ific.uv.es/event/6178/contributions/15718/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15718/ END:VEVENT BEGIN:VEVENT SUMMARY:Cazadores de materia oscura DTSTART;VALUE=DATE-TIME:20210831T180000Z DTEND;VALUE=DATE-TIME:20210831T190000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16041@indico.ific.uv.es DESCRIPTION:Speakers: David G. Cerdeño (IFT (UAM-CSIC))\nConferencia de d ivulgación en L'Hemisfèric\nCiutat de les Artes i les Ciències de Valè ncia\nhttps://www.cac.es/es/museu-de-les-ciencies/Ciclos-y-conferencias/Ac tualidad/Conferencia-cazadores-de-materia-oscura.html\n\nhttps://indico.if ic.uv.es/event/6178/contributions/16041/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16041/ END:VEVENT BEGIN:VEVENT SUMMARY:First Cherenkov directional detection of sub-MeV solar neutrinos i n Borexino DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15727@indico.ific.uv.es DESCRIPTION:Speakers: Johann Martyn (Borexino\, Johannes Gutenberg-Univers ität Mainz)\nBorexino is a 280t liquid scintillator detector at the Labor atori Nazionali del Gran Sasso (LNGS)\, Italy. Its main goal is the precis ion spectroscopy of solar neutrinos down to energies of ~190 keV and for t his task it features a high radio-purity and a high light yield of ~10\,00 0 scintillation photons per 1 MeV deposited energy. The solar neutrinos ar e measured by their elastic scattering off electrons which induce isotropi cally emitted scintillation photons that are detected by PMTs.\nIn this ta lk we present the first measurement of solar $^{7}$Be neutrinos using the ir associated Cherenkov photons in a high light yield scintillation detect or. In Borexino electrons with E>160 keV produce Cherenkov photons but the ratio of Cherenkov photons from the neutrino scattered electrons is \n\nh ttps://indico.ific.uv.es/event/6178/contributions/15727/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15727/ END:VEVENT BEGIN:VEVENT SUMMARY:Energy-Dependent Neutrino Mixing Parameters at Oscillation Experim ents DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15527@indico.ific.uv.es DESCRIPTION:Speakers: Vedran Brdar (Fermilab and Northwestern University)\ nOne of the most important achievements in the field of particle physics i s the discovery of neutrino oscillations. Despite already awarded Nobel Pr ize\, neutrino oscillation experiments still have a lot to offer\, primari ly the discovery of CP violation in the lepton sector is anticipated. The parameters entering the expression for neutrino oscillation probabilities are neutrino mixing parameters and mass squared differences. In this talk \, we argue that neutrino mixing parameters at production and detection do not necessarily need to be equivalent since such parameters are subject t o renormalization group evolution and the process of neutrino production a nd detection occurs at different energies.In this talk we discuss this in the frame of an UV compete model\; in particular we demonstrate that quan tum effects can yield relevant observable effects at various neutrino expe riments. As an example\, we consider high-energy astrophysical neutrinos a t IceCube and show that neutron decay production mechanism\, that is consi dered to be strongly disfavored by present data\, becomes viable if the si gnificant renormalization group effects are present. We also scrutinize te rrestrial experiments and show that the mismatch of neutrino parameters at production and detection can induce large effects at T2K and NOvA.\n\nhtt ps://indico.ific.uv.es/event/6178/contributions/15527/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15527/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct detection of light dark matter from evaporating primordial black holes DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15816@indico.ific.uv.es DESCRIPTION:Speakers: Marco Chianese (University of Naples Federico II)\nh ttps://indico.ific.uv.es/event/6178/contributions/15816/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15816/ END:VEVENT BEGIN:VEVENT SUMMARY:The Selena Neutrino Experiment DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15467@indico.ific.uv.es DESCRIPTION:Speakers: Alvaro E Chavarria (University of Washington)\nImagi ng sensors made from an ionization target layer of amorphous selenium (aSe ) coupled to a silicon complementary metal-oxide-semiconductor (CMOS) acti ve pixel array for charge readout are a promising technology for neutrino physics. The high spatial resolution in a solid-state target provides unpa ralleled rejection of backgrounds from natural radioactivity in the search for neutrinoless 𝛽𝛽 decay and for solar neutrino spectroscopy with $^{82}$Se. We present results on the ionization response of aSe measured f rom the photoabsorption of 122keV 𝛾 rays in a single-pixel device\, and report on the progress in the fabrication and testing of the first protot ype imaging sensors based on the Topmetal-II pixelated CMOS charge readout chip. We explore the scientific reach of a large neutrino detector with t he proposed technology based on our experimental understanding of the sens or performance.\n\nhttps://indico.ific.uv.es/event/6178/contributions/1546 7/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15467/ END:VEVENT BEGIN:VEVENT SUMMARY:Light Curves of BSM-induced Neutrino Echoes DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15621@indico.ific.uv.es DESCRIPTION:Speakers: Ali Kheirandish (Pennsylvania State University)\nAst rophysical neutrinos present a unique opportunity to search for physics be yond Standard Model. Beyond Standard Model induced interactions of neutrin os during their propagation yield distinct signatures in their observables in neutrino detectors. Energy\, flavor\, arrival direction\, and the arri val time of neutrinos can be modified when new physics is present. In part icular\, new physics scenarios will induce a time delay in the arrival tim e of neutrinos from astrophysical transients. The presence or absence of a delay in the arrival time of neutrinos compared to other cosmic messenger s will provide a powerful probe of new physics in the neutrino sector. In this talk\, we present the light curves for neutrino emission from transie nts for different new physics scenarios and discuss the expected temporal distribution for the arrival time of neutrino in each scenario. We highlig ht the power of time-domain multimessenger astrophysics and discuss the im plications for current and future neutrino detectors.\n\nhttps://indico.if ic.uv.es/event/6178/contributions/15621/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15621/ END:VEVENT BEGIN:VEVENT SUMMARY:Warming Up Cold Inflation DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15664@indico.ific.uv.es DESCRIPTION:Speakers: Saarik Kalia (Stanford University)\nThe axion is a w ell-motivated candidate for the inflaton\, as the radiative corrections th at spoil many single-field models are avoided by virtue of its shift symme try. However\, axions generically couple to gauge sectors. As the axion rolls through its potential\, this coupling can result in the production o f a co-evolving thermal bath\, a situation known as "warm inflation." Inf lationary dynamics in this warm regime can be dramatically altered and res ult in significantly different observable predictions. In this talk\, I w ill show that for large regions of parameter space\, axion inflation model s once assumed to be safely "cold" are in fact warm\, and must be reevalua ted in this context.\n\nhttps://indico.ific.uv.es/event/6178/contributions /15664/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15664/ END:VEVENT BEGIN:VEVENT SUMMARY:New BSM signatures in large scale detectors from terrestrial upsca ttering DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15924@indico.ific.uv.es DESCRIPTION:Speakers: Ryan Plestid (University of Kentucky/Fermilab)\, And rew Gustafson (Virginia Tech)\nIn this talk I will discuss how large volum e detectors can be used to search for new physics generated via up-scatter ing within the Earth itself. The production of new particles can be source d by dark matter\, neutrinos\, or any other particle capable of penetratin g into the Earth's surface. I will focus on neutrino portals and their pro spects at experiments such as Super-Kamiokande\, Borexino and ICECUBE.\n\n https://indico.ific.uv.es/event/6178/contributions/15924/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15924/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic activation of CRESST’s CaWO4 crystals DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15879@indico.ific.uv.es DESCRIPTION:Speakers: Holger Kluck (Vienna Univ of Technology)\nThe CRESST experiment searches for dark matter induced nuclear recoils inside $\\rm CaWO_4$ based cryogenic calorimeters at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy. To reliably identify a potential signal\, a precise understanding of its background budget is crucial.\n\nA potentially impor tant background category are “cosmogenics”: radionuclides produced via interactions with cosmic rays\, mainly during the crystal production at s urface facilities. Albeit $\\rm CaWO_4$ is a well-established calorimetric material\, no systematic study of its susceptibility for cosmic activatio n existed so far.\n\nIn this contribution\, we will first report the expos ure profile of CRESST’s in-house grown $\\rm CaWO_4$ crystals to cosmic rays. Then we will identify the most prominent cosmogenics via ACTIVIA cal culations. Afterwards we discuss the expected background spectrum based on Geant4 simulations and compare it to measurements. Finally\, we give an o utlook on ongoing cross-checks with alternative activation codes.\n\nhttps ://indico.ific.uv.es/event/6178/contributions/15879/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15879/ END:VEVENT BEGIN:VEVENT SUMMARY:A Geant4-based model for the TRISTAN detector DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15711@indico.ific.uv.es DESCRIPTION:Speakers: Andrea Nava (University of Milano-Bicocca)\nThe TRIS TAN project is the upgrade of the KATRIN experiment that aims at searching for sterile neutrino with mass in the keV range through precise measureme nts of the entire Tritium $\\beta$-spectrum. \nIn order to achieve this go al\, the current KATRIN detector must be replaced with a multipixel detect or based on Silicon Drift Detectors (SDDs). SDDs\, with their excellent en ergy resolution and capability of sustaining high count rates\, are common ly used for X-ray spectroscopy. Electron spectroscopy is a relatively nove l application\, it is therefore necessary to characterize SDDs response to electrons. \nTo do this we have started illuminating a single SDD with a monochromatic electron beam coming from a SEM (Scanning Electron Microscop e)\, acquiring data at different energies and angles. We have then realize d a Geant4 simulation of the electron interaction with Silicon\, and we ha ve processed the output with an empirical model that describes SDDs dead-l ayer and depth-dependent charge collection efficiency. By fitting data wit h simulations at different energies and angles we have estimated the free parameters of this empirical model. \nWe have later realized backscatterin g measurements using two SDDs\, one of which operated as a target. We have written a Geant4 simulation of the whole setup and processed its output w ith the best empirical model found with SEM data. The result of this opera tion is a satisfactory description of both the spectra of the two single d etectors and the spectrum obtained by summing the energies released in the two SDDs for coincident events. \nDeriving such a model for electron inte ractions with an SDD is mandatory in order to accurately reconstruct the c ontinuous $\\beta$-spectrum that will be measured in TRISTAN. Moreover\, w e expect that the detector response will be one of the main TRISTAN system atics\, therefore the precise estimation of its parameters allows to prese rve an high sensitivity in the search for the sterile neutrino.\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15711/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15711/ END:VEVENT BEGIN:VEVENT SUMMARY:Concept\, status\, and performance of the AMoRE-I detectors DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15984@indico.ific.uv.es DESCRIPTION:Speakers: Han Beom Kim (Insttitute for Basic Science\, Seoul N ational University)\nAMoRE is an international project to search for neutr inoless double beta decay of $^{100}$Mo with enriched Molybdenum-based cry stals that are instrumented for phonon-scintillation detection. AMoRE-I\, the present phase of the project\, utilizes thirteen $^{48depleted}$Ca$^{1 00}$MoO$_4$ and five Li$_2$$^{100}$MoO$_4$ crystals with a total mass of 6 .2 kg with heat and light detection channels and situated in a dilution re frigerator system located at the Yangyang underground laboratory. The simu ltaneous detection of phonon and scintillation light signals with metallic magnetic calorimeter (MMC) read-outs provides high-quality energy and tim e resolutions and the capability for distinguishing between alpha- and ele ctron-induced events. We will present the performance and preliminary anal ysis results of the AMoRE-I data.\n\nhttps://indico.ific.uv.es/event/6178/ contributions/15984/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15984/ END:VEVENT BEGIN:VEVENT SUMMARY:Annual Modulations of the Angular Recoil-Flux/Energy Distributions of WIMP-Scattered Target Nuclei Observed at an Underground Laboratory DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15921@indico.ific.uv.es DESCRIPTION:Speakers: Chung-Lin Shan (Preparatory Office of the Supporting Center for Taiwan Independent Researchers)\nWhile most direct Dark Matter detection experiments measure only the recoil energies of (elastic) WIMP- nucleus scattering events deposited in underground laboratory detectors\, "directional" DM detection experiments aim to provide 3-dimensional inform ation (recoil tracks and/or head-tail senses) of WIMP-scattered target nuc lei\, as a promising experimental strategy for discriminating WIMP signals from backgrounds. In this talk\, I will first introduce briefly our doubl e-Monte Carlo scattering-by-scattering simulation package for 3-dimensiona l elastic WIMP-nucleus scattering. Then I will demonstrate and compare the "annual modulations" of the angular distributions of the recoil direction (flux)/energy of target nuclei observed in different underground laborato ries. The impacts of the cross section (nuclear form factor) suppression a s well as some common misunderstandings in literature will particularly be discussed in detail.\n\nhttps://indico.ific.uv.es/event/6178/contribution s/15921/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15921/ END:VEVENT BEGIN:VEVENT SUMMARY:New Constraints on Strongly Interacting Sub-GeV Dark Matter via El ectron Scattering from a small Dual-Phase Xenon TPC DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15868@indico.ific.uv.es DESCRIPTION:Speakers: Simon Buse (University of Zurich)\nWe report new res ults on interactions of sub-GeV dark matter particles with electrons using data from a small dual-phase xenon time projection chamber operated at th e Earth's surface [1]. We consider scattering both on electrons and nuclei in the Earth’s crust\, atmosphere\, and shielding materials to compute the attenuation of the dark matter flux by the atmosphere and the [2]. Wit h an exposure of $\\sim15\\\,\\mathrm{g}\\\,\\mathrm{days}$ and based on a n ionisation-only event selection and no background subtraction\, we evalu ate the data in terms of various models\, including interactions mediated by a heavy and ultralight dark photon as well as through an electric dipol e moment [3]. For the case of a heavy dark photon mediator\, we exclude ne w parameter space for dark matter particle masses in the range $100-400\\\ ,\\mathrm{MeV}$.\n\n\n \n [1]: https://arxiv.org/abs/2003.01731v2\n [2] : https://arxiv.org/abs/1905.06348\n [3]: https://arxiv.org/abs/1703.0091 0\n\nhttps://indico.ific.uv.es/event/6178/contributions/15868/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15868/ END:VEVENT BEGIN:VEVENT SUMMARY:Pulse-Shape Discrimination in the DEAP-3600 Single-Phase Liquid-Ar gon Detector DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15855@indico.ific.uv.es DESCRIPTION:Speakers: Chris Jillings (SNOLAB/Laurentian University)\nThe D EAP-3600 detector is a large single-phase liquid-argon detector for WIMP d ark matter. The experiment has run successfully at SNOLAB since 2016 and h as world leading limits for WIMP-argon interactions. We use pulse-shape di scrimination (PSD) to separate electromagnetic events (Ar-39 beta decay\, gamma rays\, ...) from the nuclear recoil events from WIMP-nuclear scatter ing. PSD is effective in liquid argon because the nuclear recoil events ha ve a large density of energy deposition in the argon\, resulting in prefer ential excitation to an Argon eximer singlet state that decays in nanoseco nds\, whereas electromagnetic events have a low density of energy depositi on resulting in excited triplet states that decay in microseconds. We disc uss the scintillation pulse shapes in DEAP-3600 and show our recent analys is of pulse-shape discrimination. At 18 keVee\, we have achieved rejection of EM events with leakage of 1 part in 10^{10} with a nuclear recoil acce ptance of 50%. We present these results and a detailed comparison showing the effectiveness of the prompt-fraction method and the likelihood ratio. We discuss detector effects such as long-lived TPB states and PMT afterpul sing.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15855/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15855/ END:VEVENT BEGIN:VEVENT SUMMARY:Cherenkov Telescope Array sensitivty to branon dark matter models DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15850@indico.ific.uv.es DESCRIPTION:Speakers: Alejandra Aguirre-Santaella (IFT UAM-CSIC)\nTeV DM c andidates are gradually earning more and more attention within the communi ty. Among others\, extra-dimensional brane-world models may produce therma l DM candidates with masses up to 100 TeV\, which could be detected with t he next generation of very-high-energy gamma-ray observatories such as the Cherenkov Telescope Array (CTA). In this work\, we study the sensitivity of CTA to branon DM via the observation of dwarf spheroidal galaxies. We c omputed annihilation cross section values needed to reach a 5σ detection as a function of the branon mass. Additionally\, in the absence of a predi cted DM signal\, we obtained 2σ upper limits on the annihilation cross se ction. These limits lie 1.5−2 orders of magnitude above the thermal reli c cross section value. Yet\, CTA will allow to exclude a significant porti on of the brane tension-mass parameter space in the 0.1−60 TeV branon ma ss range\, and up to tensions of ∼10 TeV. More importantly\, CTA will si gnificantly enlarge the region already excluded by AMS and CMS\, and will provide valuable complementary information to future SKA radio observation s.\n[Based on JCAP 10 (2020) 041\, arXiv:2006.16706]\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/15850/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15850/ END:VEVENT BEGIN:VEVENT SUMMARY:Progress of upgrading alpha-ray imaging detector in low radioactiv ity background DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15840@indico.ific.uv.es DESCRIPTION:Speakers: Hiroshi Ito (Tokyo University of Tokyo)\nWe have bee n developing an alpha-ray detector based on a time-projection-chamber in a low radioactivity background\, in order to image the radioisotope concent ration on the material surface. In underground particle physics\, current detectors are required massive volume of target using ultra-pure material without radioactive impurities. However\, uranium or thorium impurities on the surface of the detector could be reduced fiducial volume and produced background source via emanation radon. In last conference\, we provided t he alpha-ray imaging detector with a sensitivity of a few $10^{-3}$ $\\alp ha$/cm$^2$/hr in 10cm $\\times$ 10cm of effective sample area. In this wor k\, we performed to improve the sensitivity\, and we would present a curre nt status of the upgrading alpha-ray imaging detector.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15840/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15840/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of the quenching factor in NaI(Tl) scintillator for da rk matter search DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15839@indico.ific.uv.es DESCRIPTION:Speakers: Yusuke Urano (Department of Science and Technology\, Tokushima University\, Tokushima\, Tokushima\, Japan)\nThe PICOLON (Pure Inorganic Crystal Observatory for Low energy Neutr(al)ino) experiment is s earching for WIMP dark matter with ultra-pure NaI(Tl) crystals at the unde rground laboratory in Kamioka observatory. Here\, the quenching factor (QF ) is the scintillation light yield ratio of nuclear recoil and electron re coil at the same energy deposit\, and the QF of the NaI(Tl) is required to determine the WIMP sensitivity. \nTo measure QF\, we irradiated NaI(Tl) s cintillator with 2.45-MeV monochromatic neutrons produced by the deuteron- deuteron fusion. Scattered neutrons from NaI(Tl) were detected with liquid scintillator modules placed at scattering angles of 30\, 45\, and 60 degr ee. By removing the backgrounds with the techniques of pulse shape discrim ination (PSD) and time of flight (TOF)\, nuclear recoil spectrum depending on the scattering angle was determined. \nIn this paper\, we report QFs c alculated from the nuclear recoil spectrum and the Geant4 simulation\, com parison with the results of other groups\, and prospects.\n\nhttps://indic o.ific.uv.es/event/6178/contributions/15839/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15839/ END:VEVENT BEGIN:VEVENT SUMMARY:The optical simulation model of the DarkSide-20k Veto detector DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15838@indico.ific.uv.es DESCRIPTION:Speakers: Cenk Turkoglu (AstroCeNT: Particle Astrophysics Scie nce and Technology Centre)\nDarkSide-20k is a rare-event search experiment dedicated to finding signals of dark matter particles. The DarkSide-20k t ime projection chamber detector registers ionisation and scintillation sig nals originating from the particles interacting with the liquid argon dete ctor medium. It is enclosed in a single-phase liquid argon neutron veto ta nk\, equipped with Gd-loaded panels for capturing neutrons. Due to particl e identification and vetoing carried out through the light signal\, it is crucial to maximising the light yield. Light collection efficiency depends on various aspects of the detector\, and particularly for the Veto detect or\, which has a photosensor coverage of the order of a per cent\, the ref lectivity of materials used has a big impact. To quantify the amount of co llected light a comprehensive Geant4 simulation is done\, which uses optic al characterization data. The focus of the talk will be on a detailed desc ription of the optics model for the Veto of the experiment.\n\nhttps://ind ico.ific.uv.es/event/6178/contributions/15838/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15838/ END:VEVENT BEGIN:VEVENT SUMMARY:Sensitivity of the Cherenkov Telescope Array to dark subhalos DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15837@indico.ific.uv.es DESCRIPTION:Speakers: Javier Coronado-Blázquez (IFT UAM CSIC)\nIn this wo rk\, we study the potential of the Cherenkov Telescope Array (CTA) for the detection of Galactic dark matter (DM) subhalos. We focus on low-mass sub halos that do not host any baryonic content and therefore lack any multiwa velength counterpart. If the DM is made of weakly interacting massive part icles (WIMPs)\, these dark subhalos may thus appear in the gamma-ray sky a s unidentified sources. A detailed characterization of the instrumental re sponse of CTA to dark subhalos is performed\, for which we use the ctools analysis software and simulate CTA observations under different array conf igurations and pointing strategies\, such as the scheduled extragalactic s urvey. This\, together with information on the subhalo population as infer red from N-body cosmological simulations\, allows us to predict the CTA de tectability of dark subhalos\, i.e.\, the expected number of subhalos in e ach of the considered observational scenarios. In the absence of detection \, for each observation strategy we set competitive limits to the annihila tion cross section as a function of the DM particle mass. Interestingly\, we find the best constraints to be reached with no dedicated observations\ , by just accumulating exposure time from all scheduled CTA programs and p ointings over the first 10 years of operation. This way CTA will offer the most constraining limits from subhalo searches in the intermediate range between 1 − 3 TeV\, complementing previous results with Fermi-LAT and HA WC at lower and higher energies\, respectively. This work is based on [210 1.10003] and has been developed within the CTA Consortium.\n\nhttps://indi co.ific.uv.es/event/6178/contributions/15837/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15837/ END:VEVENT BEGIN:VEVENT SUMMARY:Development of low-background NaI(Tl) crystals for the COSINE-200 experiment DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15831@indico.ific.uv.es DESCRIPTION:Speakers: Byungju Park (Univ of Science and Technology)\nCOSIN E-100 is a WIMP dark matter search experiment using ultra low-background N aI(Tl) crystals as a goal to revisit DAMA/LIBRA experiment. COSINE-100 is running with a 106 kg array of low-background NaI(Tl) crystals with approx imately 3 counts/kg/day/keV\, which is about three times higher than DAMA/ LIBRA’s crystals. For the unambiguous conclusion of the DAMA/LIBRA's obs ervation\, it is essential to have lower background crystals at least at t he level of the DAMA/LIBRA crystals. The Center for Underground Physics (C UP) has been growing low-background NaI(Tl) crystals since 2018 for COSINE -200\, and succeeded to produce low-background Tl-doped crystals. We also developed crystal machining\, polishing\, and detector assembly techniques as well. Home-made detectors were tested at the Yangyang underground labo ratory. \n\nIn this presentation\, the CUP-grown crystals and their perfor mance will be discussed.\n\nhttps://indico.ific.uv.es/event/6178/contribut ions/15831/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15831/ END:VEVENT BEGIN:VEVENT SUMMARY:The LZ Outer Detector DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15808@indico.ific.uv.es DESCRIPTION:Speakers: Harvey Birch (University of Michigan)\nThe LUX-ZEPLI N (LZ) detector will consist of 7 tonnes (5.6 tonnes fiducial) of liquifie d xenon in a dual-phase Time Projection Chamber (TPC)\, which is sensitive to the nuclear recoil induced by Weakly Interacting Massive Particles (WI MPs). Among the various type of background particles\, neutrons pose a gre at threat to the WIMPs searches due to the indistinguishable nuclear recoi l. The outer detector of LZ is equipped with 17 tonnes of Gadolinium-doped Liquid Scintillator (GdLS) that captures neutrons with very high efficien cy. The LZ outer detector will characterize the external background\, incr easing the fiducial volume of LZ by 70%. I will present the design\, expec ted performance and current status of the LZ outer detector.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15808/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15808/ END:VEVENT BEGIN:VEVENT SUMMARY:A novel method to fabricate electronic substrates of CDEX-100 by a pplying surface modification of low-background polymers DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15797@indico.ific.uv.es DESCRIPTION:Speakers: Shaojun Zhang (China Dark matter EXperiment (CDEX) m ember\, Key Laboratory of Beam Technology of Ministry of Education\, Coll ege of Nuclear Science and Technology\, Beijing Normal University\, China) \nThe detection of rare events requires transmitting the extremely weak si gnal\, in which electronic substrates with low background levels and stron g binding forces are extremely important. Polytetrafluoroethylene (PTFE) a nd its homologue poly (perfluoroethylene\, FEP) are excellent low backgrou nd and high dielectric layers in electronic substrates widely applicated i n rare event detection experiments. For JFET to transmit and amplify weak signals\, they are usually positioned very close to the detector. Therefor e\, electronic substrates are required to be screened out to have low back ground levels\, good adhesion and low-temperature resistance to meet the r equirements of rare event detection experiments.\nSurface modification of dielectric layers with PTFE and FEP is carried out by ion implantation\, t o solve the problem of difficult metallization between polymer and metal l ayers of electronic substrates. The Stopping and Range of Ions in Matter ( SRIM) simulation is used to analyze the implantation depth and ion distrib ution of the surface. A transition layer and electrolytic copper are depos ited on the polymer by the filtered cathode vacuum arc and electrochemical methods\, respectively. The morphology\, active groups and valence bonds are evaluated to determine the microstructure characteristics. Correspondi ngly\, the mainly adhesion mechanism between copper and the dielectric is explained by mechanical anchoring physical action\, chemical bonding and i ntermolecular forces. Furthermore\, γ-ray background of electronic substr ates prepared by us is relatively lower than common commercial devices.\nW e offer a new method to fabricate the direct surface metallization of perf luorinated polymers. The surface modification of polymer is to obtain elec tronic substrates with low background levels and low-temperature resistanc e\, which has good electrical performance\, and is also applied to China D ark matter EXperiment tests.\n\nhttps://indico.ific.uv.es/event/6178/contr ibutions/15797/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15797/ END:VEVENT BEGIN:VEVENT SUMMARY:Using isotopically enriched detectors to perform CEvNS measurement s. DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15721@indico.ific.uv.es DESCRIPTION:Speakers: Gonzalo Sanchez Garcia (CINVESTAV IPN)\nAfter the la test measurement of the CEvNS process with a LAr detector\, it has been sh own that this interaction can be used as a powerful tool to perform tests of both the standard model and new physics scenarios. So far\, one of the biggest challenges to perform precise measurements has been the determinat ion of systematic uncertainties related\, for instance\, to quenching and form factors. We propose the use of several isotopically enriched detecto rs exposed to the same neutrino flux to measure CEvNS with precision. By p erforming a simultaneous measurement with these detectors\, we show that t he correlation between systematic uncertainties can be used to improve the accuracy of the measurement. We illustrate this idea by studying the sens itivity of a specific array of three germanium isotopes to the characteris tic $N^{2}$ dependence of the cross section of this process. The idea is a pplicable to neutrinos coming from Spallation Neutron Sources\, as well as to reactor neutrinos\, and can be extended to other target materials such as silicon and nickel.\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15721/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15721/ END:VEVENT BEGIN:VEVENT SUMMARY:Building low background kton-scale liquid argon time projection ch ambers for physics discovery DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15713@indico.ific.uv.es DESCRIPTION:Speakers: Christopher Jackson (Pacific Northwest National Labo ratory)\nWith radiopurity controls and small design modifications a kton-s cale liquid argon time projection chamber similar to DUNE could be used fo r enhanced low energy physics searches. This includes improved sensitivity to supernova and solar neutrinos\, and even weakly interacting massive pa rticle dark matter. This talk will present initial simulation studies to o ptimize the design and evaluate physics sensitivities. It will also discus s the tools being developed to support a large-scale radiopurity assay cam paign necessary to construct such a detector.\n\nhttps://indico.ific.uv.es /event/6178/contributions/15713/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15713/ END:VEVENT BEGIN:VEVENT SUMMARY:ENUBET: a monitored neutrino beam for the precision era of neutrin o physics DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15708@indico.ific.uv.es DESCRIPTION:Speakers: Fabio Iacob (Univ Padova and INFN-Padova)\nThe ENUBE T experiment\, included in the CERN Neutrino Platform effort as NP06/ENUBE T\, is developing a new neutrino beam based on conventional techniques in which the flux and the flavor composition are known with unprecedented pre cision ($\\mathcal{O}$(1%)). Such a goal is accomplished monitoring the as sociated charged leptons produced in the decay region of the ENUBET facili ty. Positrons and muons from kaon decays are measured by a segmented calor imeter instrumenting the walls of the decay tunnel\, while muon stations a fter the hadron dump can be used to monitor the neutrino component from pi on decays. Furthermore\, the narrow momentum width (\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/15708/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15708/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of 0$\\nu\\beta\\beta$ decay search in KamLAND-Zen800 DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15707@indico.ific.uv.es DESCRIPTION:Speakers: Atsuto Takeuchi (RCNS\, Tohoku University)\nThe Majo rana nature of neutrinos is the key to understand the matter-antimatter as ymmetry in our Universe. For now\, searching for the neutrino-less double beta (0$\\nu\\beta\\beta$) decay is the only realistic way to proof that n eutrinos are Majorana particles.\nThe KamLAND-Zen experiment is 0$\\nu\\be ta\\beta$ decay search with $^{136}$Xe and ultra-low radioactive detector KamLAND. Since 2019\, we have started the KamLAND-Zen800 Phase with 750 kg enriched xenon and are aiming to the first 0$\\nu\\beta\\beta$ decay sear ch in the inverted mass hierarchy. As the background rate is dramatically reduced in Zen800 Phase\, evaluation of the new kind of background –xeno n spallation products– becomes important. \nIn this presentation\, we pr esent the up-to-date status of 0$\\nu\\beta\\beta$ analysis with KamLAND-Z en800\, especially focusing on the method of investigation of xenon spall ation products and plan of near-future update.\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15707/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15707/ END:VEVENT BEGIN:VEVENT SUMMARY:Nuclear de-excitation associated with neutrino-carbon interactions DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15702@indico.ific.uv.es DESCRIPTION:Speakers: Seisho Abe (Tohoku University)\nThe experimental sea rches for supernova relic neutrino are conducted below 30 MeV\, where atmo spheric neutrino interactions are the dominant background. Neutrino intera ctions in this low energy region have a large uncertainty due to complicat ed nuclear effects\, for example\, a momentum distribution of a nucleon in nucleus\, Pauli blocking and de-excitation of a residual nucleus. Sophist icated neutrino event generators GENIE\, NEUT and NuWro provide several mo dels to predict the momentum and Pauli blocking\, however\, they usually d o not treat the de-excitation.\n It is very important to carry out a syste matic study to predict the contribution of de-excitation\, especially for liquid scintillator detectors like KamLAND\, Borexino and JUNO since they are sensitive to measure the spectra of not only gamma-ray\, but also prot on\, neutron\, alpha.\nThis poster will present the study on de-excitation associated with neutrino-carbon interaction using TALYS and Geant4. TALYS which is an open source software package to simulate nuclear reactions is used to calculate branching ratios of gamma\, proton\, neutron and alpha emissions from excited state of residual nucleus. Geant4 is widely-used si mulator\, and especially G4RadioactiveDecay is a smart tool to trace decay chain event by event.\n By combining two softwares\, I predicted various branching ratios and spectra of produced particles via de-excitation.The r elative errors for the branding ratios are also discussed using another es timation which was carried out by using SMOKER. This prediction does not d epend on neutrino event generator\, thus\, the results can be flexibly app lied to the output of all neutrino event generators mentioned above.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15702/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15702/ END:VEVENT BEGIN:VEVENT SUMMARY:The search for neutrinoless positron emitting electron capture of 120Te with CUORE DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15699@indico.ific.uv.es DESCRIPTION:Speakers: Alice Campani (Università degli studi di Genova)\nA novel algorithm for a Bayesian analysis of multi-site rare events\nCUORE (Cryogenic Underground Observatory for Rare Events) is a ton-scale experim ent located at the LNGS with the main scientific goal of searching for neu trinoless double beta decay in $^{130}$Te. The detector consists of $\\mat hrm{TeO}_2$ crystals operated as cryogenic calorimeters. The use of natura l tellurium allows us to search for other isotopes rare decays. The neutri noless positron emitting electron capture of $^{120}$Te (natural abundance 0.09(1)%) has a clear signature from the 511-keV annihilation $\\gamma$ r ays. We present an analysis of this process based on a new algorithm to pe rform the simultaneous spectral fit over five selected decay scenarios. Ea ch scenario is characterized by a set of crystals simultaneously intereste d by a detectable energy release. We describe the background structure mod eling and tests of linearity we performed on the fit algorithm. We present the limit setting sensitivity and preliminary unblinded results of this a nalysis\, accounting for the most important systematic effects.\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15699/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15699/ END:VEVENT BEGIN:VEVENT SUMMARY:Detection prospects for the double-beta decays of $^{124}$Xe DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15697@indico.ific.uv.es DESCRIPTION:Speakers: Christian Wittweg (University of Zürich)\nThe isoto pe $^{124}$Xe is exceedingly rare and long-lived. Still\, its two-neutrino and neutrinoless double-weak decays offer exciting opportunities for neut rino and nuclear physics. The double-weak decays with neutrinos provide co nstraints for nuclear matrix element calculations on the proton-rich side of the nuclear chart [C. Wittweg\, B. Lenardo\, A. Fieguth and C. Weinheim er\, EPJ C 80 (2020) 1161]. What makes $^{124}$Xe special is the theoretic al possibility of three different neutrinoless decay modes – either via double-electron capture in a nuclear resonance\, or involving the emission of one or two positrons. These decays could be a key to understanding the mass and nature of the neutrino as well as the dominance of matter over a ntimatter in the Universe. Together with the observation of neutrinoless d ouble-beta decays in other isotopes\, $^{124}$Xe could allow to disentangl e the underlying decay mechanism. The poster will introduce the neutrinole ss and two-neutrino decays of $^{124}$Xe and discuss the detection prospec ts with upcoming experiments such as LZ\, XENONnT\, nEXO and DARWIN.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15697/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15697/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino masses and leptogenesis in a L_e-L_mu-L_tau based model DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15682@indico.ific.uv.es DESCRIPTION:Speakers: Simone Marciano (Università di Roma\, La Sapienza)\ nWe present a simple extension of the Standard Model with three right-hand ed neutrinos in a SUSY framework\, with an additional U(1) abelian flavor symmetry with a non standard leptonic charge for lepton doublets and arbi trary right-handed charges. We show how it is possible to provide the corr ect prediction for the mixing angles of the PMNS matrix and for the parame ter with a moderate fine tuning. The baryon asymmetry of the Universe is generated via thermal leptogenesis through CP-violating decays of the heav y right-handed neutrinos. We present a detailed numerical solution of the relevant Boltzmann equations accounting for the impact of the distribution of the asymmetry in the three lepton flavors.\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15682/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15682/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark Matter Physics in Neutrino Telescopes and Neutrino Physics in Dark Matter Detectors. DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15678@indico.ific.uv.es DESCRIPTION:Speakers: Andrew Cheek (CP3\, UCL)\nIt is often the case that experiments built with a focus on a specific fundamental question are also sensitive to a wider range of physical phenomena. In this talk I will dis cuss two such cases. First\, I will follow [JCAP 05 (2021) 054][1]\, which assesses what simple dark matter models will be uniquely probed by a Neut rino telescope similar to KM3NeT. Given the existing constraints from $\\g amma$-ray telescopes\, measurements of the cosmic microwave background and direct dark matter detection\, we mention a secluded $U(1)_{L_{\\mu}-L_{\ \tau}}$ model as particularly promising. Secondly\, I will follow [arXiv:2 104.03297][2]\, which describes how detecting solar neutrinos in direct de tection experiments will be vital for distinguishing between possible $U(1 )$ explanations of the anomalous magnetic moment of the muon.\n\n\n [1]: https://inspirehep.net/literature/1849546\n [2]: https://arxiv.org/abs/21 04.03297\n\nhttps://indico.ific.uv.es/event/6178/contributions/15678/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15678/ END:VEVENT BEGIN:VEVENT SUMMARY:Quasi-Dirac neutrinos in the linear seesaw model DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15634@indico.ific.uv.es DESCRIPTION:Speakers: Kevin Monsalvez Pozo (IFIC (CSIC-Univ Valencia))\nWe implement a minimal linear seesaw model (LSM) for addressing the Quasi-Di rac (QD) behaviour of heavy neutrinos\, focusing on the mass regime of $M_ {N} \n\nhttps://indico.ific.uv.es/event/6178/contributions/15634/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15634/ END:VEVENT BEGIN:VEVENT SUMMARY:BSM sources of CP violation at future long baseline experiments DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15633@indico.ific.uv.es DESCRIPTION:Speakers: Alessio Giarnetti (Roma Tre University and INFN)\nNe utrino Oscillations are one of the most important discoveries of the last thirty years. Many experiments looking at neutrinos from different sources were able to measure with a good precision almost all the oscillation par ameters. However\, considering parameters uncertainties\, there is still r oom for the possibility of the presence of Beyond Standard Model (BSM) eff ects. Some of the most studied New Physics scenarios in the Neutrino Oscil lations framework are sterile neutrinos\, Non Standard Interactions and No n Unitarity models. \nWe studied the potentialities of future long baselin e experiments like DUNE to look for BSM sources of CP violation measuring only the CP asymmetries in different oscillation channels. The relatively easiness of the measurement of such quantities\, the large amount of expec ted data and the great performances of LBL experiments could in principle provide a simple but powerful method to search for new physics effects.\n\ nhttps://indico.ific.uv.es/event/6178/contributions/15633/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15633/ END:VEVENT BEGIN:VEVENT SUMMARY:Testing non-standard neutrino interactions in (anti)-electron neut rino disappearance experiments DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15629@indico.ific.uv.es DESCRIPTION:Speakers: Mariano Chaves (Universidade Estadual de Campinas)\n We search for scalar and tensor non-standard interactions using (anti)-ele ctron neutrino disappearance in oscillation data. We found a slight prefer ence for non-zero CP violation\, coming from both tensor and scalar intera ctions. The preference for CP violation is lead by Daya Bay low-energy dat a with a significance that reaches $\\sim1.7\\sigma$ in the global analysi s (and $\\sim2.1\\sigma$ when considering only medium baseline reactors da ta) compared to the standard oscillation scenario.\n\nhttps://indico.ific. uv.es/event/6178/contributions/15629/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15629/ END:VEVENT BEGIN:VEVENT SUMMARY:The Singly-Charged Scalar Singlet as the Origin of Neutrino Masses DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15626@indico.ific.uv.es DESCRIPTION:Speakers: Tobias Felkl (University of New South Wales)\nWe con sider the generation of neutrino masses via a singly-charged scalar single t. Under general assumptions we identify two distinct structures for the n eutrino mass matrix which are realised in several well-known radiative mod els. Either structure implies a constraint for the antisymmetric Yukawa co upling of the singly-charged scalar singlet to two left-handed lepton doub lets\, irrespective of how the breaking of lepton-number conservation is a chieved. The constraint disfavours large hierarchies among the Yukawa coup lings. We study the implications for the phenomenology of lepton-flavour n on-universality\, measurements of the 𝑊-boson mass\, flavour violation in the charged-lepton sector and decays of the singly-charged scalar singl et. We also discuss the parameter space that can address the Cabibbo Angle Anomaly.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15626/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15626/ END:VEVENT BEGIN:VEVENT SUMMARY:Electromagnetic effects in elastic neutrino scattering on nucleons and nuclei DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15619@indico.ific.uv.es DESCRIPTION:Speakers: Fedor Lazarev (Moscow State University)\nElectromagn etic properties of neutrinos can be a manifestation of new physics [1].\nW e study the electromagnetic contribution to elastic neutrino-nucleon and\n neutrino-nucleus scattering processes. Following our approach developed fo r the\ncase of elastic neutrino-electron [2] and neutrino-proton [3] colli sions\, in our\nformalism we account for possible electromagnetic form fac tors of massive\nneutrinos: the charge\, magnetic\, electric\, and anapole form factors of both diagonal\nand transition types. When treating the nu cleon electromagnetic vertex\, we take\ninto account not only the charge a nd magnetic form factors of a nucleon\, but also\nits electric and anapole form factors. We examine how the effects of the neutrino\nelectromagnetic properties (in particular\, charge radii and magnetic moments) can\nbe di sentangled from those of the strange quark contributions to the nucleon’ s\nweak neutral current form factors. We also study how the neutrino elect romagnetic\nform factors can reveal themselves in coherent elastic neutrin o-nucleus scattering.\nFor illustration\, we present our results in the ca se of the 40Ar nuclear target and\nneutrino energies typical for the COHER ENT experiment.\n\nThis work is supported by Scientific and Educational Sc hool of Moscow State\nUniversity “Fundamental and Applied Space Research ” and by the Russian\nFoundation for Basic Research under grant no. 20-5 2-53022-GFEN-A.\n\n[1] C. Giunti and A. Studenikin\, Neutrino electromagne tic interactions: A window\nto new physics\, Rev. Mod. Phys. 87\, 531 (201 5)\, arXiv:1403.6344.\n[2] K. Kouzakov and A. Studenikin\, Electromagnetic properties of massive\nneutrinos in low-energy elastic neutrino-electron scattering\, Phys. Rev. D 96\,\n099904 (2017)\, arXiv:1703.00401.\n[3] K. Kouzakov\, F. Lazarev\, and A. Studenikin\, Electromagnetic neutrino\ninte ractions in elastic neutrino-proton scattering\, PoS (ICHEP2020) 205\n\nht tps://indico.ific.uv.es/event/6178/contributions/15619/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15619/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino magnetic moments in low-energy neutrino scattering on con densed matter systems DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15616@indico.ific.uv.es DESCRIPTION:Speakers: Georgy Donchenko (Lomonosov Moscow State Univ)\nNeut rino scattering on condensed matter systems at low-energy transfer can ser ve both as a tool for searching the BSM physics\, for example\, such as ne utrino electromagnetic interactions [1]\, and as a test of the Standard Mo del at low-energy scale [2]. In the case of low-energy elastic neutrino sc attering by electrons and nuclei in a liquid or a solid target\, it is nec essary to take into consideration collective effects in the electron and n uclear subsystems of the target. We develop the corresponding theoretical apparatus which is based on the formalism of the density-density and curre nt-current Green’s functions. Calculations in the case of a superfluid H e-4 target are presented to show the roles of neutrino magnetic moments an d collective excitations. Our results can be used in the search of neutrin o electromagnetic interactions in future low-energy neutrino scattering ex periments with liquid or solid targets [2].\n\nThis research has been supp orted by the Interdisciplinary Scientific and Educational School of Moscow University “Fundamental and Applied Space Research” and also by the R ussian Foundation for Basic Research under Grant No. 20-52-53022-GFEN-a. T he work of GD is supported by the BASIS Foundation No. 20-2-9-9-1.\n\n[1] C. Giunti and A. Studenikin\, Rev. Mod. Phys. 87\, 531 (2015) [arXiv:1403. 6344 [hep-ph]].\n[2] M. Cadeddu\, F. Dordei\, C. Giunti\, K. Kouzakov\, E. Picciau\, and A. Studenikin\, Phys. Rev. D 100\, 073014 (2019) [arXiv:1 907.03302 [hep-ph]].\n\nhttps://indico.ific.uv.es/event/6178/contributions /15616/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15616/ END:VEVENT BEGIN:VEVENT SUMMARY:Dirac and Majorana neutrino oscillations in magnetized moving and polarized matter DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15613@indico.ific.uv.es DESCRIPTION:Speakers: Vadim Shakhov (Physical faculty of Moscow state univ ersity)\nIt was shown for the first time in [1] that neutrino spin and spi n-flavor oscillations can be engendered by weak interactions of neutrinos with a medium in the case when there are the transversal matter currents o r transversal matter polarization. The existence of these effects was conf irmed in [2]. In [3\,4] we developed the quantum treatment of these phenom ena and different possibilities for the resonance amplification of oscilla tions were discussed\, the neutrino standard and also non-standard interac tions were accounted for. In the present paper we further develop the quan tum theory of neutrino spin and spin-flavour oscillations in moving magnet ized matter with a special focus on the effects of matter polarization. Bo th the case of Dirac and Majorana neutrinos are considered. As an astrophy sical application we consider the effect of the electron matter component polarization generated by strong magnetic field of a neutron star. This re search has been supported by the Interdisciplinary Scientific and Educatio nal School of Moscow University “Fundamental and Applied Space Research ” and also by the Russian Foundation for Basic Research under Grant No. 20-52-53022-GFEN-a.\n[1] A. Studenikin\, Neutrinos in electromagnetic fiel ds and moving media\, Phys. At. Nucl. 67 (2004) 993. \n[2] A. Kartavtsev\, G. Raffelt\, H. Vogel\, Neutrino propagation in media: Flavor\, helicity \, and pair correlations\, Phys. Rev. D 91 (2015) 125020.\n[3] P. Pustoshn y\, A. Studenikin\, Neutrino spin and spin-flavor oscillations in transver sal matter currents with standard and non-standard interactions\, Phys.Rev . D98 (2018) 113009. \n[4] P. Pustoshny\, V. Shakhov\, A. Studenikin\, Neu trino spin and spin-flavor oscillations in matter currents and magnetic fi elds\, PoS EPS-HEP2019 (2020) 429.\n\nhttps://indico.ific.uv.es/event/6178 /contributions/15613/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15613/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino quantum decoherence engendered by neutrino decay to photo ns\, familons and gravitons DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15610@indico.ific.uv.es DESCRIPTION:Speakers: Alexey Lichkunov (Lomonosov Moscow State University) \nThe phenomenon of neutrino oscillations emerges due to coherent superpos ition of neutrino mass states. An external environment can modify a neutri no evolution in a way that the coherence will be violated. Such a violatio n is called quantum decoherence of neutrino mass states and leads to the s uppression of flavor oscillations. In our previous studies (see [1] and re ference therein) we presented a new theoretical framework\, based on the q uantum field theory of open systems and applied it to the problem of neutr ino evolution. In the present paper we present the generalized framework t hat enables one to consider quantum decoherence of neutrino mass states en gendered by a neutrino decay to a lighter neutrino and a massless particle . We apply this framework to consider mechanisms of the neutrino quantum d ecoherence engendered by neutrino decay to photons\, familons and graviton s. The obtained results are of interest for experiments with reactor and a strophysical neutrinos.\nThis research has been supported by the Interdisc iplinary Scientific and Educational School of Moscow University “Fundame ntal and Applied Space Research” and also by the Russian Foundation for Basic Research under Grant No. 20-52-53022-GFEN-a. The work of KS is also supported by the RFBR under grant No. 20-32-90107 and by the “BASIS” F oundation No. 20-2-2-3-1. The work of MV is also supported by the “BASIS ” Foundation No. 20-2-1-25-1.\n\n[1] K.Stankevich\, A.Studenikin\, Neutr ino quantum decoherence engendered by neutrino radiative decay\, Phys. Rev . D 101 (2020) 056004.\n\nhttps://indico.ific.uv.es/event/6178/contributio ns/15610/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15610/ END:VEVENT BEGIN:VEVENT SUMMARY:Setting limits on heavy neutral leptons using the neutrino CC even ts at the DUNE Near Detector. DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15607@indico.ific.uv.es DESCRIPTION:Speakers: Saneli Alcides Carbajal Vigo (Pontificia Universidad Católica del Perú)\nWe study the impact of production of heavy neutral leptons (HNL) from meson decays on the number of neutrino charged current (CC) events that will be detected at the DUNE ND LArTPC. If the masses of the HNLs are below the kaon mass\, then a decreased number of CC events at the DUNE LArTPC will be observed. This decrease is used to set upper limi ts on the mixing parameters of the HNLs. We find that these limits are at least 1 order of magnitude better than the current ones for masses below 1 MeV for a year of operation in neutrino mode.\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15607/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15607/ END:VEVENT BEGIN:VEVENT SUMMARY:Primordial black holes and scotogenic dark matter DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15606@indico.ific.uv.es DESCRIPTION:Speakers: Teruyuki Kitabayashi ()\nWe study the effect of the scotogenic dark matter on the primordial black holes (PBHs) and vice versa . We show that if the PBHs evaporate in the radiation dominant era\, the u pper limit of the initial mass of the PBHs M_{in} should be constrained as 10^4 10^9 GeV for M_{in}/M_{Pl} \\sim 10^{13} may be allowed. This talk based on arXiv:2101.01921v3 (to be published in International journal of m odern physics A).\n\nhttps://indico.ific.uv.es/event/6178/contributions/15 606/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15606/ END:VEVENT BEGIN:VEVENT SUMMARY:Icecube PeV events and NSI: Role of Charged Higgs DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15599@indico.ific.uv.es DESCRIPTION:Speakers: Soumya Sadhukhan (Ramakrishna Mission Residential Co llege\, Kolkata\, India and Vivekananda Centre for Research)\nExtensions o f the Standard Model with charged Higgs\, having a non-negligible coupling with neutrinos\, can have interesting implications vis-à-vis neutrino ex periments. Such models can leave their footprints in the ultra-high energy neutrino detectors like IceCube in the form of neutrino non-standard inte ractions (NSIs) which can also be probed in lower energy neutrino experime nts. We consider a model based on the neutrinophilic two-Higgs doublets an d study its imprints in the recently reported excess neutrino events in th e PeV energy bins at the IceCube. An additional signature of the model is that it also leads to sizeable NSIs. We perform a combined study of the la test IceCube data along with various other constraints arising from neutri no experiments e.g.\, Borexino\, TEXONO\, COHERENT\, DUNE\, and T2HK\, tog ether with the limits set by the LEP experiment\, and explore the paramete r space which can lead to a sizeable NSI.\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15599/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15599/ END:VEVENT BEGIN:VEVENT SUMMARY:LAPPD deployment in the ANNIE experiment DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15597@indico.ific.uv.es DESCRIPTION:Speakers: Venkatesh Veeraraghavan (Iowa State University)\nThe Accelerator Neutrino Neutron Interaction Experiment (ANNIE) experiment is a 26-ton gadolinium-loaded water Cherenkov detector located on the Booste r Neutrino Beam at Fermilab. The experiment has a two-fold motivation: to perform a physics measurement and to advance new detector technologies. Th e measurement of final state neutron multiplicity from neutrino interactio ns in water as a function of momentum transfer will lower systematic uncer tainties for future long-baseline neutrino experiments. The experiment is currently commissioning large-area picosecond photodetectors (LAPPDs) that will improve time and spatial resolution. This marks the first usage of L APPDs in a physics experiment. I will present some of the on-going work to wards testing\, characterization\, and deployment of LAPPDs.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15597/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15597/ END:VEVENT BEGIN:VEVENT SUMMARY:Transformer Networks for NOvA Event Classification DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15592@indico.ific.uv.es DESCRIPTION:Speakers: Alejandro Yankelevich (University of California at I rvine)\nNOvA is a long-baseline neutrino experiment studying neutrino osci llations with Fermilab’s NuMI beam. A convolutional neural network (CNN) that analyzes topological features is used to determine neutrino flavor i n both the near and far detectors and observe the disappearance of muon ne utrinos and the appearance of electron neutrinos. Alternative approaches t o flavor identification using machine learning are being investigated wit h the goal of developing a network trained with both event-level and parti cle-level images in addition to reconstructed physical variables while ma intaining the performance of the CNN. Such a network could be used to anal yze the individual prediction importances of these inputs. An original net work that uses a combination of transformer and MobileNet CNN blocks will be discussed.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15592 / LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15592/ END:VEVENT BEGIN:VEVENT SUMMARY:Synthetic data for the study of the CUORE detector response functi on DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15587@indico.ific.uv.es DESCRIPTION:Speakers: Alberto Gianvecchio (UNIMIB)\nRare event searches sh are the need to isolate signal from background events\, therefore experime nts must develop good energy resolution detectors.\nIn this scenario\, CUO RE (Cryogenic Underground Observatory for Rare Events) exploits an array o f 988 TeO$_{2}$ crystals operated as Low-Temperature Detectors (LTDs) at 1 0 mK. The main goal of the experiment is to search for neutrino-less doubl e beta decay ($0\\nu\\beta\\beta$) in $^{130}$Te. CUORE detectors show an excellent energy resolution making the experiment one of the most competit ive for $0\\nu\\beta\\beta$ searches in the world. \nWhat I am going to p resent deals with the generation of synthetic data for the study of the CU ORE detector response function. It is a novel technique consisting of simu lations that reproduce the data acquisition by taking into account non-ide al elements\, such as noise as well as the shape of the signals.\nSyntheti c data are processed with the CUORE official analysis software\, allowing the evaluation of the analysis impact on the final results.\nThe goal of m y work is to reproduce the peaks (in the energy spectrum) intrinsic shape and resolution linear trend as a function of energy. On one hand\, the pea k profile significantly deviates from a Gaussian distribution. On the othe r hand\, the linear trend of the resolution (FWHM) as a function of energy is somewhat unexpected for LTDs. \nTo find contributions to both effects\ , I initially investigated the impact of pileup on the peak shape\, identi fying significant deviations with respect to a Gaussian response. Addition ally\, I studied the effect of pulses with variable shapes\, highlighting a deviation from the Gaussian profile of the peak and an enlargement of th e energy resolution comparable with observed data. Moreover\, I was able t o reproduce the resolution linear trend as a function of energy.\nSyntheti c data is the only method so far that provides a simulation\, even though preliminary\, of the observed peak behavior. This innovative simulation ga ve very promising results and proved to be an extremely effective techniqu e for the study of the detector response function in CUORE.\n\nhttps://ind ico.ific.uv.es/event/6178/contributions/15587/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15587/ END:VEVENT BEGIN:VEVENT SUMMARY:Directional measurement in Borexino: Calibration of Cherenkov phot ons in a liquid scintillator detector using gamma sources DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15585@indico.ific.uv.es DESCRIPTION:Speakers: Sindhujha Kumaran (IKP-2 Forschungszentrum Jülich a nd RWTH Aachen University)\nBorexino is a 280-ton liquid scintillator dete ctor located at the Laboratori Nazionali del Gran Sasso (LNGS)\, Italy. Th e main goal of Borexino is to measure solar neutrinos via elastic scatteri ng off electrons in the liquid scintillator. The electrons are then detect ed by the photo-multiplier tubes via isotropically emitted scintillation p hotons. However\, in the first few nanoseconds after a neutrino interactio n\, Cherenkov photons (\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15585/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15585/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmogenic background suppression for the 
ICARUS detector using a concrete overburden DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15582@indico.ific.uv.es DESCRIPTION:Speakers: Biswaranjan Behera (Colorado State University )\nThe ICARUS detector will search for LSND like neutrino oscillations exposed a t shallow depth to the FNAL BNB beam in the context of the SBN program. In the approved FNAL SBN experiment the impact of cosmic rays is mitigated b y a $4\\pi$ Cosmic Ray Tagger (CRT) detector encapsulating the TPCs inside the pit and by a ~3 m concrete overburden both for the near and the far d etectors. Cosmic backgrounds rejection is particularly relevant for the IC ARUS detector. Due to its larger size and distance from target compared to SBND\, in ICARUS the neutrino signal/cosmic background ratio is 40 times more unfavorable with in addition a greater than 3 times larger out-of-spi ll comics rate. In this talk\, I will be addressing the question of a prob lematic background to genuine neutrino events especially into the electron neutrino appearance analysis by a detailed MonteCarlo calculation of the cosmic rays crossing the ICARUS detector.\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15582/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15582/ END:VEVENT BEGIN:VEVENT SUMMARY:Optimization of a single module of CUPID DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15580@indico.ific.uv.es DESCRIPTION:Speakers: Alberto Ressa (La Sapienza - University of Rome)\nIn view of the next generation experiment CUPID\, many R&D tests are\nongoin g to define the detector design. CUPID aims to search for\nneutrinoless do uble beta decay in a "zero background" environment\,\nrejecting alpha part icles thanks to the simultaneous detection of heat\nand scintillation ligh t. It is of primary importance to optimize the\nlight collection to perfor m an efficient particle identification. R&D\ntests on a single module of C UPID showed promising results in terms of\nlight yield and background reje ction. Moreover the assembly planned for\nCUPID has been tested to prove t he light detector performances and the\nenergy resolution of cubic Li2MoO4 crystals.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15580/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15580/ END:VEVENT BEGIN:VEVENT SUMMARY:Low Threshold Germanium Detectors for Neutrino-Nucleus Elastic Sca ttering and the Studies of its Quantum-Mechanical Coherency Effects DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15574@indico.ific.uv.es DESCRIPTION:Speakers: Vivek Sharma (Institute of Physics\, Academia Sinica \, Taipei\, Taiwan)\nNeutrino Nucleus Elastic Scattering ($\\nu A_{el}$) o ffers a unique laboratory to study Quantum Mechanical superpositions in el ectroweak interactions\, towards which several experimental programs are b eing actively pursued. In the TEXONO experiment\, we are currently focused to measure the $\\nu A_{el}$ cross-section for the reactor neutrinos (E$_ \\nu$ 95%) for $\\nu A_{el}$ with reactor and solar neutrinos for Xe/CsI\, Ge and Ar targets\, whereas coherency is only partial for DAR-$\\pi$ and weak for atmospheric neutrinos. Accordingly\, studies of $\\nu A_{el}$ wit h different neutrino sources provide complementary information and cover t he transitions from completely coherent to decoherent states. We also excl ude the complete coherency and decoherency conditions for COHERENT (CsI) d ata and project the sensitivity for reactor $\\nu A_{el}$ with Ge detector .\n\n 1. Research program towards observation of neutrino-nucleus coherent \n scattering.\, H. T. Wong et al.\, [J. Conf. Ser. 39\, 266 (2006)][1] .\n 2. Coherency in neutrino-nucleus elastic scattering.\, S. Kerman et al .\, [Phys. Rev. D93\, 113006 (2016)][2].\n 3. Studies of quantum-mechanica l coherency effects in neutrino-nucleus elastic scattering. V. Sharma et a l.\, [Phys. Rev. D 103\, 092002 (2021)][3].\n\n\n [1]: http://iopscience. iop.org/article/10.1088/1742-6596/39/1/064\n [2]: https://journals.aps.or g/prd/abstract/10.1103/PhysRevD.93.113006\n [3]: https://journals.aps.org /prd/abstract/10.1103/PhysRevD.103.092002\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15574/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15574/ END:VEVENT BEGIN:VEVENT SUMMARY:Understanding the systematic effects for the directional measureme nt of Be-7 solar neutrinos with Borexino DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15561@indico.ific.uv.es DESCRIPTION:Speakers: Apeksha Singhal (IKP-2 Forschungszentrum Juelich and RWTH Aachen University)\nBorexino\, located at the Laboratori Nazionali d el Gran Sasso in Italy\, is a liquid scintillator detector that measures s olar neutrinos via their forward elastic scattering off electrons . The sc intillation process of detection makes it impossible to distinguish electr ons scattered by neutrinos from the electrons emitted from the decays of r adioactive backgrounds. Due to the unprecedented radio-purity achieved by the Borexino detector\, the real time spectroscopic detection of solar neu trinos from both the pp chain and CNO fusion cycle of the Sun has been per formed. With the newly presented analysis\, it is now possible for the fir st time\, to detect solar neutrinos using the few Cherenkov photons emitte d at early times\, in the direction of scattered electrons with an energy threshold of 0.16 MeV in the liquid scintillator. The angle which correlat es the direction of the Sun and the direction of the emitted Cherenkov pho tons is a key parameter to extract the Be7 neutrino signal from data. This poster will describe the strategy used in the evaluation of various syste matic effects including the geometric conditions of the detector and the d ata selection cuts that can influence the shape of the directional angle d istribution for backgrounds\, which is crucial to disentangle the directio nal Be-7 solar neutrino signal from the isotropic background in data.\n\nh ttps://indico.ific.uv.es/event/6178/contributions/15561/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15561/ END:VEVENT BEGIN:VEVENT SUMMARY:Data analysis strategy used for the detection of CNO solar neutrin os with Borexino DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15560@indico.ific.uv.es DESCRIPTION:Speakers: Luca Pelicci (Forschungszentrum and RWTH University) \nBorexino is a large liquid scintillator experiment located at the underg round INFN Laboratori Nazionali del Gran Sasso\, in Italy. It was designed and built with the primary goal of real-time detection of low energy sola r neutrinos\, and in more than ten years of data taking it has measured al l the neutrino fluxes produced in the proton-proton-chain\, i.e. the main fusion process accounting for ~99% of the energy production in the Sun. Re cently\, after improvements and developments in both hardware and software \, Borexino has provided the first observation of solar neutrinos emitted from the subdominant Carbon-Nitrogen-Oxygen (CNO) fusion cycle. One of the key aspects of the analysis is the effectiveness and the performances of the multivariate fitting technique adopted to disentangle the neutrino sig nals from the backgrounds present in the detector. All the crucial steps o f the analysis strategy adopted to extract the interaction rate of CNO neu trinos will be described in this poster.\n\nhttps://indico.ific.uv.es/even t/6178/contributions/15560/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15560/ END:VEVENT BEGIN:VEVENT SUMMARY:The JUNO OSIRIS detector DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15550@indico.ific.uv.es DESCRIPTION:Speakers: Tobias Sterr (Eberhard Karls Universität Tübingen\ , Physikalisches Institut)\n(Poster contribution\, TAUP conference\, 26.8. – 3.9.2021\, Valencia\, Spain)\n\n-Tobias Sterr (1)\, for the JUNO OSIR IS Group\n\n1 Eberhard Karls Universität Tübingen\, Physikalisches Insti tut\, Germany\n\nThe Online Scintillator Internal Radioactivity Investigat ion System (OSIRIS) is a 20-ton liquid scintillator detector currently und er construction at the Jiangmen Underground Neutrino Observatory (JUNO) in Kaiping\, China. OSIRIS features 76 newly developed\, “intelligent PMTs ” (iPMTs) surrounding a cylindrical acrylic vessel enclosed in a Cherenk ov muon veto. Two calibration systems\, an Automated Calibration Unit (ACU ) and a laser calibration system are available. The detector will be integ rated into the Liquid Handling System (LHS) of JUNO. The main purpose of O SIRIS is the monitoring of the radiopurity of the liquid scintillator duri ng the filling phase of JUNO\, measuring contamination levels of 238U\, 23 2Th\, 85Kr\, 210Po and 14C. A consecutive physics phase addressing solar n eutrinos and 0νββ decay is foreseen.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15550/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15550/ END:VEVENT BEGIN:VEVENT SUMMARY:Purity monitoring for ProtoDUNE-SP DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15549@indico.ific.uv.es DESCRIPTION:Speakers: Yiwen Xiao (University of California Irvine)\nThe De ep Underground Neutrino Experiment (DUNE) is a next-generation long-baseli ne neutrino oscillation experiment based on liquid argon time projection c hamber (LArTPC) technology. In July 2020\, DUNE’s single-phase (SP) prot otype ProtoDUNE-SP (PD-SP) at CERN finished its two-year Phase-1 running\, which successfully collected test-beam data and cosmic ray data. A key as pect of LArTPC calibration is the lifetime of drift electrons\, which corr ects the charge attenuation caused by drift electrons which are captured b y impurities. A purity monitor is a miniature TPC that measures the lifeti me of electrons generated from the photocathode via the photoelectric effe ct. It enables continuous monitoring of the state of the detector\, especi ally while filling the cryostat and when liquid argon recirculation system s are operating. The purity monitoring system in ProtoDUNE-SP Phase-1 (PD- SP-I) continuously monitored liquid argon purity throughout the entire lif etime of PD-SP-I\, which was critical to the experiment’s successful com missioning\, operation\, and data taking. I will discuss the design\, impl ementation\, and results of purity monitors in PD-SP-I and future plans.\n \nhttps://indico.ific.uv.es/event/6178/contributions/15549/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15549/ END:VEVENT BEGIN:VEVENT SUMMARY:New physics from oscillations: sensitivity for the DUNE near detec tor DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15548@indico.ific.uv.es DESCRIPTION:Speakers: Salvador Urrea González (IFIC (CSIC-Univ Valencia)) \nWe study the capabilities of the DUNE near detector to probe deviations from unitarity of the leptonic mixing matrix\, the 3+1 sterile formalism a nd Non-Standard Interactions affecting neutrino production and detection. We clarify the relation and possible mappings among the three formalisms a t short-baseline experiments\, and we add to current analyses in the liter ature the study of the νμ→ντ appearance channel. We study in detail the impact of spectral uncertainties on the sensitivity to new physics usi ng the DUNE near detector\, which has been widely overlooked in the litera ture. Our analysis show that this plays an important role on the results a nd\, in particular\, that it can lead to a strong reduction in the sensiti vity to sterile neutrinos from νμ→νe transitions\, by more than two o rders of magnitude. This stresses the importance of a joint experimental a nd theoretical effort to improve our understanding of neutrino nucleus cro ss sections\, as well as hadron production uncertainties and beam focusing effects. Nevertheless\, even with our conservative and more realistic imp lementation of systematic uncertainties\, we find that an improvement over current bounds in the new physics frameworks considered is generally expe cted.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15548/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15548/ END:VEVENT BEGIN:VEVENT SUMMARY:Xenon doping of Liquid Argon in ProtoDUNE Single Phase DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15545@indico.ific.uv.es DESCRIPTION:Speakers: Niccolo' Gallice (Università degli Studi di Milano - INFN Milano)\nDoping Liquid Argon (LAr) with Xenon is a well known techn ique to shift the light emitted by Argon (128 nm) to a longer wavelength t o ease its detection. The largest Xenon doping test ever performed in a LA rTPC was carried out in ProtoDUNE Single Phase (ProtoDUNE-SP) at the CERN Neutrino Platform. From February to May 2020\, a gradually increasing amou nt of Xenon was injected to compensate for the light loss due to air conta mination. The response of such a large TPC (770 t of Liquid Argon and 440 t of fiducial mass) has been studied using the ProtoDUNE Photon Detection System (PDS) and a dedicated setup installed before the run.\nWith the fir st\, it was possible to study the total light detected in the system as a function of the xenon concentration and to characterise the light collecti on efficiency with respect to the track position. With the second system i t was possible to disentagle the LAr (128 nm) light from the Xenon (178 nm ) light using two dedicated X-Arapuca modules. The run was fully satisfact ory\, it was possible to measure directly the increase of the Xenon light component during doping\; furthermore most of the LAr light quenched by im purities was fully recovered even at small Xenon concentration (\n\nhttps: //indico.ific.uv.es/event/6178/contributions/15545/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15545/ END:VEVENT BEGIN:VEVENT SUMMARY:Time Projection Chambers instrumented with resistive Micromegas fo r the SAND near detector of DUNE DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15540@indico.ific.uv.es DESCRIPTION:Speakers: Pierre Granger (CEA/Irfu)\nThe Deep Underground Neut rino Experiment (DUNE) is a next-generation long-baseline neutrino acceler ator experiment. It aims for precise measurements of the neutrino oscillat ion parameters\, in particular the violation of the charge-parity symmetry and the neutrino mass hierarchy. DUNE consists of a Far Detector (FD) com plex with four multi-kiloton liquid argon detectors\, and a Near Detector (ND) complex located close to the neutrino source at Fermilab (USA).\nThe ND complex regroups three different detectors among which SAND (System for on-Axis Neutrino Detection) will be the only one permanently on the neutr ino beam axis.\nThe main purpose of SAND is to monitor in detail the emitt ed neutrino beam and its stability through time\, a crucial characteristic to realize accurate oscillation measurements at the percent level.\nSAND will reuse the superconducting magnet and the electromagnetic calorimeter of the KLOE experiment. There are currently two different designs proposed for the inner tracker\, which will be a fully new object.\nOne of the two consists of a large 3D matrix of 1.5cm side scintillator cubes (3DST) sur rounded by 3 gaseous Time Projection Chambers.\nThis setup allows to reali ze accurate beam monitoring combining the 3DST unprecedented capability of neutron detection and energy measurement with the high precision momentum resolution for charged particles offered by the TPCs. The proposed TPC de sign allows to reach spatial resolutions of a few hundreds of micrometers using 1cm² pads thanks to the use of resistive Micromegas technology for the charge readout. Results of prototypes testing of Micromegas modules wi th cosmics and test beam data will be shown\, together with the expected p erformances of the SAND TPCs based on simulation.\n\nhttps://indico.ific.u v.es/event/6178/contributions/15540/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15540/ END:VEVENT BEGIN:VEVENT SUMMARY:Characterization of the DUNE photodetectors and study of the event burst phenomenon DTSTART;VALUE=DATE-TIME:20210830T171500Z DTEND;VALUE=DATE-TIME:20210830T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15539@indico.ific.uv.es DESCRIPTION:Speakers: Alessandro Minotti (INFN - University of Ferrara)\nT he Deep Underground Neutrino Experiment (DUNE) is an upcoming neutrino phy sics experiment that will answer some of the most compelling questions in particle physics and cosmology. The DUNE far detectors employ silicon phot omultipliers (SiPMs) to detect light produced by charged particles interac ting in a large liquid argon time projection chamber (LarTPC).\nThe SiPMs are photosensors consisting of an array of single-photon avalanche diodes (SPAD) operating in Geiger mode. Their high sensitivity and dynamic range\ , as well as the possibility to fill large surfaces with high-granularity sensors\, makes them an ideal choice for DUNE. An international consortiu m of research groups is currently engaged in a systematic comparison of th e performances of the SiPM models that have been custom developed for DUNE by two manufacturers. Such detailed studies\, which include gain measurem ents and a structure study of the dark count rate at 77 K\, are meant to d etermine the best choice of the photodetection system for DUNE\, as well a s characterize the response of the chosen detectors for the DUNE simulatio n. Moreover\, an investigation of a newly observed phenomenon\, in which q uick bursts of tens of events at close range are collected in individual S iPMs\, is being carried out\, which potentially impacts the design of futu re models and their implementation in particle physics experiments.\nThis poster reports the main results in terms of characterization of the SiPMs that will be employed in DUNE\, as well as of our studies of the novel bur sts phenomenon.\n\nhttps://indico.ific.uv.es/event/6178/contributions/1553 9/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15539/ END:VEVENT BEGIN:VEVENT SUMMARY:Prospects of search for new physics in the Double Beta Decay with KamLAND-Zen 800 DTSTART;VALUE=DATE-TIME:20210830T164500Z DTEND;VALUE=DATE-TIME:20210830T170000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15477@indico.ific.uv.es DESCRIPTION:Speakers: Yuto Kamei (Research Center for Neutrino Science\, T ohoku university)\nTwo-neutrino double beta decay (2$\\nu\\beta\\beta$) is a rare radioactive decay that is a weak process of second-order. It has b een observed in neutrino-less double beta decay (0$\\nu\\beta\\beta$) sear ch experiments to verify the Majorana nature of neutrino. Precise observat ion of 2$\\nu\\beta\\beta$ is important to reduce the theoretical uncertai nty in the calculation of nuclear matrix elements required to obtain the e ffective Majorana mass from a lifetime of 0$\\nu\\beta\\beta$. Also\, 2$\\ nu\\beta\\beta$ itself is interesting because new physics could be hiding in the energy spectrum\, for examples\, Majoron emission mode 0$\\nu\\beta \\beta$ and 2$\\nu\\beta\\beta$ with neutrino-self-interaction.\n KamLAND -Zen 800 is an experiment to search 0$\\nu\\beta\\beta$ of $^{136}$Xe with ultra-pure large liquid scintillator detector\, KamLAND. KamLAND-Zen 800 has been observing since 2019 with 750 kg of Xenon gas 91% enriched in $^{ 136}$Xe. We can analyze 2$\\nu\\beta\\beta$ with high statistics.\nI prese nt the prospects of precisely measurement of 2$\\nu\\beta\\beta$ half life and search for new physics in 2$\\nu\\beta\\beta$ with KamLAND-Zen 800 in this presentation.\n\nhttps://indico.ific.uv.es/event/6178/contributions/ 15477/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15477/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for New Physics in 2$\\nu$DBD Decay with CUPID DTSTART;VALUE=DATE-TIME:20210830T163000Z DTEND;VALUE=DATE-TIME:20210830T164500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15474@indico.ific.uv.es DESCRIPTION:Speakers: Emanuela Celi (Gran Sasso Science Institute)\nThe de velopment of cryogenic calorimeters to search for neutrinoless double-beta decay (0$\\nu$DBD) has given in the last years increasingly promising res ults.\nTo achieve a nearly background-free condition\, scintillating cryst als for 0$\\nu$DBD have been developed. Thanks to the light-assisted parti cle discrimination\, this technology demonstrated the complete rejection o f the dominant alpha background. In addition\, the possibility of achievin g ton-scale exposures\, maintaining an excellent energy resolution\, lays the foundations for the CUPID project.\nCUPID is a next-generation experim ent aiming to exploit $^{100}$Mo enriched scintillating Li$_2$MoO$_4$ crys tals\, operating as cryogenic calorimeters\, to investigate the entire inv erted hierarchy region for neutrino messes. Thanks to the high Q$_{\\beta\ \beta}$ of $^{100}$Mo and the $\\alpha$-discrimination\, the CUPID goal is to achieve a background level in the region of interest of 10$^{-4}$ coun ts/(keV kg yr). \nAlthough the 0$\\nu$DBD is the main objective of CUPID\, other processes are open to experimental investigation\, particularly tho se inducing a distortion of the 2$\\nu$DBD spectral shape. Given the relat ively fast half-life of $^{100}$Mo 2$\\nu$DBD\, we expect to reach unprece dented sensitivities in the search for 2$\\nu$DBD bSM induced distortions. \nIn this poster a general overview of the CUPID experiment will be given as well as the first sensitivity estimation on others bSM processes.\n\nh ttps://indico.ific.uv.es/event/6178/contributions/15474/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15474/ END:VEVENT BEGIN:VEVENT SUMMARY:New results and perspectives on 130Te double beta decay to the fir st 0+ excited state from CUORE DTSTART;VALUE=DATE-TIME:20210830T161500Z DTEND;VALUE=DATE-TIME:20210830T163000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15469@indico.ific.uv.es DESCRIPTION:Speakers: Guido Fantini (Università di Roma La Sapienza)\nThe CUORE experiment is a closely packed array of 988 cryogenic calorimeters aimed at investigating lepton number violation via neutrino-less double be ta decay (0νββ) in 130Te. We present the latest results on searches for the double beta decay (DBD) of 130Te to the first 0+ excited state of 130 Xe in the 0νββ and Standard Model channels and discuss future perspecti ves. The de-excitation gamma rays emitted by the excited Xe nucleus in the final state yield a unique signature\, which can be searched for with low background by studying coincident events in two or more bolometers. With a 372.5 kg×yr TeO2 exposure the median limit setting sensitivities at 90\ \% Credible Interval (C.I.) were estimated as 5.6 × 10^24 yr for the 0ν ββ decay and 2.1 × 10^24 yr for the 2νββ decay. No significant evide nce for either of the decay modes was observed and a Bayesian lower bound at 90% C.I. on the decay half lives is obtained as: (T1/2)0ν0+ > 5.9 × 1 0^24 yr for the 0νββ mode and (T1/2)2ν0+ > 1.3 × 10^24 yr for the 2ν ββ mode. These represent the most stringent limits on the DBD of 130Te t o excited states and improve by a factor ∼5 the previous results on this process.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15469/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15469/ END:VEVENT BEGIN:VEVENT SUMMARY:Analysis techniques for the search of 128-Te 0vbb decay with the C UORE TeO2 cryogenic crystals DTSTART;VALUE=DATE-TIME:20210830T160000Z DTEND;VALUE=DATE-TIME:20210830T161500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15468@indico.ific.uv.es DESCRIPTION:Speakers: Valentina Dompè ()\nCUORE is a ton-scale experiment comprised of 988 TeO2 cryogenic crystals\, located at the underground Lab oratori Nazionali del Gran Sasso of INFN (Italy). The CUORE detectors are operated as pure calorimeters at a base temperature of ~10 mK\, that is re ached and maintained thanks to a custom built cryogen-free dilution cryost at designed with the aim of minimizing the vibrational noise and the envir onmental radioactivity.\nIn addition to the search for neutrinoless double beta decay of 130-Te\, which represents the main physics goal of CUORE\, its ultra-low background and large mass make it suitable for the search of other rare processes. One of these is the neutrinoless double beta decay of 128-Te\, the second tellurium isotope with the highest natural isotopic abundance (31.75%). The study of this transition is complicated by the hi gh background present in the energy region where the decay peak is expecte d\, namely at (866.7 +/- 0.7) keV. The dominant contribution to this backg round is due to the 130-Te two-neutrino double beta decay events.\nCUORE r epresents the first experiment able to operate a ton-scale mass of cryogen ic TeO2 bolometers in stable conditions\, and this allows it to access a f actor >10 higher sensitivity to the neutrinoless double beta decay of 128- Te with respect to past direct experiments.\n\nhttps://indico.ific.uv.es/e vent/6178/contributions/15468/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15468/ END:VEVENT BEGIN:VEVENT SUMMARY:Operation update and Calibration plan for the Scintillating Bubble Chamber (SBC) Collaboration's 10-kg LAr detector at Fermilab DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16018@indico.ific.uv.es DESCRIPTION:Speakers: Sumanta Pal (Univ. of Alberta\, McDonald Institute)\ nThe Scintillating Bubble Chamber (SBC) Collaboration is developing a nove l detection technique aimed at detecting low-mass (0.7-7 GeV/$c^2$) WIMP i nteractions and coherent elastic neutrino-nucleus scattering (CE$\\nu$NS) of reactor neutrinos. Using a target volume composed of superheated argon with xenon doping\, the nucleation signal from electron recoils (the limit ing factor for low-threshold studies in bubble chambers) is suppressed\, a llowing for the exploration of new parameter space. Particle interactions with the target fluid can lead to the production of heat (bubbles) and sci ntillation light. By combining these observables\, the SBC Collaboration i s aiming to reach a threshold of 100 eV for nuclear recoil detection with discrimination\, to be demonstrated for the first time in a 10-kg device a t Fermilab.\n\nIn this talk\, I will discuss current activities at Fermila b towards the commissioning and operation of this device. I will also disc uss our calibration run plan\, which aims to measure the response of this chamber to both electron- and nuclear-recoils at the target 100-eV thresho ld.\n\nhttps://indico.ific.uv.es/event/6178/contributions/16018/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16018/ END:VEVENT BEGIN:VEVENT SUMMARY:At what local temperature does xenon bubble? DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16016@indico.ific.uv.es DESCRIPTION:Speakers: P.A. (Sander) Breur (SLAC national accelerator labor atory)\nDuring the past decades experiments using liquid xenon as a detect or material have grown rapidly in the fields of dark matter and neutrino s earches. During the scale up of such detectors there is a big push to move the electronics closer to the detectors which are submerged in cryogenic noble gases. One such example is the development of ASICs operating in liq uid xenon for the amplification and digitization of charge and light signa ls. A big question is how much heat can be generated before these chips cr eates bubbles (nucleate boiling) in the xenon. Such bubbles could create h igh-voltage\, pressure and electronic noise problems within a detector. We report the first precision measurement of the superheat temperature requi red for bubble nucleation in liquid xenon of Δ Twall\,ONB = (16.9±0.5) K and Δ Twall\,ONB = (19.2+0.4−1.1) K at pressures of P = (0.98±0.02) b ar and P = (1.32+0.05−0.01) bar\, respectively. In this talk we will pre sent the results together with the video material of creating bubbles in l iquid xenon.\n\nhttps://indico.ific.uv.es/event/6178/contributions/16016/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16016/ END:VEVENT BEGIN:VEVENT SUMMARY:First results from the HENSA/ANAIS collaboration at the Canfranc U nderground Laboratory DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15972@indico.ific.uv.es DESCRIPTION:Speakers: Nil Mont-Geli (Institute of Energy Technologies (INT E)\, Technical University of Catalonia (UPC))\nNeutrons are one of the mai n sources of experimental background in underground laboratories. A good k nowledge of their spectral distribution is required in order to assess the effect on low counting rate experiments in astrophysics\, dark matter and neutrino research. The High Efficiency Neutron-Spectrometry Array (HENSA) has been developed in order to achieve the characterization of the neutro n background at the Canfranc Underground Laboratory (LSC). \n\nHENSA is a detection system based on the Bonner Spheres principle [THO02]. In order t o be sensitive at different energy ranges (from thermal energies to 10 Ge V)\, it is composed by several independent long 3He-filled proportional co unters embedded in High Density PolyEthylene (HDPE) moderators with differ ent sizes. The neutron flux spectrum is obtained from the experimental cou nting rates by means of iterative reconstruction algorithms. Key to the re liability of the reconstruction process is the use of an initial guess spe ctrum close to the true spectrum. Early versions of HENSA have already bee n used for characterization of the neutron background at LSC\, before the start of the scientific experiments [JOR13]\, and in the shallow undergrou nd facility Felsenkeller in Dresden [GRI20].\n\nThe HENSA/ANAIS collaborat ion aims for a precise determination of the neutron background\, including its possible seasonal fluctuation\, affecting ANAIS-112\, an experiment l ooking for dark matter annual modulation with NaI(Tl) scintillators [AMA21 ]. For the initial tests some modules of the HENSA setup were installed in Hall B at LSC\, in a position close to ANAIS-112 setup. The measurements started in March 2021 and a long term characterization of the neutron back ground in this position is foreseen until December 2022. \n\nIn this work\ , FLUKA Monte Carlo calculations of the neutron background spectrum at the LSC facility will be reported. The simulations are based on previous meas urements of the rock composition and intrinsic radioactivity [AMA06]. Thes e calculations provides a guess input for reconstruction of the spectral d istribution in HENSA measurements. In addition\, the first results of HENS A/ANAIS experimental measurements in Hall B will be presented and discusse d.\n\n[AMA06] J. Amaré et al. Journal of Physics: Conference Series 39 (2006) 35.\n[AMA21] J. Amaré et al.\, Physical Review D 103\, (2021) 1020 05.\n[GRI20] M. Grieger et al.\, Physical Review D 101 (2020) 123027.\n[J OR13] D. Jordán et al.\, Astroparticle Physics 42 (2013) 1\n[THO02] D.J. Thomas and A.V. Alevra\, NIMA 476 (2002) 12–20.\n\n\n\n`\n\nhttps://indi co.ific.uv.es/event/6178/contributions/15972/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15972/ END:VEVENT BEGIN:VEVENT SUMMARY:Migdal event rates for D-D and D-T neutron generators DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15923@indico.ific.uv.es DESCRIPTION:Speakers: Christopher McCabe (King's College London)\nThe ‘M igdal effect’ is an atomic physics effect that leads to the emission of a bound-state electron from atomic or molecular systems when the atomic nu cleus is suddenly perturbed. This effect has been used by several experime ntal collaborations to extend the sensitivity of dark matter direct experi ments to sub-GeV mass dark matter candidates. The MIGDAL (Migdal In Galact ic Dark mAtter expLoration) collaboration has been formed to detect the te ll-tale signature of an electron that has been ejected from an atom or mol ecule upon the scattering of fast neutrons\, providing a unique and unambi guous measurement of the Migdal effect. The experiment will run with inten se D-D and D-T neutron generators at the Rutherford Appleton Laboratory (R AL) in the UK.\nIn this talk\, I will present the atomic-physics theory un derlying the Migdal effect and discuss the differences and similarities of the effect between dark matter direct detection experiments and at the D- D and D-T neutron energies employed at RAL. I will then present estimates for the number of events that can be observed at the experimental set-up a t RAL for several different gas species.\n\nhttps://indico.ific.uv.es/even t/6178/contributions/15923/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15923/ END:VEVENT BEGIN:VEVENT SUMMARY:Density functional theory calculates general crystal responses for electron-dark matter interactions in silicon and germanium DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15915@indico.ific.uv.es DESCRIPTION:Speakers: Marek Matas (ETH Zurich)\nWe test the influence of t he detailed description of the electronic structure in crystalline silicon and germanium on the resulting calculated response of the electrons to ge neral dark matter interactions. \n We show that if the dark matter int eraction energy reaches a threshold of about 30 eV\, electron excitations from tightly-bound germanium 3$d$ states become important and since these are very narrow\, they suffer from incorrect electron self-interaction in the local density approximation to density functional theory. We address t his problem by introducing a Hubbard U-correction term that corrects the e nergy of these bands and restores them to the experimentally observed valu e. We then calculate the scattering rates coming from general crystal resp onses and put constraints on current experiments that are using silicon an d germanium targets.\n\nhttps://indico.ific.uv.es/event/6178/contributions /15915/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15915/ END:VEVENT BEGIN:VEVENT SUMMARY:Influence of NaI background and mass on testing the DAMA modulatio n DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15907@indico.ific.uv.es DESCRIPTION:Speakers: Madeleine Zurowski (University of Melbourne)\nWe pre sent here the model dependent and independent sensitivity studies for NaI detectors designed to test the DAMA result and compare the predicted limit s from SABRE with the present performance of both COSINE and ANAIS. We fin d that the strongest discovery and exclusion limits are set by a detector with the lowest background (assuming equal run times)\, and also note that our method correctly computes the present exclusion C.L. previously publi shed by ANAIS and COSINE. In particular\, with a target mass of 50 kg and background rate of 0.36 cpd/kg/keV (after veto)\, SABRE will be able to ex clude the DAMA signal with 3$\\sigma$ confidence or `discover' it with 5$\ \sigma$ confidence within 2 years. This strongly motivates the quest for e ver lower backgrounds in NaI detectors.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15907/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15907/ END:VEVENT BEGIN:VEVENT SUMMARY:Study of He-CF4-isobutane mixtures for directional dark matter sea rches with the CYGNO Time Projection Chamber DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15904@indico.ific.uv.es DESCRIPTION:Speakers: Fernando Amaro (LIBPys - Coimbra University)\nCYGNO is developing a gaseous Time Projection Chamber (TPC)\, which will be host ed at Laboratori Nazionali del Gran Sasso\, Italy\, and will rely on a tri ple Gas Electron Multiplier (GEM) stack for charge multiplication and elec troluminescence (EL) production. The EL will be collected with a high reso lution scientific camera for particle identification and 2D track reconstr uction\, with the aim of discriminating nuclear recoils and their directio n. \nThis work aims at determining how the addition of small percentages o f isobutane to the He-CF4 (60/40) select CYGNO TPC gas mixture influences the EL yield\, charge gain and energy resolution. A Large Area Avalanche P hotodiode (LAAPD) was used to readout the EL produced in the avalanches of a single GEM. Isobutane fractions up to 5% were added to the CYGNO He/CF 4 (60/40) base mixture.\nOur results show that the inclusion of isobutane does not severely compromise the amount of EL photons detected\, while mai ntaining the energy resolution and increasing the charge gain of the CYGNO He-CF4 (60/40) base mixture.\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15904/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15904/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter Axion search with riNg Cavity Experiment DANCE: Desig n and development of auxiliary cavity for simultaneous resonance of linear polarizations DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15890@indico.ific.uv.es DESCRIPTION:Speakers: Hiroki Fujimoto (Department of Physics\, University of Tokyo)\nAxion-like particles (ALPs) are undiscovered pseudo-scalar part icles that are candidates for ultralight dark matter. ALPs interact with p hotons slightly and cause the rotational oscillation of linearly polarized light. DANCE searches for ALP dark matter by amplifying the rotational os cillation with a bow-tie ring cavity. \n The sensitivity of the current pr ototype experiment DANCE Act-1 is degraded by around 3 orders of magnitude due to the resonant frequency difference between s- and p- polarizations in the bow-tie ring cavity.The simultaneous resonance of linear polarizati ons is necessary to amplify both the carrier field and the ALP signal\, an d to achieve the design sensitivity.\n In order to tune the resonant frequ ency difference\, a method of introducing an auxiliary cavity was proposed . We are now introducing the idea of the auxiliary cavity to DANCE Act-1. In this conference\, we will report on the design\, the control scheme and the current status of the auxiliary cavity of DANCE Act-1.\n\nhttps://ind ico.ific.uv.es/event/6178/contributions/15890/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15890/ END:VEVENT BEGIN:VEVENT SUMMARY:Simulation-based shielding design of the COSINUS experiment DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15885@indico.ific.uv.es DESCRIPTION:Speakers: Alexander Fuss (TU Wien & HEPHY)\nThe COSINUS experi ment aims for probing the nature of the long-standing annual modulation si gnal observed by the DAMA/LIBRA collaboration. After successful years of d etector prototyping\, the construction of a dedicated experimental facilit y will start this year in Hall B of the LNGS underground laboratory. At th e heart of the setup\, NaI crystals – the same material as used in DAMA/ LIBRA – will be operated as scintillating cryogenic calorimeters.\n\nTo reach the necessary sensitivity to potential signals\, background mitigati on is of utmost importance. Besides using radiopure crystals and going und erground\, this can be achieved by surrounding the detectors with dedicate d passive (and active) shielding layers. To optimize these layers and henc e minimize background contributions from environmental radioactivity as we ll as intrinsic contamination of materials used for cryostat\, shielding a nd infrastructure\, we performed detailed Monte Carlo simulations.\n\nIn t his contribution\, we will present the results of our simulation studies t ogether with the final design of the COSINUS experimental setup.\n\nhttps: //indico.ific.uv.es/event/6178/contributions/15885/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15885/ END:VEVENT BEGIN:VEVENT SUMMARY:Background model of the ANAIS-112 dark matter experiment DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15876@indico.ific.uv.es DESCRIPTION:Speakers: Susana Cebrian (Universidad de Zaragoza)\nThe ANAIS- 112 experiment is intended to test the observation of an annual modulation signal by the DAMA/LIBRA experiment using 112.5 kg of NaI(Tl) detectors o perated in the Canfranc Underground Laboratory (Spain). Data taking is goi ng on since August\, 2017 and annual modulation results from the analysis of three years of data have been presented\, being compatible with the abs ence of modulation.\n\nA complete study of the ANAIS-112 detector backgrou nd was carried out before unblinding data for the first modulation analysi s using the first year of data. A background model was developed for each detector from the direct measurement of primordial and cosmogenic activity in crystals and other components and Monte Carlo simulation. The knowledg e of some cosmogenic isotopes activities considered in this model has been improved by profiting from the large accumulated three-year exposure\, an d using only events outside the Region of Interest\, has led to a better e xplanation of the detector background time evolution. These background stu dies have been relevant to understand the different background components and to predict sensitivity as well as to model the time evolution consider ed in the annual modulation analysis.\n\nHere\, the ANAIS-112 background m odel will be firstly described\; then\, considering different analysis con ditions and energy ranges\, the comparison of model and measurements for e nergy spectra and counting rate time evolution for three years of data wil l be discussed.\n\nhttps://indico.ific.uv.es/event/6178/contributions/1587 6/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15876/ END:VEVENT BEGIN:VEVENT SUMMARY:Likelihood Methods in the CRESST-Experiment DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15870@indico.ific.uv.es DESCRIPTION:Speakers: Daniel Schmiedmayer (TU-Wien & HEPHY Vienna)\nDespit e overwhelming astrophysical evidence for the existence of Dark Matter and intense efforts towards its detection\, no clear signal has been found so far. Nonetheless\, monumental advancements have been made in the field wh ich allowed to put significant constraints on the parameter space for poss ible particle candidates. For this reason\, various statistical methods ha ve been employed and developed. For many direct dark matter searches the o ptimal interval method\, an extension of the maximum gap method developed by Yellin\, has been the golden standard. Recently however\, many experime nts have shifted to maximum likelihood based methods for their statistical data analysis.\n\nCRESST is a direct Dark Matter search experiment utiliz ing scintillating cryogenic bolometers as detectors. This detector princip le allows for an extremely low detection threshold as well as particle dis crimination. These features allowed CRESST to be one of the leading experi ments in low-mass Dark Matter searches for many years.\n\nIn this contribu tion an application of the maximum likelihood formalism to the data of CRE SST detectors is presented. Recent improvements in detector performance an d better understanding of the detector behavior have made the use of a com plete and un-binned likelihood approach both possible and beneficial. This method enables a better understanding of the properties of individual det ectors as well as the use of profile likelihood for limit calculations.\n\ nhttps://indico.ific.uv.es/event/6178/contributions/15870/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15870/ END:VEVENT BEGIN:VEVENT SUMMARY:Astroparticle physics obtaining more attention from a new type of audience DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15761@indico.ific.uv.es DESCRIPTION:Speakers: Marko Holma (Muon Solutions Oy\, Finland)\nThe high- energy physics is experiencing an interesting twist of events as some basi c principles related to cosmic-rays and atmospheric production of cascadin g earthbound particles appear becoming more mainstream\, at least in other sciences. We offer a few examples to support the point. First\, the corre sponding author of this work is a geologist by education and yet in the pr ocess to cross the barrier between two branches of science that have not t raditionally crossed the paths too often (the radionuclide dating been one of the major exceptions). This particular personal journey may not yet be a tip of an iceberg\, but it is\, at the very least\, an example of a new tendency of cross-pollination between disciplines. In this case\, the dri ving force is muons and muography\, the rapidly evolving application of mu ons in as wide range of disciplines as archaeology\, engineering\, and ear th sciences (including planetology and research of asteroids). \n\nMuograp hy is a novel geophysical imaging and monitoring method for density contra sts and temporal density changes in solid and liquid materials. It is base d on the differential attenuation of atmospheric muons in various directio ns in the material between the radiation source (air showers in the atmosp here) and the detector. The latter can be installed on ground or undergrou nd. Characterization of material densities can obtain many forms and it ca n be carried out with many types of gaseous\, scintillation\, and nuclear emulsion detectors. These include drift chambers\, micro-mesh gaseous stru ctures\, resistive plate chambers\, multi-wire proportional chambers\, sci ntillation detectors\, and Cherenkov telescopes. Some detectors are mobile \, some transportable\, and some stationary. Some detectors are used in st able conditions\, whereas in some cases the application dictates that the detector must be robust and of high endurance. The latter is especially tr ue for the long-term open-air or underground monitoring campaigns. Most of the varied detector types can be deployed in multiple environments (e.g.\ , within buildings\, on the surface of the earth\, caves\, and tunnels)\, some even underwater (e.g.\, borehole detectors). The materials\, too\, ca n be of many types and origins (e.g.\, a pyramid\, historical building\, e ngineered structure\, an active\, dormant or fossil volcano\, karst cave\, a soil bed or bedrock formation\, and an open pit or underground mine). M ost importantly\, at least regarding the current topic\, the researchers t hemselves can have backgrounds that differ from one another drastically (a n archaeologist\, volcanologist\, architect\, geologist\, geophysicist\, m ineral explorationist\, mining engineer\, etc.). \n\nIt is the above cross -pollination between the different disciplines that establishes muography not only a highly multidisciplinary but also a cross-disciplinary field of research. It also aids to enlarge and widen the audience base of astropar ticle physics. Even if this new research may not automatically be of great interest to astroparticle physicists\, it is likely fruitful in the long run as some research topics are hard to carry out without specialized skil ls and expertise in these other disciplines (e.g.\, muon propagation and e nergy loss in real-world rocks). In the short term\, however\, the best va lue proposition for the astroparticle physicists is that their own researc h is becoming increasingly referenced by authors who are non-physicists an d in journals that are not necessarily followed by astroparticle physicist s. It is also likely that this new pool of researchers increases the total reference counts of some astroparticle physics publications.\n\nWe will p rovide more examples of the development of muography and the expanding dis tribution of astroparticle physics amongst the other disciplines in our lo nger\, follow-up work.\n\nhttps://indico.ific.uv.es/event/6178/contributio ns/15761/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15761/ END:VEVENT BEGIN:VEVENT SUMMARY:Core-collapse simulation of SN 1987A binary progenitor and its mul timessenger signals DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15759@indico.ific.uv.es DESCRIPTION:Speakers: Ko Nakamura (Fukuoka University)\nWe perform a three -dimensional self-consistent core-collapse supernova simulation using a bi nary evolution progenitor model of SN 1987A by Urushibara et al. (2018). T his progenitor model is based on a slow-merger of 14 and 9 solar-mass star s and it satisfies most of the observational constraints such as red-to-bl ue evolution\, lifetime\, total mass and position in the Hertzsprung-Russe ll diagram at collapse\, and chemical anomalies. We find that this progeni tor model successfully present explosion and leave a 1.53 solar-mass neutr on star with a kick velocity of 70 km/s and a spin period of 0.1 s. Assumi ng a detector sensitivity of Kamiokande-II and the distance to the superno va of 51 kpc\, we obtain 16 neutrino detection events in one second. Some characteristic modes in its gravitational wave signal will also be discuss ed in our presentation.\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15759/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15759/ END:VEVENT BEGIN:VEVENT SUMMARY:Implementation of IceTop data in the IceCube Realtime Alert System DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15756@indico.ific.uv.es DESCRIPTION:Speakers: Najia Moureen Binte Amin (University of Delaware)\nT he IceCube Neutrino Observatory is a cubic-kilometer detector at the geogr aphic South Pole searching for astrophysical neutrinos. A realtime analysi s framework is implemented for multi-messenger time-domain astronomy. When the data acquisition system identifies candidate neutrinos of astrophysic al origin\, an alert is sent to the multi-messenger community for rapid fo llow-up observations. The main background for astrophysical neutrinos is l eptons produced in cosmic ray air showers: neutrinos from the northern hem isphere and muons from the southern hemisphere. These atmospheric backgrou nds are reduced using a data-driven selection based on the observed event energy and arrival direction. An array of ice-Cherenkov tanks on the surfa ce\, IceTop\, detects showers of secondary particles created in cosmic ray air showers. We will show that data from IceTop can be used to further re duce the background due to atmospheric muons\, and we will describe how it has been implemented within the IceCube alert system.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15756/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15756/ END:VEVENT BEGIN:VEVENT SUMMARY:Tunka-Grande scintillation array: resent results DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15741@indico.ific.uv.es DESCRIPTION:Speakers: Anna Ivanova (Irkutsk State University)\nThe number of the objectives of the TAIGA Astrophysical complex includes the study of the flux of charged cosmic rays and diffuse gamma rays with energies abov e 100 TeV. This complex is located in the Tunka Valley\, about 50 km from Lake Baikal at the site of the Tunka-133 Cherenkov facility. TAIGA include s the TAIGA-HiSCORE wide-angle Cherenkov array\, the network of Imaging At mospheric Cherenkov Telescopes (TAIGA-IACT)\, the Tunka-Grande and TAIGA-M uon scintillation arrays. \nThe results of an analysis of the joint events of the Tunka-Grande scintillation array and TAIGA-HiSCORE and Tunka -133 Cherenkov facilities are presented. Joint events comparison results verify scintillation experiment sufficient accuracy for the joint study of mass composition of cosmic rays and gamma-hadron separation.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15741/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15741/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing the magnitude of asymmetries in the lateral density distri bution of electrons in EAS DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15737@indico.ific.uv.es DESCRIPTION:Speakers: Animesh Basak (North Bengal University)\nThe lateral density distributions (LDD) of inclined cosmic ray air shower are asymmet ric and the corresponding iso-density contours are of increasing eccentric ellipses with zenith angles of different showers. The polar asymmetry of the iso-density contours introduces a significant shift of the EAS core\, which is quantitatively expressed as a gap length (GL) parameter between t he EAS core and the center of the modified density pattern consisting of s everal equi-density ellipses. The LDD of EAS particles is usually approxim ated by a particular type of lateral density function (LDF) which is gener ally assumed to be polar symmetric about the EAS axis\, and cannot descri be the asymmetric LDDs accurately. A polar angle-dependent modified latera l density function of EASs has been derived analytically by considering th e effect of attenuation of EAS particles in the atmosphere. From the simul ation studies\, it has been found that the GL manifests sensitivity to the cosmic ray mass composition. The cosmic ray mass sensitivity of the later al shower age is also re-examined by applying the modified LDF to the simu lated data.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15737/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15737/ END:VEVENT BEGIN:VEVENT SUMMARY:Behaviour of the lateral shower age of cosmic ray extensive air sh owers DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15731@indico.ific.uv.es DESCRIPTION:Speakers: Rajat K Dey (University of North Bengal)\nSome simpl e arguments are introduced for a possible explanation of the behaviour of the lateral shower age of proton-initiated showers. The corresponding anal ytical treatment based on the proposed argument is then illustrated. Using the Monte Carlo simulation code CORSIKA\, we have validated how the diffe rent characteristics associated with the lateral shower age predicted in t he present analytical parametrization\, can be understood. The lateral sho wer age of a proton-initiated shower and its correlations with the lateral shower ages of electron- and neutral pion-initiated showers supports the idea that the result of superposition of several electromagnetic sub-showe rs initiated by neutral pions might produce the lateral density distributi on of electrons of a proton initiated shower. It is also noticed with the simulated data that the stated feature still persists even in the local sh ower age representation.\n\nhttps://indico.ific.uv.es/event/6178/contribut ions/15731/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15731/ END:VEVENT BEGIN:VEVENT SUMMARY:Transition neutrino magnetic moments in CE$\\nu$NS DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15724@indico.ific.uv.es DESCRIPTION:Speakers: Kåre Fridell (Technical University of Munich)\nCohe rent Elastic Neutrino Nucleus Scattering (CE$\\nu$NS) is a novel technique to look for new physics beyond the Standard Model. We study the prospects of probing a transition magnetic moment in CE$\\nu$NS experiments\, and t he potential to shed light on the Dirac vs Majorana nature of neutrinos. W e show the NUCLEUS experiment as an example\, and demonstrate that propert ies of a potential sterile neutrino can be deduced through a consideration of the final state distribution.\n\nhttps://indico.ific.uv.es/event/6178/ contributions/15724/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15724/ END:VEVENT BEGIN:VEVENT SUMMARY:nEXO light detection system DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15719@indico.ific.uv.es DESCRIPTION:Speakers: Bindiya Chana (Carleton University)\nnEXO is a futur e 5-tonne scale Liquid Xenon experiment looking for neutrino-less double b eta decay of isotope Xe-136. To attain the projected half-life sensitivity of ~10^28 years\, at least 1% of energy resolution is required at the Q-v alue (Qββ = 2.458 MeV) of the decay. \nnEXO has planned to employ Silico n Photomultipliers (SiPMs) along the barrel of the cylindrical Time Projec tion Chamber with the electrons drifting towards anodes located on the cyl inder top endcap. The energy resolution is driven in large part by the lig ht detection capability\, with a minimum of 3% of scintillation photons ha ving to be detected. \nNewly developed vacuum ultra-violet (VUV) SiPMs wil l be used for detecting scintillation photons with wavelength in the ultra violet regime (165-195 nm). For achieving the target energy resolution\, t he SiPMs must have high photon detection efficiency (>15%) accompanied by low correlated avalanche noise and low dark noise rates. The primary goal of this research project is to characterize the VUV-SiPMs and measure thei r various features like gain\, crosstalk\, afterpulsing\, dark noise rate\ , reflectivity and photon detection efficiency. Along with all these measu rements\, a well-established monitoring tool will be required to test the large number of SiPMs before installation in the detector. IV (current-vol tage) curve characterisation is being explored as a rapid testing tool for the performances of SiPM. In this talk\, the results from characterisatio n of nEXO SiPMs and IV curve based SiPM monitoring method will be presente d.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15719/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15719/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent advancements of the experiment to search for 2K capture in $^{124}$Xe using a large proportional counter DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15700@indico.ific.uv.es DESCRIPTION:Speakers: Vladimir Kazalov (INR RAS)\nHere we report the curre nt sensitivity of the large proportional counter to a $^{124}$Xe 2$\\nu$EC EC filled with xenon gas up to 5 atm. One of the main procedures for detec ting ECEC decays of $^{124}$Xe in an experiment using a gas target is iden tifying three charge ionization clusters released during the absorption of two X-ray quanta and Auger electrons from a daughter atom. The developed new algorithm for digital processing of signals taken from the detector ma de it possible to consider the loss of electrons due to diffuseness and re combination in the track and correct the total energy release for the resp onse of a separate absorbed particle. Thus\, by increasing the efficiency of selecting useful events\, we expect an increase in the sensitivity to t he half-life 2$\\nu$2K-mode for a 6-year run to $2×10^{22}$ y (at 90% C.L .) in the current experiment.\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15700/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15700/ END:VEVENT BEGIN:VEVENT SUMMARY:Diffusion of density inhomogeneities in the early universe DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15659@indico.ific.uv.es DESCRIPTION:Speakers: Sovan Sau (University of Hyderabad)\nDensity inhomog eneities can be generated very early in the universe. They are one of the reasons for all the large-scale structures in the early universe. Density inhomogeneities play an important role in nucleosynthesis calculations and affect the phase transition dynamics. These inhomogeneities decay by part icle diffusion in the early universe. We have studied the decay starting f rom the electroweak phase transition up to the starting of the nucleosynth esis era. We study the decay of these inhomogeneities in the early univers e with and without considering the expansion of the universe. We calculate the interaction cross-section of the quarks with the neutrinos\, the elec trons\, and the muons and obtain the diffusion coefficients. We find that the expansion of the universe causes the inhomogeneities to decay at a fas ter rate. We find that the inhomogeneities generated at the electroweak ep och have very low amplitudes at the time of the quark hadron phase transit ion. So unless inhomogeneities are generated with a very high amplitude\, they will have no effect on the quark hadron phase transition. In the hadr onic phase\, we have considered the interaction of neutron\, proton\, elec tron\, and muon. We include the interaction of the muons with the neutrons and the protons till 100 MeV. We also find that large density inhomogenei ties generated during the quark hadron transition with sizes of the order of 1 km must have amplitudes greater than 10^5 times the background densit y to survive up to the nucleosynthesis epoch in an expanding universe.\n\n https://indico.ific.uv.es/event/6178/contributions/15659/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15659/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmological implications of EW vacuum instability: constraints on the Higgs-curvature coupling from inflation DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15658@indico.ific.uv.es DESCRIPTION:Speakers: Andreas Mantziris (Imperial College London)\nThe cur rent experimentally measured parameters of the Standard Model (SM) suggest that our Universe lies in a metastable electroweak vacuum\, where the Hig gs field is prone to vacuum decay to a lower state with catastrophic conse quences. Our measurements dictate that such an event has not taken place y et\, despite the many different mechanisms that could have triggered it in our past light-cone. The focus of our work has been to calculate the prob ability of the false vacuum to decay during the period of inflation and us e it to constrain the last unknown renormalisable SM parameter $\\xi$\, wh ich couples the Higgs field with space-time curvature. More specifically\, we derived lower $\\xi$-bounds from vacuum stability in three inflationar y models: quadratic and quartic chaotic inflation\, and Starobinsky-like p ower-law inflation. We also took the time-dependence of the Hubble rate in to account both in the geometry of our past light-cone and in the Higgs ef fective potential\, which is approximated with three-loop renormalisation group improvement supplemented with one-loop curvature corrections. Finall y\, an overview of some preliminary results regarding this calculation in the context of $R^2$-inflation will be given .\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15658/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15658/ END:VEVENT BEGIN:VEVENT SUMMARY:Model independent approach to photodisintegration of $^7Li$ at th e range of energies of interest to BBN DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15657@indico.ific.uv.es DESCRIPTION:Speakers: Aswathi V (Christ University )\nOne of the elements that was synthesized primordially in the standard Big Bang Nucleosynthesi s is Lithium. Lithium\, being fragile gets easily destroyed at relatively low temperatures in the mixing process between stellar surface and hot int ernal layers. So that\, at the end of the stellar lifetime the lithium con tent is believed to be depleted. Series of experimental measurements on l ithium isotopes were carried out at High Intensity Gamma Ray Source (HIGS) at Duke Free Electron Laser Laboratory. More recently experiments [1]-[2 ] were performed \, to measure the differential cross section of the photo -neutron reaction channel in photodisintegration of $^7Li$\, where the pr ogeny nuclei is in the ground state as well as in excited states . \nThe p urpose of present contribution is to study the reaction channel $ ^7Li+ \\ gamma \\to$ $^6Li+n $ using linearly polarized photons . The model indepe ndent irreducible tensor formalism [3]-[5] will be used to study the diffe rential cross section of the reaction. We study the angular dependence of differential cross section by expressing differential cross section in ter ms of legendre polynomials. In view of the several theoretical and ongoin g experimental studies\, a detailed theoretical study of the spin structur e of the amplitudes in $ ^7Li+ \\gamma \\to ^6Li+n $ and their expansion i n terms of 'electric' and `magnetic' amplitudes is needed to analyze the m easurements of spin observables as well as differential cross section\, wh ich leads to a better understanding of the problem at astrophysical energi es.\n\nReferences:\n[1]W. A. Wurtz\, R. E. Pywell \, B. E Norum\, S. Kucuk er \, B. D. Sawatzky\, \, H. R. Weller\, M. W. Ahmed\, S. Stave\, “Measu rement of the absolute and differential cross sections for 7Li(γ\, n0)\, ” *Phys.Rev.C*\, \, **84**\, 044601 (2011).\n[2]W. A. Wurtz\, R. E. Py well\, B. E. Norum\, S. Kucuker\, B. D. Sawatzky\, H. R. Weller\, S. Stave \, M.W.Ahmed\, “Photodisintegration of 7Li with progeny nuclei in excite d states\,” *Phys.Rev.C*\, **92**\, 044603 (2015).\n[3]G. Ramachandran\ , S. P. Shilpashree\, “Deutron disintegration of polarised photons at as trophysical energies\,” *Phys.Rev.C*\, **74**\, 052801(R) (2006).\n[4 ]G. Ramachandran\, Yee. Yee. Oo\, S. P. Shilpashree\, “Photodisintegrati on of polarides deuteron at astrophysical energies\,” *J.Phys.G:Nucl.Par t.Phys* \, **32**\, B17 – B21 (2006).\n[5]S. P. Shilpashree\, Swarnamal a. Sirsi\, G. Ramachandran\, “Photodisintegration of aligned deuteron at astrophysical energies using linearly polarised photons\,” *Int.Jou.Mod .Phys.E*\, **22**\, 1350030 (2013).\n\nhttps://indico.ific.uv.es/event/6 178/contributions/15657/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15657/ END:VEVENT BEGIN:VEVENT SUMMARY:Metallic Magnetic Calorimeters for the BabyIAXO experiment DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15656@indico.ific.uv.es DESCRIPTION:Speakers: Andreas Abeln (Kirchhoff-Institute for Physics\, Hei delberg University)\nThe next generation helioscopes BabyIAXO and IAXO wil l search for evidence of axions and axion-like particles (ALPs) produced i n the center of the Sun. In the helioscope a strong magnetic field would c onvert ALPs via the generic ALP-photon coupling into photons. A very promi sing candidate for the focal plane X-ray detectors are low temperature met allic magnetic calorimeters (MMCs). Combining good energy resolution and h igh quantum efficiency\, MMC-based detectors would allow to investigate th e solar axion spectrum and derive information on axion models beyond disco very. Furthermore\, by analyzing the resulting X-ray spectrum\, details ab out the interior of the Sun could be deduced.\nIn this contribution\, we p resent the 8x8 pixel detector array maXsIAXO which was specifically optimi zed for the needs of BabyIAXO. This detector features an absorber area of 1 cm$^2$ with a filling factor of 94.4 $\\%$ to match the focal spot size of the X-ray optics. The X-ray absorbers have a thickness of 10 µm and ar e made of gold to ensure a high stopping power over the complete energy ra nge of interest up to 8 keV as well as around 14 keV where a strong line i s expected. The expected energy resolution is about 11 eV (FWHM). At the l ight of a background characterization of similar MMC arrays\, we conclude discussing the advantages of using this X-ray detector system for BabyIAXO and IAXO.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15656/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15656/ END:VEVENT BEGIN:VEVENT SUMMARY:Inflationary Dynamics of Tsallis Holographic Scalar Field Models i n Chern-Simons Modified Gravity DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15655@indico.ific.uv.es DESCRIPTION:Speakers: Gargee Chakraborty (Amity University\, Kolkata)\nTh e study aims to reconstruct the scalar field model of Dark Energy (DE) nam ely tachyon\, k-essence and dilation scalar field models of DE through hol ographic dark fluid under Chern-Simon's Modified Gravity. $\\Lambda$CDM fi xed point is attained in case of tachyon scalar field model under this cos mological settings $[1-8]$. Some constraints have been derived on the int eraction term as Tsallis Holographic DE parameter in the interacting scena rio by considering k-essence scalar field model. Equation of State (EoS) p arameter for all the cases have been deduced and found to be consistent wi th the observational data from Planck+WP+BAO for current universe i.e.\, a t $z=0$. Exception is that\, the behaviour of reconstructed scalar field m odel is phantom $[9-13]$. Evolutionary behaviour of reconstructed scalar f ield and potential for various cases have been plotted and studied.\n\n\n\ n\nReferences:\n[1] A. G. Riess et al.\, Astron. J.\, 116\, 1009 (1998).\n [2] S. Perlmutter et al.\, Astrophys. J.\, 517\, 565 (1999).\n[3] P. Astie r et al.\, Astron. Astrophys.\, 447\, 31 (2006).\n[4] M. Tegmark et al. (S DSS Collaboration)\, Phys. Rev. D\, 69\, 103501 (2004).\n[5] K. Abazajian et al. (SDSS Collaboration)\, Astron. J.\, 128\, 502 (2004).\n[6] K. Abaza jian et al.\, (SDSS Collaboration)\, Astron. J.\, 129\, 1755 (2005).\n[7] D. N. Spergel et al.\, (WMAP Collaboration)\, Astrophys. J. Suppl.\, 148\, 175 (2003).\n[8] D. N. Spergel et al.\, (WMAP Collaboration)\, Astrophys. J. Suppl.\, 170\, 377 (2007).\n[9] M. Tavayef\, A.Sheykhi\, K. Bamba\, H. Moradpour\, Phys. Lett. B\, 781\, 195 (2018).\n[10] S. Nojiri\, S. D. Odi ntsov\, H. Stefancic\, Phys. Rev. D\, 74\, 086009 (2006).\n[11] S. Nojiri\ , S. D. Odintsov\, J. Phys. A\, 40\, 6725 (2007).\n[12] G. Cognola\, E. El izalde\, S. Nojiri\, S. D. Odintsov\, S. Zerbini\, Phys. Rev. D\, 75\, 086 002\n(2007).\n[13] S. Nojiri\, S. D. Odintsov\, J. Phys. Conf. Ser.\, 66\, 012005 (2007).\n\nhttps://indico.ific.uv.es/event/6178/contributions/1565 5/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15655/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmology of modified Chaplygin gas under the purview of f(T) grav ity DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15653@indico.ific.uv.es DESCRIPTION:Speakers: Surajit Chattopadhyay (Dept of Mathematics\, Amity U niversity\, Kolkata)\nIn this work\, we investigate the cosmological appli cation of modified Chaplygin gas\n(MCG) interacting with pressureless dark matter (DM) in the f(T) modified gravity\nframework\, where T is the tors ion scalar in teleparallelism. The interaction term has\nbeen chosen propo rtional to the MCG density with positive coupling constant. In the\nEinste in general relativity (GR) framework\, the interacting MCG has been found to\nhave equation of state (EoS) parameter behaving like quintessence. How ever\, the f(T)\ngravity reconstructed via the interacting MCG has been fo und to have EoS crossing\nthe phantom boundary of −1. Thus\, one can gen erate a quintom-like EoS from an\ninteracting MCG model in flat universe i n the modified gravity cosmology framework.\nThe reconstructed f(T) model has been found to interpolate between dust and ΛCDM.\nStability of the re constructed f(T) has been investigated and it has been observed\nthat the model is stable against gravitational perturbation. Cosmological evolution of\nprimordial perturbations has also been investigated and the self-inte racting potential\nhas been found to increase with cosmic time and the squ ared speed of sound has been\nfound to be non-negative.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15653/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15653/ END:VEVENT BEGIN:VEVENT SUMMARY:First search for new forces at the micron scale using optically le vitated microspheres DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15652@indico.ific.uv.es DESCRIPTION:Speakers: Alexander Fieguth (Stanford University)\nWe report o n a search for non-Newtonian forces that couple to mass\, with a character istic scale of ${\\sim}10~\\mu$m\, using an optically levitated microspher e as a precision force sensor. A silica microsphere trapped in an upward-p ropagating\, single-beam\, optical tweezer is utilized to probe for intera ctions sourced from a nanofabricated attractor mass with a density modulat ion brought into close proximity to the microsphere and driven along the a xis of periodic density in order to excite an oscillating response. We obt ain force sensitivity of ${ 10^8$ for $\\lambda > 10~\\mu$m. This is the f irst test of the inverse-square law using an optically levitated test mass of dimensions comparable to $\\lambda$\, a complementary method subject t o a different set of system effects compared to more established technique s.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15652/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15652/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing Lorentz Invariance Violation with Atmospheric Neutrinos at INO-ICAL DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15622@indico.ific.uv.es DESCRIPTION:Speakers: Sadashiv Sahoo (Institute of Physics Bhubaneswar\; H omi Bhabha National Institute Mumbai)\nUnified theories such as string the ory suggests spontaneous Lorentz Invariance Violation(LIV) by introducing a new spacetime structure at the Planck Scale ($m_p \\sim 10^{19}$ GeV). T his effect can be observed at low energies with strength of $\\sim 1/m_p$ using perturbative approach. In the Minimal Standard Model Extension (SME) framework\, the neutrino mass-induced flavor oscillation gets modified in the presences of LIV. The Iron Calorimeter (ICAL) detector at the propose d India-based Neutrino Observatory (INO) offers an unique window to probe these LIV parameters by observing atmospheric neutrinos and anti neutrinos separately over a wide range of baselines in the multi-GeV energy range. In this paper\, for the first time\, we study in detail how the CPT-violat ing LIV parameters $(a_{e\\mu}\, a_{e\\tau}\, a_{\\mu\\tau})$ can alter mu on survival probabilities and expected $\\mu^-$ and $\\mu^+$ event rates a t ICAL. Using 500 kt$\\cdot$yr exposure of ICAL\, we place stringent bound s on these CPT-violating LIV parameters at 95% C.L which are slightly bett er than the present Super-Kamiokande limits. We discuss the effect of the marginalization over the oscillation parameters and the advantage of havin g the hadron energy information and charge identification capability at IC AL in constraining these LIV parameters. We also study the impact of these LIV parameters on mass ordering determination and precision measurement o f atmospheric oscillation parameters.\n\nhttps://indico.ific.uv.es/event/6 178/contributions/15622/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15622/ END:VEVENT BEGIN:VEVENT SUMMARY:Detection of Core-Collapse Supernova Neutrino at JUNO DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15620@indico.ific.uv.es DESCRIPTION:Speakers: Xin Huang (IHEP)\nJUNO is an underground neutrino ob servatory under construction in Jiangmen\, China. It uses\n20kton liquid s cintillator as a target\, which enables it to detect supernova burst neutr inos of\nlarge statistics for the next galactic core-collapse supernova (C CSN) and also pre-supernova\nneutrinos from the nearby CCSN progenitors. A ll flavors of supernova burst neutrinos can be\ndetected by JUNO via sever al interaction channels\, including inverse beta decay (IBD)\, elastic\nsc attering on electron and proton\, etc. Among them\, IBD events makes it po ssible to get the\ndirectional information of CCSN even in a liquid scinti llator detector. The real-time monitoring\nsystems for the next CCSN based on FPGA and DAQ are under development in JUNO\, which\nallows prompt aler t and trigger-less data acquisition of CCSN events\n\nhttps://indico.ific. uv.es/event/6178/contributions/15620/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15620/ END:VEVENT BEGIN:VEVENT SUMMARY:A comparative study of Dirac and Majoarana ultrahigh-energy neutri no oscillations in an interstellar magnetic field DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15615@indico.ific.uv.es DESCRIPTION:Speakers: Konstantin Kouzakov (Moscow State University)\nOne o f the important developments in the field of neutrino astrophysics is a se arch for ultrahigh-energy (UHE) cosmic neutrinos (even above PeV–EeV ene rgies)\, which are believed to be produced by reactions of UHE cosmic rays composed of protons and nuclei. These neutrinos can be detected with neut rino telescopes\, such as IceCube\, ANTARES\, Baikal-GVD\, and KM3NeT\, an d are expected to provide information about cosmic accelerators and the hi gh-energy\, distant universe. One of the major advantages of exploring the UHE neutrinos as astrophysical messengers is supposed to be their ability \, as opposed to the case of charged particles\, of traveling in straight lines in magnetic fields in space. This feature allows one to point back t heir intensively energetic sources in the sky\, including active galactic nuclei\, supernovae and associated phenomena like γ-ray bursts\, and comp act objects such as black holes and neutron stars. At the same time\, even though neutrinos are generally believed to be electrically neutral partic les they can still have nonzero magnetic moments [1]. This means that the propagation of the UHE cosmic neutrinos can be influenced by interstellar magnetic fields due to the effect of spin oscillations [2]. In this contri bution we examine the UHE neutrino propagations in interstellar space in t he Dirac and Majorana cases. Employing the two-neutrino mixing approximati on and using the most stringent astrophysical constraints on neutrino magn etic moments\, we show that both the flavor and the spin oscillations of t he Dirac and Majorana neutrinos exhibit qualitatively different behaviors in an interstellar magnetic field for neutrino-energy values characteristi c of\, respectively\, the cosmogenic neutrinos\, the Greisen-Zatsepin-Kuz ’min (GZK) cutoff\, and well above the cutoff. \n\nThe work is supported by the Interdisciplinary Scientific and Educational School of Moscow Stat e University "Fundamental and Applied Space Research" and by the Russian F oundation for Basic Research under grant no. 20-52-53022-GFEN-A. \n\n**Ref erences**\n[1] C. Giunti and A. Studenikin\, Neutrino electromagnetic inte ractions: A window to new physics\, Rev. Mod. Phys. 87\, 531 (2015)\, arXi v:1403.6344 [hep-ph] \n[2] P. Kurashvili\, K.A. Kouzakov\, L. Chtorlishvil i\, and A.I. Studenikin\, Spin-flavor oscillations of ultrahigh-energy cos mic neutrinos in interstellar space: The role of neutrino magnetic moments \, Phys. Rev. D 96\, 103017 (2017)\, arXiv:1711.04303 [hep-ph].\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15615/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15615/ END:VEVENT BEGIN:VEVENT SUMMARY:Collective neutrino oscillations in moving and polarized matter DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15614@indico.ific.uv.es DESCRIPTION:Speakers: Yufeng Li (Institute of High Energy Physics)\nWe stu dy neutrino flux evolution in an extreme astrophysical environment peculia r to supernovae accounting for the collective effects and effects of an ar bitrarily moving and polarized media and a strong magnetic field. The effe ct of the transversally moving matter on the flavour and spin-flavour osci llations in a magnetic field was considered in [1-3]. In the present pape r we further develop the quantum theory of neutrino flavour and spin-flavo ur oscillations in moving magnetized matter with a special focus on the po ssible effects of the transversal matter polarization. Both the cases of D irac and Majorana neutrinos are considered. In addition\, we also account for the superimposed effect of the collective neutrino oscillations and di scuss possible spectral splits of the final neutrino fluxes that can arise due to flavour and spin-flavour oscillations in this case.\n\n\n \nThis r esearch has been supported by the Interdisciplinary Scientific and Educati onal School of Moscow University “Fundamental and Applied Space Research ” and also by the Russian Foundation for Basic Research under Grant No. 20-52-53022-GFEN-a. The work of KS is also supported by the RFBR under gra nt No. 20-32-90107 and by the “BASIS” Foundation No. 20-2-2-3-1.\n \n[ 1] A. Studenikin\, Neutrinos in electromagnetic fields and moving media\, Phys.Atom.Nucl. 67 (2004) 993-1002 (Yad.Fiz. 67 (2004) 1014-1024).\n[2] P. Pustoshny\, A. Studenikin\, Neutrino spin and spin-flavour oscillations i n transversal matter currents with standard and non-standard interactions\ , Phys. Rev. D 98 (2018) 113009. \n[3] Y.-F.Li\, K.Kouzakov\, V.Shakhov\, K.Stankevich\, A.Studenikin\, Z.Yuan\, Interplay of neutrino flavor\, spin and collective oscillations in supernovae\, PoS ICHEP2020 (2021) 206.\n\n https://indico.ific.uv.es/event/6178/contributions/15614/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15614/ END:VEVENT BEGIN:VEVENT SUMMARY:Spin and spin-flavor oscillations due to neutrino charge radii int eraction with an external environment DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15611@indico.ific.uv.es DESCRIPTION:Speakers: Konstantin Stankevich (Moscow State University)\nIt is believed that the running (for instance\, COHERENT) and forthcoming ter restrial neutrino experiments will be sensitive to the neutrino charge rad ius [1] that is one of the neutrino fundamental electromagnetic characteri stics [2] predicted [3] to be non-zero even in the Standard Model. In this work we continue our studies [4] on neutrino oscillations accounting for diagonal and non-diagonal neutrino charge radii. We consider spin and spin -flavor neutrino oscillations in an extreme astrophysical environment and on the basis of exact expressions for the corresponding neutrino oscillati on probabilities we study conditions for possible neutrino resonances enge ndered by the neutrino charge radii. We apply the obtained results to an e xtreme astrophysical environment. \nThis research has been supported by th e Interdisciplinary Scientific and Educational School of Moscow University “Fundamental and Applied Space Research” and also by the Russian Foun dation for Basic Research under Grant No. 20-52-53022-GFEN-a. The work of KS is also supported by the RFBR under grant No. 20-32-90107 and by the “BASIS” Foundation No. 20-2-2-3-1.\n[1] M.Cadeddu\, F.Dordei\, C.Giunt i\, K.Kouzakov\, E.Picciau\, A.Studenikin\, Phys.Rev.D 100 (2019) 073014.\ n[2] C.Giunti\, A.Studenikin\, Rev.Mod.Phys. 87 (2015) 531.\n[3] J.Bernabe u\, L.G.Cabral-Rosetti\, J.Papavassiliou\, J.Vidal\, Phys.Rev.D 62 (2000) 113012.\n[4] K.Kouzakov\, F.Lazarev\, V.Shakhov\, K.Stankevich\, A.Studeni kin\, PoS ICHEP2020 (2021) 217.\n\nhttps://indico.ific.uv.es/event/6178/co ntributions/15611/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15611/ END:VEVENT BEGIN:VEVENT SUMMARY:Effects of nonzero Majorana CP phases on oscillations of supernova neutrinos DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15609@indico.ific.uv.es DESCRIPTION:Speakers: Artem Popov (Lomonosov Moscow State University)\nWe study the effects of nonzero Dirac and Majorana CP-violating phases in neu trino oscillations in a magnetic field of astrophysical environments. It i s shown that in the presence of strong magnetic fields and dense matter\, nonzero CP phases can induce new resonances\, particularly in the oscillat ions channels $\\nu_e \\leftrightarrow \\bar{\\nu}_e$\, $\\nu_e \\leftrigh tarrow \\bar{\\nu}_\\mu$ and $\\nu_e \\leftrightarrow \\bar{\\nu}_{\\tau}$ . We show that neutrino-antineutrino oscillations can affect the $\\bar{\\ nu}_e$/$\\nu_e$ ratio for neutrinos coming from the supernovae explosion\, provided that the Majorana CP-violation phases are nonzero. The detection of supernovae neutrino fluxes in the future experiments\, such as JUNO\, DUNE and Hyper-Kamiokande\, can give an insight into the nature of CP viol ation and\, consequently\, provides a tool for distinguishing the Dirac or Majorana nature of neutrinos.\n\nThis research has been supported by the Interdisciplinary Scientific and Educational School of Moscow University “Fundamental and Applied Space Research” and also by the Russian Found ation for Basic Research under Grant No. 20-52-53022-GFEN-a. The work of A . P. has been supported by the Foundation for the Advancement of Theoretic al Physics and Mathematics “BASIS” under Grant No. 19-2-6-209-1.\n\n** References**\n[1] A. Popov\, A. Studenikin\, “Manifestations of nonzero Majorana CP-violating phases in\noscillations of supernova neutrinos"\, Ph ys.Rev.D 103 (2021) 11\, 115027\n\nhttps://indico.ific.uv.es/event/6178/co ntributions/15609/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15609/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of cosmogenic neutron production in SK-Gd DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15603@indico.ific.uv.es DESCRIPTION:Speakers: Masataka Shinoki (Tokyo University of Science)\nSK-G d experiment has been started with gadolinium (Gd) added to ultra-pure wat er in Super-Kamiokande. SK-Gd dramatically improves the sensitivity to sup ernova relic neutrino searches by tagging neutrons. Cosmic-ray muons flyin g into Super-Kamiokande induce hadronic showers. Those break oxygen nuclei in water and produce unstable radioactive isotopes and neutrons\, which a re major background sources for supernova relic neutrino searches.\nIn add ition\, the cosmogenic neutrons can be used for the detector calibration s ource. Since cosmic-ray muons fly into Super-Kamiokande continuously with the rate of 2 events/s\, the cosmogenic neutrons can be used to check the stability and uniformity of the Gd concentration in the detector.\nIn this presentation\, I will report the current status of cosmogenic neutron mea surement in SK-Gd.\n\nhttps://indico.ific.uv.es/event/6178/contributions/1 5603/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15603/ END:VEVENT BEGIN:VEVENT SUMMARY:Supernova neutrino burst search at KamLAND DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15602@indico.ific.uv.es DESCRIPTION:Speakers: Minori Eizuka (RCNS\, Tohoku Univ.)\nThe observation of neutrinos from SN1987A had improved our understanding of \nthe mechani sm of the supernova explosion and neutrino properties. Now\, several state -of-the-art neutrino detectors are running. There is a chance to reveal th e explosion mechanism and neutrino properties in more details. In this stu dy\, we search for neutrino events from supernovae with KamLAND\, which is a 1kt liquid scintillator detector\, via inverse-beta decay reaction. Kam LAND can measure low energy events ($E_{\\nu}>1.8$MeV) with low background conditions from delayed-coincidence scheme and have long-term stable data from 2002\, including an unexplored dataset by other neutrino detectors ( Dec. 2013 ~ Jul. 2020). Selection criteria for supernova events are two or more inverse beta decays within 10 s. We present the search results and u pper limits on supernova rate in our galaxy.\n\nhttps://indico.ific.uv.es/ event/6178/contributions/15602/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15602/ END:VEVENT BEGIN:VEVENT SUMMARY:Identification of the cosmogenic $^{11}$C background in the solar neutrino experiment Borexino DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15598@indico.ific.uv.es DESCRIPTION:Speakers: Alessio Porcelli (Universiteit Gent)\nBorexino is a liquid scintillator detector situated underground in the Laboratori Nazion ali del Gran Sasso in Italy. Its physics program evolves around the study of solar and geo-neutrinos. By now\, Borexino has measured neutrinos from the fusion processes in the pp chain and CNO cycle. Especially for the det ection of pep and CNO neutrinos\, an important background is formed by the cosmogenic radio-isotope $^{11}$C that is produced by muon spallation of $^{12}$C nuclei in the scintillator. \n\nGiven the comparatively long life time (30 mins) and high rate (30 cpd and 100 ton)\, dedicated veto strate gies had to be developed to permit the detection of pep and CNO neutrinos. The present contribution presents two veto methods. One is the well-estab lished Three Fold Coincidence (TFC) technique that relies on time and spac e correlation of muons\, spallation neutrons\, and radioactive $^{11}$C de cays\; it has been used in different implementations in all former Borexin o analyses. In addition\, a newly devised algorithm searching for time-cor related bursts of $^{11}$C events will be presented\, highlighting as well the potential gain from a combined application with the TFC technique. \n \nAlthough both methods have been primarily developed for $^{11}$C tagging in Borexino\, they are not limited to this specific experiment or spallat ion isotope\, offering a broad range of potential applications in low-back ground neutrino experiments.\n\nhttps://indico.ific.uv.es/event/6178/contr ibutions/15598/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15598/ END:VEVENT BEGIN:VEVENT SUMMARY:Evaluation of neutron tagging performance in the Hyper-Kamiokande experiment DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15562@indico.ific.uv.es DESCRIPTION:Speakers: Shota Izumiyama (Tokyo Institute of Technology)\nHyp er-Kamiokande (HK) is a next generation multi-purpose neutrino and nucleon -decay experiment scheduled to begin operation in 2027. The experimental s etup of HK will consist of the neutrino beam line and a suite of near dete ctors at J-PARC\, and a far detector of the same name\, HK. The far detect or HK\, filled with 260 kton of pure water is able to detect a Cherenkov l ight from the relativistic charged particles produced in the (anti)neutrin o interactions. To distinguish neutrino and antineutrino interactions in H K\, a neutron signal can be used. This is especially important in the Diff used Supernovae Neutrinos Background search\, which is one of the physics targets of HK. Using neutron signals allows HK to highly suppress backgrou nd events and to improve the signal sensitivity. Furthermore\, the neutron tagging largely reduces neutrino-induced backgrounds with neutrons in the nucleon decay search where nucleon decays rarely accompany neutrons. In t he pure water detector\, the generated neutron is thermalized in water and captured by a hydrogen nucleus. The hydrogen nucleus emits a 2.2 MeV gamm a-ray that is seen as a delayed signal of the prompt Cherenkov events even tually. In this study\, we simulated the neutron signal and one of the dom inant backgrounds\, created by Rn\, which might mimic the neutron signals\ , and evaluated tagging efficiency in HK. The neutron tagging algorithm an d the results will be presented.\n\nhttps://indico.ific.uv.es/event/6178/c ontributions/15562/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15562/ END:VEVENT BEGIN:VEVENT SUMMARY:Characterization of the JUNO Large-PMT readout electronics DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15559@indico.ific.uv.es DESCRIPTION:Speakers: Beatrice Jelmini (Università degli Studi di Padova & INFN Padova)\nThe Jiangmen Underground Neutrino Observatory (JUNO) is a neutrino medium baseline experiment under construction in southern China\, expecting to begin data taking in 2023. The experiment has been proposed with the main goals of determining the neutrino mass ordering and measure three oscillation parameters with sub-percent precision. To reach these go als\, JUNO is located about 53 km from two nuclear power plants and will d etect electron antineutrinos from reactors through inverse beta decay. Fur thermore\, an unprecedented energy resolution of 3% at 1 MeV is required. The JUNO detector consists of 20 kton of liquid scintillator (LS) containe d in a 17.7 m radius acrylic vessel\, which is instrumented with a system of about 18000 20-inch Large-PMTs and 25600 3-inch small-PMTs\, with a tot al photocoverage greater than 75%.\n\nThe signal from the Large-PMTs is pr ocessed by the JUNO electronics system\, which can be divided into two mai n parts: the front-end electronics\, placed underwater\, consisting of a G lobal Central Unit (GCU)\; and the back-end electronics\, outside water\, consisting of DAQ and trigger. Each GCU reads three Large-PMTs and has the main tasks of performing the analog-to-digital conversion of the signals\ , generating a local trigger to be sent to the global trigger\, reconstruc ting the charge\, tagging events with a timestamp\, and temporarily storin g data in the local FPGA memory before transferring it to DAQ upon a globa l trigger request. The poster will mainly focus on the description of the underwater electronics for the Large-PMTs. Results from tests on a small s etup with 13 GCUs at Laboratori Nazionali di Legnaro\, Italy\, as well as from the upcoming integration test with 700 GCUs in China\, will be presen ted.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15559/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15559/ END:VEVENT BEGIN:VEVENT SUMMARY:Performance evaluation of 3-inch PMT for Hyper-Kamiokande DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15558@indico.ific.uv.es DESCRIPTION:Speakers: Tatsushi Kinoshita ()\nHyper-Kamiokande is the next generation water Cherenkov detector for the study of neutrino oscillations including the search for leptonic CP violation using high intensity neutr ino beam produced in J-PARC. In order to reduce the systematic uncertainty of the CP violation measurement\, a 1kton scale Intermediate water Cheren kov detector (IWCD) is planned to be constructed around 1km downstream the J-PARC neutrino beamline. The multi-PMT modules\, which consist of 19 3-i nch PMTs will be installed in the IWCD to improve the detector performance with their higher granularity.\nIn this poster\, we will present the meas urements of the performance for 3-inch PMT such as time resolution\, dark noise rate and relative photon detection efficiency.\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/15558/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15558/ END:VEVENT BEGIN:VEVENT SUMMARY:What is a breakdown of continuous component hidden under 4.4-MeV g amma-ray peak from the AmBe source? DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15557@indico.ific.uv.es DESCRIPTION:Speakers: Kohei Wada (Yokohama National University)\nAmericium -Beryllium (AmBe) is a typical source to be use for a calibration of neutr on detection efficiency in underground astroparticle experiments. It has b een considered to emit a neutron and 4.4 MeV gamma ray simultaneously\, wh ich allows us to select events with a neutron by tagging the 4.4 MeV gamma -ray signal. This time\, we focus on the higher energy component around 5- 10 MeV in a deposited energy distribution\,under the measurement with inor ganic scintillators. Any component hidden under the 4.4 MeV peak could be counted with no neutron emission in the tagging events. We aim to understa nd the breakdown of the continuous component from the AmBe source to contr ibute reduction of a systematic uncertainty related to the neutron detecti on efficiency for the astroparticle physics. We will present a result of m easurements for neutrons and gamma rays using NaI(Tl) and liquid scintilla tion detectors.\n\nhttps://indico.ific.uv.es/event/6178/contributions/1555 7/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15557/ END:VEVENT BEGIN:VEVENT SUMMARY:Evaluation of event reconstruction with small-scale water Cherenko v detectors DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15556@indico.ific.uv.es DESCRIPTION:Speakers: Koki Yamauchi (Tokyo University of Science)\nThe Hyp er-Kamiokande experiment is planned to start in 2027 aiming for precise me asurement of neutrino oscillation using J-PARC neutrino beam including the search for CP violation. Hyper-Kamiokande detector is a 260 kiloton water Cherenkov detector and has large statical power\, requiring systematic un certainty at the 1% level or less on neutrino oscillation measurements. Fo r this purpose\, a new 1 kiloton scale Intermediate Water Cherenkov Detect or (IWCD)\, which is based on the same detection principle as Hyper-Kamiok ande is proposed to measure the neutrino flux and interaction cross sectio n near the generation point of the neutrino beam before oscillation. The g oal of IWCD is to reduce the systematic uncertainty in the long baseline n eutrino oscillation measurement of the Hyper-Kamiokande experiment. Water Cherenkov Test Experiment (WCTE) is a 50 ton scale water Cherenkov detecto r and currently under preparation to evaluate the performance of IWCD. WCT E will use new photosensor technologies such as multi-PMT modules and will study the response of small water Cherenkov detectors to electron\, muon\ , and hadron beams at CERN.\nIn this poster\, we will present the performa nce of event reconstruction with the IWCD and WCTE detectors using the sim ulation.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15556/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15556/ END:VEVENT BEGIN:VEVENT SUMMARY:Development of high-sensitivity radon detector in water for neutri no physics DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15554@indico.ific.uv.es DESCRIPTION:Speakers: Atsushi Takeda (ICRR\, Univ. of Tokyo)\nRadon contam ination in water causes serious background for low energy physics in Super -Kamiokande experiment\, especially\, search for distortions of the solar neutrino energy spectrum induced by the MSW effect. \nContinuous monitorin g of radon concentration in water with \n\nhttps://indico.ific.uv.es/event /6178/contributions/15554/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15554/ END:VEVENT BEGIN:VEVENT SUMMARY:Energy Response Model for JUNO Experiment DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15553@indico.ific.uv.es DESCRIPTION:Speakers: Miao Yu (Institution of High Energy Physics\, China) \nEnergy Response Model for JUNO Experiment\n\nMiao Yu\, on behalf of JUNO collaboration\n\nThe Jiangmen Underground Neutrino Observatory (JUNO) is a multi-purpose neutrino experiment with 20000 ton liquid scintillator (LS ) detector under civil construction. The primary physics goal for JUNO is to determine the neutrino mass ordering by precisely measuring the fine os cillation pattern of reactor neutrinos at around 53 km baseline. Antineutr inos emitted by nuclear reactors are detected by inverse beta decay (IBD) interaction $\\bar\\nu_e + p→ e^+ + n$ where the positron carries most f raction of neutrino energy. To precisely construct incoming neutrino energ y spectrum\, it’s vital to have a better understanding for positron ener gy response (e.g. nonlinearity and resolution) in LS. While the common cal ibration sources are almost gamma sources\, it is required to develop a ca libration-based energy response model for positrons with the help of calib ration data. In this poster\, a unified model to describe both nonlinearit y and energy resolution is presented\, and the effects from scintillation light and Cherenkov light are studied separately in detail. Also\, possibl e disentanglement between scintillation and Cherenkov light contributions in energy response based on feasible external measurements are discussed f or better model constraints.\n\nhttps://indico.ific.uv.es/event/6178/contr ibutions/15553/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15553/ END:VEVENT BEGIN:VEVENT SUMMARY:First results from the ARTIE experiment DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15544@indico.ific.uv.es DESCRIPTION:Speakers: Luca Pagani (UC Davis)\nA measurement of the transmi ssion coefficient for neutrons through a thick (~3 atoms/b) liquid natural argon target in the energy range 30-70 keV was performed by the Argon Res onance Transmission Interaction Experiment (ARTIE) using a time of flight neutron beam at Los Alamos National Laboratory.\nIn this energy range theo ry predicts an anti-resonance in the $^{40}$Ar cross section near 57 keV\, but the existing data\, coming from an experiment performed in the 90s (W inters. et al.)\, does not support this.\nThis discrepancy gives rise to s ignificant uncertainty in the penetration depth of neutrons through liquid argon\, an important parameter for next generation neutrino and dark matt er experiments.\nIn this talk\, the first results from the ARTIE experimen t will be presented.\nThe ARTIE measurement of the total cross section as a function of energy confirms the existence of the anti-resonance near 57 keV\, but not as deep as the theory prediction.\n\nhttps://indico.ific.uv. es/event/6178/contributions/15544/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15544/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino Mixing by modifying the Yukawa coupling structure of cons trained sequential dominance DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15538@indico.ific.uv.es DESCRIPTION:Speakers: Joy Ganguly (Indian Institute of Technology Hyderab ad)\nIn the constrained sequential dominance (CSD)\, tri-bimaximal mixing (TBM) pattern in the neutrino sector has been explained\, by proposing a c ertain Yukawa coupling structure for the right-handed neutrinos of the mod el. However\, from the current experimental data it is known that the valu es of neutrino mixing angles are deviated from the TBM values. In order to explain this neutrino mixing\, we first propose a phenomenological model where we consider Yukawa couplings which are modified from that of CSD. Es sentially\, we add small complex parameters to the Yukawa couplings of CSD . Using these modified Yukawa couplings\, we demonstrate that neutrino mix ing angles can deviate from their TBM values. We also construct a model\, based on a flavor symmetry\, in order to justify the modified form of Yuka wa couplings of our work.\n\nhttps://indico.ific.uv.es/event/6178/contribu tions/15538/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15538/ END:VEVENT BEGIN:VEVENT SUMMARY:The cosmic muon-induced background for the LEGEND-1000 Alternative Site at LNGS DTSTART;VALUE=DATE-TIME:20210901T171500Z DTEND;VALUE=DATE-TIME:20210901T173000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15508@indico.ific.uv.es DESCRIPTION:Speakers: Moritz Neuberger (TUM (Techincal University Munich)) \nThe in-situ production of long-lived isotopes by cosmic muon interaction s may generate a non-negligible background for the search for rare events in the deep subsurface\, defining a minimum depth requirement. Monte Carlo studies for a GERDA-like experiment at LNGS-depth identified the delayed decay of $^{77(\\mathrm{m})}$Ge as the dominant in-situ cosmogenic backgro und in the search for the neutrinoless double-beta decay of $^{76}$Ge [1\, 2]\, with a projected background index (BI) of $2.7\\times 10^{-6}$ cts/(k eV$\\cdot$kg$\\cdot$yr) after delayed coincidence rejection at Q$_{\\beta \\beta}=2039~\\mathrm{MeV}$ [2]. The future tone-scale LEGEND-1000 experim ent requires a total BI from all individual contributions of $\\leq10^{-5} $ cts/(keV$\\cdot$kg$\\cdot$yr) [3\,4]. Dedicated Monte Carlo simulation s tudies of the $^{77(\\mathrm{m})}$Ge background for LEGEND-1000\, includin g different mitigation strategies\, were performed at the alternative LNGS site\, as opposed to the SNOLAB baseline site. We will present the effect s of passive and active measures to further reduce this background contrib ution to meet the overall background requirements.\n\n[1] L. Pandola et al .\, Nucl. Instr. Methods A 570 (2007) 149\n[2] C. Wiesinger et al.\, Eur. Phys. J. C (2018) 78:597\n[3] AIP Conference Proceedings\, Volume 1894\, I ssue 1\, id.020027\n[4] LEGEND-1000 pCDR. To be available at https://legen d-exp.org/science/publications\n\nhttps://indico.ific.uv.es/event/6178/con tributions/15508/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15508/ END:VEVENT BEGIN:VEVENT SUMMARY:Optimizing the time resolution of cryogenic calorimeters with NTDs : the CALIPSO project DTSTART;VALUE=DATE-TIME:20210901T164500Z DTEND;VALUE=DATE-TIME:20210901T170000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15492@indico.ific.uv.es DESCRIPTION:Speakers: Irene Nutini (Università e Sezione INFN di Milano B icocca)\nThe CALIPSO project deals with the development and optimization o f low temperature (~10 mK) solid state detectors. The goal of the project is to propose new strategies for improving the time resolution of cryogeni c scintillating calorimeters\, read with NTD thermistors. We will test new NTD-detector coupling techniques and optimize the NTD operation to make t he response faster. In parallel\, we will work on improving the scintillat ion light yield for different crystals at low temperatures. Rare events ph ysics experiments utilizing the NTD-detector technology on a large scale\, such as the ones searching for the neutrinoless double beta decay (CUORE\ ; CUPID)\, could profit from the results of this project.\n\nhttps://indic o.ific.uv.es/event/6178/contributions/15492/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15492/ END:VEVENT BEGIN:VEVENT SUMMARY:New measurement of double beta decays to excited states in the CUP ID-Mo experiment DTSTART;VALUE=DATE-TIME:20210901T163000Z DTEND;VALUE=DATE-TIME:20210901T164500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15488@indico.ific.uv.es DESCRIPTION:Speakers: Toby Dixon (UC Berkeley)\nCUPID-Mo\, located at the Laboratoire Souterrain de Modane\, in France was a demonstrator for CUPID\ , a next generation search for $0 \\nu \\beta \\beta$ in $^{100}$Mo. It co nsisted of an array of 20 Li$_2$MoO$_4$ bolometers and 20 Ge light detecto rs for particle ID. It has demonstrated excellent crystal radio-purity ($^ {238}$U/$ ^{232}$Th chains $0.3 - 1$ $\\mathrm{\\mu Bq/kg}$ for relevant i sotopes)\, $\\alpha$\, $\\beta/\\gamma$ particle discrimination ($>99.9\\% $)\, and energy resolution ($\\sim 7 \\ \\mathrm{keV}$ FWHM at $2615$ $\\ mathrm{keV}$). This performance allowed CUPID-Mo to place the leading limi t on the half life of $0 \\nu \\beta \\beta$ in $^{100}$Mo of $T_{1/2}^{0 \\nu}>1.5 \\cdot 10^{24}$\\\,yr despite a very modest $2.16$ kg-yr exposu re.\nIn this work we present the results from the search for double beta d ecays of $^{100}$Mo to excited states of $^{100}$Ru. Precision measurement of the $2\\nu\\beta\\beta$ decay can help constrain nuclear models which are needed to interpret $0\\nu\\beta\\beta$ results as a limit on the neu trino mass.\nIn these decays\, the electrons are accompanied by one or mor e de-excitation gamma quanta. Multi-site events provide a very clear exper imental spectrum technique to search for these decays and separate them fr om possible background sources.\nFinally\, we demonstrate how the analysis techniques we have developed could be employed by the next generation exp eriment CUPID to reach an unprecedented sensitivity to decays to excited s tates and other rare processes.\n\nhttps://indico.ific.uv.es/event/6178/co ntributions/15488/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15488/ END:VEVENT BEGIN:VEVENT SUMMARY:Rejecting Spallation Backgrounds in KamLAND-Zen with KamNet DTSTART;VALUE=DATE-TIME:20210901T161500Z DTEND;VALUE=DATE-TIME:20210901T163000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15487@indico.ific.uv.es DESCRIPTION:Speakers: Hasung Song (Boston University)\nKamLAND-Zen is a li quid scintillator detector searching for neutrinoless double beta decay of Xenon-136. Recently\, KamLAND-Zen set world-leading limits on this elusiv e process. One of the primary challenges of this search is the rejection o f backgrounds from radioactive isotopes introduced by cosmic-ray spallatio n. We developed a state-of-the-art neural network classifier\, called KamN et\, to reject background events and improve detection sensitivity. Howeve r\, as we rely more heavily on deep neural networks to play key roles in d ata analysis\, it becomes increasingly important to understand exactly how they work. Here\, we take a look at KamNet through the lens of network in terpretability. Using Monte Carlo (MC) simulations and experimental data\, we present the results of recent studies of the origin of KamNet's reject ion power. We find that KamNet has the ability to discern multi-vertex eve nts (one or more gammas in addition to a beta) from single-vertex beta eve nts (only betas). This beta vs beta+gamma discrimination is used to help u s ascertain spallation background levels. KamNet's rejection performance f or key spallation backgrounds will be presented and we discuss how KamNet can inform us about the types of backgrounds it's rejecting.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15487/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15487/ END:VEVENT BEGIN:VEVENT SUMMARY:Germanium Detector Front-End Electronics for the LEGEND Experiment DTSTART;VALUE=DATE-TIME:20210901T160000Z DTEND;VALUE=DATE-TIME:20210901T161500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15481@indico.ific.uv.es DESCRIPTION:Speakers: Michael Willers (Technische Universität München)\n The question of whether the neutrino is identical to its anti-particle\, i .e.\, a Majorana particle\, is one of the most fundamental challenges in p article physics. This basic property is connected to the origin of the neu trino mass and could help explain the predominance of matter over antimatt er in our Universe. Neutrinoless double-beta ($0\\nu\\beta\\beta$) decay - a so-far unobserved radioactive transition - is the only known\, feasible method to probe the Majorana nature of the neutrino in the laboratory. A discovery of $0\\nu\\beta\\beta$ decay would unambiguously demonstrate tha t new lepton-number-violating physics exists and connect it to the origin of the neutrino mass.\n\nThe Large Enriched Germanium Experiment for Neutr inoless $\\beta\\beta$ Decay (LEGEND) is an ton-scale\, $^{76}$Ge based\, experimental program with discovery potential at half-lives beyond $10^{28 }$ years.\nIn this contribution I will discuss the discrete\, low-mass & l ow-background\, germanium detector front-end (FE) electronics for the firs t 200-kg phase of the experiment (LEGEND-200)\, which is currently under c onstruction at the Gran Sasso underground laboratory (Laboratori Nazionale del Gran Sasso\, LNGS\, Italy). In addition\, I will present the R&D effo rts on ASIC-based readout electronics for the ton-scale phase of the exper iment (LEGEND-1000).\n\nThis work is supported by the U.S. DOE\, and the N SF\, the LANL\, ORNL and LBNL LDRD programs\; the European ERC and Horizon programs\; the German DFG\, BMBF\, and MPG\; the Italian INFN\; the Polis h NCN and MNiSW\; the Czech MEYS\; the Slovak SRDA\; the Swiss SNF\; the U K STFC\; the Russian RFBR\; the Canadian NSERC and CFI\; the LNGS and SURF facilities.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15481/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15481/ END:VEVENT BEGIN:VEVENT SUMMARY:Tests of the Lorentz invariance violation in double-beta decay DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15636@indico.ific.uv.es DESCRIPTION:Speakers: Sabin Stoica (International Centre for Advanced Trai ning and Research in Physics (CIFRA))\nThere is currently interest in test ing possible Lorentz invariance violation (LIV) in different physical proc esses. LIV effects have also been searched in the neutrino sector\, mainl y in neutrino oscillation experiments. However\, there are LIV effects ind uced by a Lorentz-violating operator in the Standard Model extension (SME) theory\, called countershaded operator\, which does not affect the neutri no oscillations. Such effects\, related to the time-like component of this operator\, which are controlled by the oscillation-free (of) coefficient (aof3)00\, would produce small deviations in the\nshape of the energy spec tra of electrons emitted in double-beta decays. Such investigations are cu rrently been conducted in several double beta decay experiments as EXO\, G ERDA\, SuperNEMO\, CUORE and CUPID-0. These analysis are based on accurate theoretical predictions of the electron spectra and their angular correla tions in 2νββ decay. \nIn my talk I will give a current review of this topic. I will first present the precise calculation of the summed energy electron spectra and their deviations due to LIV\, and the constraints of the (aof3)00 coefficient obtained from these analyzes. Next\, I show that current investigations of LIV can be complemented by searches in the singl e electron spectra and angular correlations between the emitted electrons. Distortions due to LIV occur in the single electron spectra (maximal at s mall electron energies) and other effects may be highlighted by analyzing the angular correlation spectra and the ratio between the SME electron spe ctra and their SM forms. Finally\, I will present an\nalternative\, new me thod to constrain (aof3)00 through the measurement of the angular correlat ion coefficient\, and show that future experiments can improve these limit s significantly.\n\nReferences\n1. S. Stoica\, Investigation of Lorentz sy mmetry violation in double-beta decay\, MEDEX’19\, Prague\, May 28-June 2\, 2019 (invited lecture).\n2. O. Nitescu\, S. Ghinescu\, and S. Stoica\, J. Phys. G 47\, 055112 (2020).\n3. O. Nitescu\, S. Ghinescu\, and S. Stoi ca\, Phys. Rev. D 103\, L031701 (2021).\n4. S. Stoica\, Study of kinemati c factors in double-beta decay\, Conference on Neutrino and Nuclear Physic s (CNNP2020)\, February 20-24\, Cape Town\, South Africa (invited lecture) .\n\nhttps://indico.ific.uv.es/event/6178/contributions/15636/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15636/ END:VEVENT BEGIN:VEVENT SUMMARY:First tritium endpoint measurement with Cyclotron Radiation Emissi on Spectroscopy (CRES) DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15723@indico.ific.uv.es DESCRIPTION:Speakers: Christine Claessens (Center for Experimental Nuclear Physics and Astrophysics\, University of Washington\, WA\, USA)\nThe Proj ect 8 collaboration is seeking a direct measurement of the absolute neutri no mass scale from the distortion of the tritium beta decay spectrum near the endpoint with a sensitivity of $\\sim 40\\\,\\mathrm{meV/c^2}$. To thi s end\, the collaboration has successfully established CRES\, a frequency- based approach to detect electrons and determine their kinetic energy. Thi s talk will present the data and analysis of the first tritium spectrum re corded using the CRES technique. The spectrum shows no events beyond the e ndpoint\, demonstrating the ultra-low background obtainable with this tech nology. This talk will further report on the improved energy resolution an d the influence of the main systematic error sources on the shape of the m easured spectrum and the tritium endpoint determination.\nThis work is sup ported by the US DOE Office of Nuclear Physics\, the US NSF\, the PRISMA+ Cluster of Excellence at the University of Mainz\, and internal investment s at all institutions.\n\nhttps://indico.ific.uv.es/event/6178/contributio ns/15723/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15723/ END:VEVENT BEGIN:VEVENT SUMMARY:Simulation of Nuclear Recoils due to Supernova Neutrino-induced Ne utrons in Liquid Xenon Detectors DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15612@indico.ific.uv.es DESCRIPTION:Speakers: Sayan Ghosh (Saha Institute of Nuclear Physics)\nDet ectable number of nuclear recoil (NR) events can occur from neutrinos from supernova (SN) bursts through the coherent elastic neutrino-nucleus scatt ering (CE$\\nu$NS) process in large scale liquid xenon detectors designed for direct dark matter search depending on the SN mass and distance. In th is presentation\, we show that in addition to the direct NR events due to CE$\\nu$NS process\, the SN neutrinos can be detected via the nuclear reco ils due to the elastic scattering of the neutrons produced due to the inel astic interactions of the neutrino with the xenon nuclei. We find that the contribution of the supernova neutrino-induced neutrons ($\\nu$I$n$) can significantly modify the total xenon NR spectrum\, at large recoil energie s\, from the spectrum expected from CE$\\nu$NS contribution alone. Moreove r\, for recoil energies $>20$ keV\, the dominant contribution is obtained from the ($\\nu$I$n$) events. Using the nuclear spectra of both the CE$\\n u$NS and the $\\nu$I$n$ events\, we numerically calculate the observable S 1 and S2 signals for a typical liquid xenon based detector accounting for the multiple scattering effects for the $\\nu$I$n$ and find that at suffic iently large signals events\, S1$>$50 photo-electrons (PE) and S2$>$2300 P E\, are dominantly contributed by $\\nu$I$n$ scatterings. We note that sin ce $\\nu$I$n$ contribution to the recoil spectrum arises due to the charge d current interaction of the SN $\\nu_e$s with the target nuclei while the neutral current interactions\, responsible for CE$\\nu$NS events\, comes from of all the six species of neutrinos\, the capability of detecting the se individual recoil events\, especially in the S2 channel\, in future lar ge scale liquid xenon detectors may offer the possibility of extraction of information regarding the distribution of the SN explosion energy into di fferent flavours of neutrinos.\n\nhttps://indico.ific.uv.es/event/6178/con tributions/15612/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15612/ END:VEVENT BEGIN:VEVENT SUMMARY:New Constraints on Heavy Neutral Leptons using the ArgoNeuT Experi ment DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15705@indico.ific.uv.es DESCRIPTION:Speakers: Patrick Green (The University of Manchester)\nArgoNe uT was a 0.24 ton Liquid Argon Time Projection Chamber (LArTPC) detector a t Fermilab running from 2009 to 2010. It was located along the NuMI neutri no beam and collected six months of data in anti-neutrino beam mode. ArgoN euT has performed several first neutrino cross-section measurements on arg on\, however its dataset can also be used to probe physics beyond the Stan dard Model. One such model is Heavy Neutral Leptons (HNL) that couple to t he standard model via mixing with tau neutrinos. These would be produced b y the NuMI beam via decays of D-mesons into secondary taus\, which then de cay into HNLs. The HNLs then travel along the NuMI beamline and can decay into an active neutrino and a muon and anti-muon pair either within ArgoNe uT or in the cavern upstream of the detector. This talk presents a search for such HNLs with ArgoNeuT and the resulting new constraints on the HNL m ass and mixing angles.\n\nhttps://indico.ific.uv.es/event/6178/contributio ns/15705/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15705/ END:VEVENT BEGIN:VEVENT SUMMARY:Solar Neutrino Detection Sensitivity in DARWIN via Electron Scatte ring DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15720@indico.ific.uv.es DESCRIPTION:Speakers: Shayne Reichard ()\nThe proposed liquid xenon observ atory DARWIN will exhibit sensitivity to solar neutrinos via elastic elect ron scattering. In this channel\, DARWIN will have the potential to measur e the fluxes of five solar neutrino components: $pp$\, $^7$Be\, $^{13}$N\, $^{15}$O and $pep$. The precision of the $^{13}$N\, $^{15}$O and $pep$ co mponents is hindered by the double-beta decay of $^{136}$Xe and\, thus\, w ould benefit from a depleted target. A high-statistics observation of $pp$ neutrinos would allow for measurements of the electroweak mixing angle\, $\\sin^2\\theta_w$\, and the electron-type neutrino survival probability\, $P_{ee}$\, in the electron recoil energy region from a few keV up to 200 keV for the first time\, with relative precision of 5% and 4%\, respective ly\, with 10 live years of data and a 30 tonne fiducial volume. An observa tion of $pp$ and $^7$Be neutrinos would constrain the neutrino-inferred so lar luminosity to 0.2%. A combination of all flux measurements would disti nguish between the high- (GS98) and low-metallicity (AGS09) solar models w ith 2.1-2.5$\\sigma$ significance\, independent of external measurements f rom other experiments or a measurement of $^8$B neutrinos through coherent elastic neutrino-nucleus scattering in DARWIN. Finally\, it is demonstrat ed that with a depleted target DARWIN may be sensitive to the neutrino cap ture process of $^{131}$Xe.\n\nhttps://indico.ific.uv.es/event/6178/contri butions/15720/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15720/ END:VEVENT BEGIN:VEVENT SUMMARY:A New Approach to Probe Non-Standard Interactions in Atmospheric N eutrino Experiments DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15632@indico.ific.uv.es DESCRIPTION:Speakers: Anil Kumar (Institute of Physics\, Bhubaneswar)\nWe propose a new approach to explore the neutral-current non-standard neutri no interactions (NSI) in atmospheric neutrino experiments using oscillatio n dips and valleys in reconstructed muon observables\, at a detector like ICAL that can identify the muon charge. We focus on the flavor-changing NS I parameter $\\varepsilon_{\\mu\\tau}$\, which has the maximum impact on t he muon survival probability in these experiments. We show that non-zero $ \\varepsilon_{\\mu\\tau}$ shifts the oscillation dip locations in $L/E$ di stributions of the up/down event ratios of reconstructed $\\mu^-$ and $\\m u^+$ in opposite directions. We introduce a new variable $\\Delta d$ repre senting the difference of dip locations in $\\mu^-$ and $\\mu^+$\, which i s sensitive to the magnitude as well as the sign of $\\varepsilon_{\\mu\\t au}$\, and is independent of the value of $\\Delta m^2_{32}$. We further n ote that the oscillation valley in the ($E$\, $\\cos \\theta$) plane of th e reconstructed muon observables bends in the presence of NSI\, its curvat ure having opposite signs for $\\mu^-$ and $\\mu^+$. We demonstrate the id entification of NSI with this curvature\, which is feasible for detectors like ICAL having excellent muon energy and direction resolutions. We illus trate how the measurement of contrast in the curvatures of valleys in $\\m u^-$ and $\\mu^+$ can be used to estimate $\\varepsilon_{\\mu\\tau}$. Usin g these proposed oscillation dip and valley measurements\, the achievable precision on $|\\varepsilon_{\\mu\\tau}|$ at 90% C.L. is about 2% with 500 kt$\\cdot$yr exposure. The effects of statistical fluctuations\, systemat ic errors\, and uncertainties in oscillation parameters have been incorpor ated using multiple sets of simulated data. Our method would provide a dir ect and robust measurement of $\\varepsilon_{\\mu\\tau}$ in the multi-GeV energy range.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15632/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15632/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino NSI effects on future solar sector measurements DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15630@indico.ific.uv.es DESCRIPTION:Speakers: Susana Molina Sedgwick (IFIC (CSIC-Univ Valencia))\n The next-generation neutrino experiment JUNO will determine the solar osci llation parameters - $\\sin^2 \\theta_{12}$ and $\\Delta m^2_{21}$ - with great accuracy\, in addition to measuring $\\sin^2\\theta_{13}$\, $\\Delta m^2_{31}$ and the mass ordering. In parallel\, the continued study of sol ar neutrinos at Hyper-Kamiokande will provide complementary measurements i n the solar sector. In this talk\, I will present the expected sensitivity to non-universal and flavour-changing non-standard interactions (NSI) wit h $d$-type quarks from the combination of these two future experiments. I will also discuss the robustness of solar oscillation parameter measuremen ts in the presence of NSI and comment on the enduring potential viability of the LMA-D solution.\n\nhttps://indico.ific.uv.es/event/6178/contributio ns/15630/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15630/ END:VEVENT BEGIN:VEVENT SUMMARY:Observation of CNO cycle solar neutrinos in Borexino DTSTART;VALUE=DATE-TIME:20210902T154000Z DTEND;VALUE=DATE-TIME:20210902T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15590@indico.ific.uv.es DESCRIPTION:Speakers: Oemer Penek (IKP-2 Forschungszentrum Juelich)\nThe B orexino detector\, located at the Laboratori Nazionali del Gran Sasso in I taly\, is a radiopure 280 ton liquid scintillator detector with a primary goal to measure low-energy solar neutrinos created in the core of the Sun. These neutrinos are a consequence of nuclear fusion reactions in the sola r core where Hydrogen is burned into Helium and provide a direct probe of the energy production processes\, namely the proton-proton ($pp$) chain an d the Carbon-Nitrogen-Oxygen (CNO) cycle. The fusion of Hydrogen in the ca se of the CNO cycle\, which is expected to contribute in the order of less than $\\sim\\\,1\\%$ to the total solar energy\, is catalyzed by Carbon\, Nitrogen\, and Oxygen directly depending on the abundances of these eleme nts in the solar core. Neutrinos from the $pp$ chain have been studied in Borexino with outstanding precision through the measurement of $pp$\, $pep $\, $^{7}$Be\, and $^{8}$B neutrinos over the past decade\, while the exis tence of neutrinos from the CNO cycle have been confirmed recently for the first time with a high statistical significance. The measurement of CNO n eutrinos is challenging due to the high spectral correlation with the deca y electrons of the background isotope $^{210}$Bi and the $pep$ solar neutr ino signal. The experimental achievement of thermal stabilization of the B orexino detector after mid 2016\, has opened the possibility to develop a method to constrain the $^{210}$Bi rate through its decay daughter and $\\ alpha$ emitter $^{210}$Po which can be identified in Borexino with an effi ciency close to $100$ percent on an event-by-event basis. Moreover\, the flux of $pep$ neutrinos can be constrained precisely through a global anal ysis of solar neutrino data which is independent of the dataset used for t he CNO analysis. This talk is dedicated to the first experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun which is at the same time the dominant energy production mechanism in heavier stars compar ed to the Sun in the Universe.\n\nhttps://indico.ific.uv.es/event/6178/con tributions/15590/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15590/ END:VEVENT BEGIN:VEVENT SUMMARY:Spectroscopy of geoneutrinos with Borexino DTSTART;VALUE=DATE-TIME:20210902T152500Z DTEND;VALUE=DATE-TIME:20210902T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15586@indico.ific.uv.es DESCRIPTION:Speakers: Sindhujha Kumaran (IKP-2 Forschungszentrum Jülich a nd RWTH Aachen University)\nBorexino is a 280-ton liquid scintillator dete ctor located at the Laboratori Nazionali del Gran Sasso (LNGS)\, Italy and is one of the two detectors that has measured geoneutrinos so far. The un precedented radio-purity of the scintillator\, the shielding with highly p urified water\, and the placement of the detector at 3800 m w.e. depth hav e resulted in very low background levels\, making Borexino an excellent ap paratus for geoneutrino measurements. This talk will summarize the latest geoneutrino analysis with Borexino\, using the data obtained from December 2007 to April 2019. The updated statistics and the optimized analysis tec hniques such as an increased fiducial volume and sophisticated cosmogenic vetoes\, have led to more than a factor two increase in exposure when comp ared to the previous measurement in 2015\, resulting in a significant impr ovement in the precision. In addition\, Borexino was also able to reject t he null hypothesis of the mantle geoneutrino signal with 99% C.L.\, for th e first time\, by exploiting the detailed knowledge of the crust surroundi ng the detector. This talk will also include other geological interpretati ons of the obtained results such as the calculation of the radiogenic heat and the comparison of the results to various predictions. Additionally\, upper limits for a hypothetical georeactor that might be present at differ ent locations inside the Earth will also be discussed.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15586/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15586/ END:VEVENT BEGIN:VEVENT SUMMARY:Study of Ocean Bottom Detector for observation of geo-neutrinos fr om the mantle DTSTART;VALUE=DATE-TIME:20210902T151000Z DTEND;VALUE=DATE-TIME:20210902T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15583@indico.ific.uv.es DESCRIPTION:Speakers: Taichi Sakai (Tohoku Univ. Research Center for Neutr ino Science)\nObservation of anti-neutrinos emitted from radioactive isoto pes inside the Earth(geo-neutrinos) bring direct information on the Earth ’s chemical composition and its heat balance\, which strongly relate to the Earth’s dynamics.\nTo date\, two experiments (KamLAND and Borexino) have measured geo-neutrinos and constrained the range of acceptable models for the Earth’s composition\, but distinguishing the mantle flux by lan d-based detectors is challenging as the crust signal is about 70 % of the total anti-neutrino flux. \nGiven the oceanic crust is thinner than contin ental crust and has lower concentration of radioactive elements\, geo-neu trino detector in the ocean\, Ocean Bottom Detector (OBD)\, makes it sensi tive to geo-neutrinos originating from the Earth’s mantle. Another uniq ue feature of OBD is keeping the distance from the reactors which are the main background sources for land-based detectors. In addition\, this mova ble detector can observe at multiple points in the ocean.\nOur working gro up was jointly constructed from interdisciplinary communities in Japan whi ch include particle physics\, geoscience\, and ocean engineering. We have started to work on technological developments of OBD.\nIn this presentati on\, I present the status of development and future plan.\n\nhttps://indic o.ific.uv.es/event/6178/contributions/15583/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15583/ END:VEVENT BEGIN:VEVENT SUMMARY:Generalizing the Scotogenic model DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15631@indico.ific.uv.es DESCRIPTION:Speakers: Pablo Escribano Valiente (IFIC (CSIC-Univ Valencia)) \nThe Scotogenic model is an economical setup that induces Majorana neutri no masses at the 1-loop level and includes a dark matter candidate. We dis cuss a generalization of the original Scotogenic model with arbitrary numb ers of generations of singlet fermion and inert doublet scalar fields. Fir st\, the full form of the light neutrino mass matrix is presented\, with s ome comments on its derivation and with special attention to some particul ar cases. The behavior of the theory at high energies is explored by solvi ng the Renormalization Group Equations.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15631/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15631/ END:VEVENT BEGIN:VEVENT SUMMARY:Short-Baseline neutrino oscillation searches with the ICARUS detec tor DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15542@indico.ific.uv.es DESCRIPTION:Speakers: Christian Farnese (INFN Padova)\nThe ICARUS collabor ation employed the 760-ton T600 detector in a successful three-year physic s run at the underground LNGS laboratories studying neutrino oscillations with the CNGS neutrino beam from CERN\, and searching for atmospheric neut rino interactions. ICARUS performed a sensitive search for LSND-like anoma lous νe appearance in the CNGS beam\, which contributed to the constraint s on the allowed parameters to a narrow region around 1 eV$^2$\, where all the experimental results can be coherently accommodated at 90% C.L. Afte r a significant overhaul at CERN\, the T600 detector has been installed at Fermilab. In 2020 cryogenic commissioning began with detector cool down\, liquid Argon filling and recirculation. ICARUS has started operations and is presently in its commissioning phase\, collecting the first neutrino e vents from the Booster Neutrino Beam and the NuMI off-axis. The main goal of the first year of ICARUS data taking will then be the definitive verifi cation of the recent claim by NEUTRINO-4 short baseline reactor experiment both in the $\\nu_\\mu$ channel with the BNB and in the $\\nu_e$ with NuM I. After the first year of operations\, ICARUS will commence its search fo r evidence of a sterile neutrino jointly with the SBND near detector\, wit hin the Short Baseline Neutrino (SBN) program. The ICARUS exposure to the NuMI beam will also give the possibility for other physics studies such as light dark matter searches and neutrino-Argon cross section measurements. The proposed contribution will address ICARUS achievements\, its status a nd plans for the new run at Fermilab and the ongoing developments of the a nalysis tools needed to fulfill its physics program.\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/15542/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15542/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of Neutrino Elastic-scattering Observation with NaI(Tl) exp eriment (NEON) DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15714@indico.ific.uv.es DESCRIPTION:Speakers: Insoo Lee (IBS)\nCoherent elastic neutrino-nucleus s cattering (CEvNS) has important role for measuring neutrino properties and proving non-standard interactions.\n\nNeutrino Elastic-scattering Observa tion with NaI(Tl) experiment (NEON) aims to detect this CEvNS in an NaI(Tl ) crystal using reactor anti-electron neutrino at Hanbit nuclear power pla nt.\n\nNEON detector which is installed 24 m distance away from the active reactor core consists of a 15 kg NaI(Tl) in the radiation shielding struc tures including a ~700 L liquid scintillator.\n\nData taking has started f rom December 2020 which includes 1 month reactor-off period.\n\nWe report the current status of NEON experiment in this talk.\n\nhttps://indico.ific .uv.es/event/6178/contributions/15714/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15714/ END:VEVENT BEGIN:VEVENT SUMMARY:Physics reach of a Scintillating Bubble Chamber in CEvNS and its i nterplay with DM direct searches for extra vector mediators DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15681@indico.ific.uv.es DESCRIPTION:Speakers: Eduardo Peinado (Instituto de Fisica UNAM)\nWe will discuss the physics reach of a low threshold (100 eV) scintillating argon bubble chamber sensitive to Coherent Elastic neutrino-Nucleus Scattering ( CEνNS) from reactor neutrinos.  We will focus on the sensitivity for a l ight Z′ gauge boson mediator\, and also review the complementarity of su ch experiment with DM direct detection experiments when the DM interacts w ith the light mediator.\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15681/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15681/ END:VEVENT BEGIN:VEVENT SUMMARY:Gaseous detectors for Neutrino-nucleus coherent scattering at the ESS DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15569@indico.ific.uv.es DESCRIPTION:Speakers: Francesc Monrabal (DIPC)\nThe recent detection of th e coherent elastic neutrino-nucleus scattering (CEνNS )opens the possibil - ity to use neutrinos to explore physics beyond standard model with small size detectors. However\, the CEνNS process generates signals at the few keV level\, requiring of very sensitive detecting technologies for its de tection.\nThe European Spallation Source (ESS) has been identified as an o ptimal source of low energy neutrinos offering an opportunity for a defini tive exploration of all phenomenological applications of CEνNS. In this p roject I propose apply the high pressure xenon gas TPC technology to the d etection of the CEνNS process at the ESS. This will require the developme nt of very low-energy detectors and to improve the current knowledge of th e quenching factor for nuclear recoils in xenon gas at keV energies. The m ajor goal of this project is to build a 20 kg xenon gaseous detector and o perate it at the ESS\, such detector will provide more than 7\,000 CEνNS events per year\, overtaking the sensitivities of much larger detectors in current spallations sources.\nIn this talk I’ll present the advantages of the gaseous TPC technology to exploit the physics of the CEνNS process and the experimental program towards the construction and operation of a gaseous detector at the ESS.\n\nhttps://indico.ific.uv.es/event/6178/contr ibutions/15569/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15569/ END:VEVENT BEGIN:VEVENT SUMMARY:Low-energy reactor neutrino physics with the CONNIE experiment DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15703@indico.ific.uv.es DESCRIPTION:Speakers: Irina Nasteva (Federal University of Rio de Janeiro (BR))\nThe Coherent Neutrino-Nucleus Interaction Experiment (CONNIE) uses fully depleted high-resistivity CCDs (charge coupled devices) with the aim of detecting the coherent elastic scattering of reactor antineutrinos wit h silicon nuclei and probing physics beyond the Standard Model. CONNIE is located at a distance of about 30 m from the core of the 3.8 GW Angra-2 nu clear reactor in Rio de Janeiro\, Brazil. The experiment has been taking d ata since 2016 with a noise level of less than 2 electrons RMS and an acti ve mass of 50 g. The analysis of the 2016-2018 data allowed us to set a 95 % C.L. upper limit on the coherent scattering rate\, which was used to pla ce stringent constraints on simplified extensions of the Standard Model wi th light mediators. Currently\, the experiment is operating with an improv ed readout and a lower energy threshold of 50 eV. We present the performan ce of the CONNIE experiment and new results of the blind analysis of 2019 data. We also report on the ongoing upgrade and the prospects for detectin g the coherent elastic scattering of reactor neutrinos with the new detect or technology of skipper CCDs.\n\nhttps://indico.ific.uv.es/event/6178/con tributions/15703/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15703/ END:VEVENT BEGIN:VEVENT SUMMARY:Detecting CEνNS and searching for new physics at reactor site wit h the CONUS experiment DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15589@indico.ific.uv.es DESCRIPTION:Speakers: Aurélie Bonhomme (MPIK Heidelberg)\nThe detection o f neutrinos through the coherent elastic neutrino-nucleus scattering (CEν NS) process opens a new window to study the fundamental properties of this elusive particle and to probe physics beyond the Standard Model. The CONU S experiment – operational since April 2018 – is located at a distance of 17m from the 3.9GWth core of the nuclear power plant Brokdorf (Germany ). It aims to detect CEνNS in the fully coherent regime with four 1 kg HP Ge point-contact detectors with a ~300eVee energy threshold.\nThe full spe ctral analysis of the first CONUS data set allows to set the current best limit on CEνNS with reactor antineutrinos and to deduce competitive limit s on physics beyond the standard model\, such as non-standard neutrino int eractions or the neutrino magnetic moment. These new results will be prese nted in this talk. Special emphasis will be put on the strategy followed b y the collaboration to further reduce the systematic uncertainties\, in pa rticular via a dedicated measurement of the ionization quenching factor of nuclear recoils in germanium.\n\nhttps://indico.ific.uv.es/event/6178/con tributions/15589/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15589/ END:VEVENT BEGIN:VEVENT SUMMARY:Exploring Coherent Elastic Neutrino-Nucleus Scattering of Reactor Neutrinos with the NUCLEUS Experiment DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15578@indico.ific.uv.es DESCRIPTION:Speakers: Victoria Wagner (Technische Universität München)\n Coherent elastic neutrino nucleus scattering (CE$\\nu$NS) offers a unique way to study neutrino properties and to search for new physics beyond the Standard Model. The NUCLEUS experiment aims to measure CE$\\nu$NS of react or anti-neutrinos down to unprecedented low nuclear recoil energies. The n ovel gram-scale fiducial-volume cryogenic detectors feature an ultra-low e nergy threshold of $\\sim$20 eV in nuclear recoil and a rise time of a few 100 $\\mu$s which allows the operation above ground. The fiducialization of the detectors provides an effective discrimination of ambient $\\gamma$ - and surface backgrounds. Furthermore\, the use of multiple targets promi ses a high physics potential.\nThe NUCLEUS experiment will be located at a new experimental site at the Chooz nuclear power plant in France\, provid ing a high average anti-neutrino flux of $1.7\\cdot10^{12}\\\,\\bar{\\nu_e }/(\\text{s}\\cdot\\text{cm}^2)$. The commissioning of the full experiment al setup is planned for 2022. This talk will review the physics potential of NUCLEUS and its current status.\n\nhttps://indico.ific.uv.es/event/617 8/contributions/15578/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15578/ END:VEVENT BEGIN:VEVENT SUMMARY:Physics reach of the ESSnuSB experiment DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15573@indico.ific.uv.es DESCRIPTION:Speakers: Monojit Ghosh (Ruder Boskovic Institute)\nESSnuSB pr oject is a design study for an upcoming accelerator-based neutrino oscilla tion experiment which will be driven by the ESS proton accelerator. The pr imary goal of this experiment is to measure the leptonic CP-violation phas e with high precision at the second oscillation maximum. In this presentat ion\, I will discuss the physics sensitivities of the proposed ESSnuSB exp eriment. In particular\, I will discuss its capability to measure the lept onic CP phase\, neutrino mass hierarchy\, octant of the atmospheric mixing angle and the precision of atmospheric mixing angle and atmospheric mass squared difference. Further\, I will discuss how the matter density can af fect the CP measurement capability of ESSnuSB. In addition\, I will also d iscuss the capability of this experiment to probe two of the new physics s cenarios which are (i) light sterile neutrinos and (ii) invisible neutrino decay.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15573/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15573/ END:VEVENT BEGIN:VEVENT SUMMARY:First results of nuGeN experiment at Kalinin Nuclear Power Plant o n coherent elastic neutrino-nucleus scattering DTSTART;VALUE=DATE-TIME:20210901T154000Z DTEND;VALUE=DATE-TIME:20210901T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15547@indico.ific.uv.es DESCRIPTION:Speakers: Alexey Lubashevskiy (JINR)\nThe $\\nu$GeN project is aimed to study neutrino scattering at the close vicinity of the reactor c ore of Kalinin Nuclear Power Plant (KNPP). Its main interests are connecte d with the detection of coherent elastic neutrino-nucleus scattering (CE$\ \nu$NS) and the search for the magnetic moment of neutrino. The experiment al setup is constructed under reactor unit #3 of KNPP at a distance of abo ut 10 m from the center of the 3.1 GW$_{th}$ core. In this way\, we obtain an enormous antineutrino flux of more than 5x10$^{13}$ $\\nu$/cm$^2$/s. M aterials of the reactor surrounding provide about 50 m w.e. overburden\, t hat serves as a good shielding against cosmic radiation. In combination wi th low ambient background\, it gives us a unique opportunity to investigat e antineutrino properties at the best location in the world. A special lif ting mechanism allows moving the spectrometer towards to the reactor core changing the neutrino flux and thus suppressing main systematic errors cau sed by possible long-term instability and insufficient knowledge of neutri no flux. To detect signals from the neutrino scattering we use high-purity low-threshold germanium detectors surrounded by passive and active shield ings. A specially developed acquisition system allows suppressing noisy ev ents. A detailed description of the experimental setup will be presented. In 2021 we finished optimization of the experimental setup and performed t he first dedicated search of the CE$\\nu$NS in the framework of our projec t by comparing the experimental spectra taken with regimes of reactor ON a nd OFF. The results of this analysis will be presented for the first time. \n\nhttps://indico.ific.uv.es/event/6178/contributions/15547/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15547/ END:VEVENT BEGIN:VEVENT SUMMARY:Electromagnetic neutrino: The theory\, laboratory experiments and astrophysical probes DTSTART;VALUE=DATE-TIME:20210901T152500Z DTEND;VALUE=DATE-TIME:20210901T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15530@indico.ific.uv.es DESCRIPTION:Speakers: Alexander Studenikin (Moscow State University & JINR (Dubna))\nIn the present talk we continue our discussions [1-5] on neutri no electromagnetic properties and start with a short introduction to the d erivation of the general structure of the electromagnetic form factors of Dirac and Majorana neutrinos. \n\nThen we consider experimental constrain ts on neutrino magnetic and electric dipole moments\, electric millicharge \, charge radii and anapole moments from the terrestrial laboratory experi ments (the bounds obtained by the reactor MUNU\, TEXONO and GEMMA experime nts and the solar Super-Kamiokande and the recent Borexino experiments). A special credit is done to the most severe constraints on neutrino magneti c moments\, millicharge and charge radii [6-10]. The world best reactor [6 ] and solar [7] neutrino and astrophysical [11\,12] bounds on neutrino mag netic moments\, as well as bounds on millicharge from the reactor neutrino s [8] are included in the recent issues of the Review of Particle Physics (see the latest Review: P.A. Zyla et al. (Particle Data Group)\, Prog. The or. Exp. Phys. 2020\, 083C01). The best astrophysical bound on neutrino m illicharge was obtained in [13]. The most severe astrophysical bound on n eutrino magnetic moment has been obtained recently in [14].\n\nIn the rece nt studies [15] it is shown that the puzzling results of the XENON1T colla boration [16] at few keV electronic recoils could be due to the scattering of solar neutrinos endowed with finite Majorana transition magnetic mome nts of the strengths lie within the limits set by the Borexino experiment with solar neutrinos [7]. The comprehensive analysis of the existing and n ew extended mechanisms for enhancing neutrino transition magnetic moments to the level appropriate for the interpretation of the XENON1T data and le aving neutrino masses within acceptable values is provided in [17].\n\nCon sidering neutrinos from all known sources\, as well as including all avail able data from XENON1T and Borexino\, the strongest up-to-date exclusion l imits on the active-to-sterile neutrino transition magnetic moment are der ived in [18] .\n\nA comprehensive analisys of constraints on neutrino elec tric millicharge from experiments of elastic neutrino-electron interaction and future prospects involving coherent elastic neutrino-nucleus scatteri ng is presented in [19]. \n\nWe also present results of the recent detaile d study [20] of the electromagnetic interactions of massive neutrinos in t he theoretical formulation of low-energy elastic neutrino-electron scatter ing. The formalism of neutrino charge\, magnetic\, electric\, and anapole form factors defined as matrices in the mass basis with account for three- neutrino mixing is presented. Using the derived new expression for a neut rino electromagnetic scattering cross section [20]\, we further developed studies of neutrino electromagnetic properties using the COHERENT data [9] and obtained [10] new bounds on the neutrino charge radii from the COHERE NT experiment. Worthy of note\, our paper [10] has been included by the E ditors Suggestion to the Phys. Rev. D “Highlights of 2018”\, and t he obtained constraints on the nondiagonal neutrino charge radii since 201 9 has been included by the Particle Data Group to the Review of Particle P hysics.\n\nThe main manifestation of neutrino electromagnetic interactions \, such as: 1) the radiative decay in vacuum\, in matter and in a magnetic field\, 2) the neutrino Cherenkov radiation\, 3) the plasmon decay to neu trino-antineutrino pair\, 4) the neutrino spin light in matter\, and 5) th e neutrino spin and spin-flavour precession are discussed. Phenomenologi cal consequences of neutrino electromagnetic interactions (including the s pin light of neutrino [21]) in astrophysical environments are also reviewe d. \n\nThe second part of the proposed talk is dedicated to results of our mostly recently performed detailed studies of new effects in neutrino spi n\, spin-flavour and flavor oscillations under the influence of the transv ersal matter currents [22\, 23] and a constant magnetic field [24\,25]\, a s well as to our newly developed approach to the problem of the neutrino q uantum decoherence [26] and also to our recent proposal [27] for an experi mental setup to observe coherent elastic neutrino-atom scattering (CEνAS) using electron antineutrinos from tritium decay and a liquid helium targe t that as we have estimated opens a new frontier in constraining the neutr ino magnetic moment. \n\nThe discussed in the second part of the talk new results include two new effects that can be summarized as follows:\n\n1) as it was shown for the first time in [22] neutrino spin and spin-flavor o scillations can be engendered by weak interactions of neutrinos with the m edium in the case when there are the transversal matter currents\; in [23] the quantum treatment of these phenomena is presented and different possi bilities for the resonance amplification of oscillations are discussed\, t he neutrino Standard Model and non-standard interactions are accounted for \; \n\n2) within a new treatment [24] of the neutrino flavor\, spin and sp in-flavour oscillations in the presence of a constant magnetic field\, whi ch is based on the use of the exact neutrino stationary states in the magn etic field\, it is shown that there is an interplay of neutrino oscillatio ns on different frequencies. In particular: a) the amplitude of the flavo ur oscillations νLe↔ νLμ at the vacuum frequency is modulated by the magnetic field frequency μB \, and b) the neutrino spin oscillation prob ability (without change of the neutrino flavour) exhibits the dependence o n the neutrino energy and mass square difference Δm2 . \n\nThe discovere d new phenomena in neutrino oscillations should be accounted for reinterpr etation of results of already performed experiments on detection of astrop hysical neutrino fluxes produced in astrophysical environments with strong magnetic fields and dense matter. These new neutrino oscillation phenomen a are also of interest in view of future experiments on observations of su pernova neutrino fluxes with large volume detectors like DUNE\, JUNO and H yper-Kamiokande.\n\nThree other new results discussed in the concluding pa rt of the talk are as follows:\n\n3) a new theoretical framework\, based o n the quantum field theory of open systems applied to neutrinos\, has been developed [26] to describe the neutrino evolution in external environment s accounting for the effect of the neutrino quantum decoherence\; we have used this approach to consider a new mechanism of the neutrino quantum dec oherence engendered by the neutrino radiative decay to photons and dark ph otons in an astrophysical environment\, the corresponding new constraints on the decoherence parameter have been obtained\; \n\n4) in [27] we have p roposed an experimental setup to observe coherent elastic neutrino-atom sc attering (CEνAS) using electron antineutrinos from tritium decay and a li quid helium target and shown that the sensitivity of this apparatus (when using 60 g of tritium) to a possible electron neutrino magnetic moment ca n be of order about 7×10−13μB at 90% C.L.\, that is more than one orde r of magnitude smaller than the current experimental limit\;\n\n5) in our most recent paper [28] we investigate effects of non-zero Dirac and Major ana CP violating phases on neutrinoantineutrino oscillations in a magnetic field of astrophysical environments\; it is shown that in the presence of strong magnetic fields and dense matter\, non-zero CP phases can induce n ew resonances in the oscillations channels ν e ↔ ν¯e\, νe ↔ ν¯µ and νe ↔ ν¯τ \; the resonances can potentially lead to significant phenomena in neutrino oscillations accessible for observation in experime nts\; the detection of supernovae neutrino fluxes in the future experiment s\, such as JUNO\, DUNE and Hyper-Kamiokande\, can give an insight into th e nature of CP violation and\, consequently\, provides a tool for distingu ishing the Dirac or Majorana nature of neutrinos.\n\nThe best world experi mental bounds on neutrino electromagnetic properties are confronted with t he predictions of theories beyond the Standard Model. It is shown that stu dies of neutrino electromagnetic properties provide a powerful tool to pro be physics beyond the Standard Model.\n\nThis research has been supported by the Interdisciplinary Scientific and Educational School of Moscow Unive rsity “Fundamental and Applied Space Research” and also by the Russian Foundation for Basic Research under Grant No. 20-52-53022-GFEN-a.\n\n\nRe ferences:\n\n[1] A. Studenikin\, Neutrino magnetic moment: A window to new physics\, Nucl.Phys.B Proc.Suppl. 188 (2009) 220.\n\n[2] C. Guinti and A. Studenikin\, Neutrino electromagnetic interactions: A window to new physi cs\, Rev. Mod. Phys. 87 (2015) 531-591.\n\n[3] C. Giunti\, K. Kouzakov\ , Y. F. Li\, A. Lokhov\, A. Studenikin\, S. Zhou\, Electromagnetic neutrin os in laboratory experiments and astrophysics\, Annalen Phys. 528 (2016) 198.\n\n[4] A. Studenikin\, Neutrino electromagnetic interactions: A wind ow to new physics - II\,\nPoS EPS-HEP2017 (2017) 137.\n\n[5] A. Studenikin \, Electromagnetic neutrino properties: new constraints and new effects\,\ nPoS ICHEP2020 (2021)180.\n\n[6] A. Beda\, V. Brudanin\, V. Egorov et al. \, The results of search for the neutrino magnetic\nmoment in GEMMA experi ment \, Adv. High Energy Phys. 2012 (2012) 350150.\n\n[7] M. Agostini et a l (Borexino coll.)\, Limiting neutrino magnetic moments with Borexino Phas e-II solar neutrino data\, Phys. Rev. D 96 (2017) 091103.\n\n[8] A. Stude nikin\, New bounds on neutrino electric millicharge from limits on neutrin o magnetic moment\, Europhys. Lett. 107 (2014) 21001.\n\n[9] D. Papoulia s\, T. Kosmas\, COHERENT constraints to conventional and exotic neutrino p hysics\, Phys. Rev. D 97 (2018) 033003.\n\n[10] M. Cadeddu\, C. Giunti\, K. Kouzakov\, Y.F. Li\, A. Studenikin\, Y.Y. Zhang\, Neutrino charge rad ii from COHERENT elastic neutrino-nucleus scattering\, Phys. Rev. D 98 ( 2018) 113010.\n\n[11] N. Viaux\, M. Catelan\, P. B. Stetson\, G. G. Raffel t et al.\, Particle-physics constraints from the globular cluster M5: neut rino dipole moments\, Astron. & Astrophys. 558 (2013) A12.\n\n[12] S. Arce o-Díaz\, K.-P. Schröder\, K. Zuber and D. Jack\, Constraint on the magne tic dipole moment of neutrinos by the tip-RGB luminosity in ω-Centauri\, Astropart. Phys. 70 (2015) 1.\n\n[13] A. Studenikin\, I. Tokarev\, Mill icharged neutrino with anomalous magnetic moment in rotating magnetized ma tter\, Nucl. Phys. B 884 (2014) 396-407.\n\n[14] F. Capozzi and G. Raffelt \, Axion and neutrino bounds improved with new calibrations of the tip of the red-giant branch using geometric distance determinations\, Phys.Rev.D 102 (2020) 083007\, arXiv:2007.03694v4 (24 Mar 2021).\n\n[15] O. G. Miran da\, D. K. Papoulias\, M. Tórtola\, J. W. F. Valle\, XENON1T signal from transition neutrino magnetic moments \, Phys.Lett. B 808 (2020) 135685.\n\ n[16] E. Aprile et al. [XENON]\, Observation of excess electronic recoil E vents in XENON1T\, Phys. Rev. D 102 (2020) 072004.\n\n[17] K. Babu\, S. Ja na\, M. Lindner\, Large neutrino magnetic moments in the light of recent e xperiments\, JHEP 2010 (2020) 040. \n\n[18] V. Brdar\, A. Greljo\, J. Kop p\, T. Opferkuch\, The neutrino magnetic moment portal: Cosmology\, astrop hysics\, and direct detection\, JCAP01 (2021) 039.\n\n[19] A. Parada\, Con straints on neutrino electric millicharge from experiments of elastic neut rino-electron interaction and future experimental proposals involving cohe rent elastic neutrino-nucleus scattering\, Adv.High Energy Phys. 2020 (202 0) 5908904.\n\n[20] K. Kouzakov\, A. Studenikin\, Electromagnetic proper ties of massive neutrinos in low-energy\nelastic neutrino-electron scatter ing\, Phys. Rev. D 95 (2017) 055013. \n\n[21] A. Grigoriev\, A. Lokhov\, A. Studenikin\, A. Ternov\, Spin light of neutrino in astrophysical enviro nments\, JCAP 1711 (2017) 024 (23 p.).\n\n[22] A. Studenikin\, Neutrinos in electromagnetic fields and moving media\, Phys. At. Nucl. 67 (2004) 99 3.\n\n[23] P. Pustoshny\, A. Studenikin\, Neutrino spin and spin-flavour oscillations in transversal\nmatter currents with standard and non-sta ndard interactions\, Phys. Rev. D 98 (2018) 113009.\n\n[24] A. Popov\, A. Studenikin\, Neutrino eigenstates and flavour\, spin and spin-flavour o scillations in a constant magnetic field\, Eur. Phys. J. C 79 (2019) 144.\ n\n[25] P. Kurashvili\, K. Kouzakov\, L. Chotorlishvili\, A. Studenikin\, Spin-flavor oscillations of ultrahigh-energy cosmic neutrinos in interste llar space: The role of neutrino magnetic moments”\, Phys. Rev. D 96 (20 17) 103017.\n\n[26] K. Stankevich\, A. Studenikin\, Neutrino quantum decoh erence engendered by neutrino radiative decay\, Phys. Rev. D 101 (2020) 056004.\n\n[27] M. Cadeddu\, F. Dordei\, C. Giunti\, K. Kouzakov\, E. Picc iau\, A. Studenikin\, Potentialities of a low-energy detector based on 4H e evaporation to observe atomic effects in coherent neutrino scattering an d physics perspectives\, Phys. Rev. D 100 (2019) 073014.\n\n[28] A. Popov\ , A. Studenikin\, Manifestations of non-zero Majorana CP violating phases in oscillations of supernova neutrinos\, Phys. Rev. D 103 (2021) 115027.\n \nhttps://indico.ific.uv.es/event/6178/contributions/15530/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15530/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing exotic neutrino physics with CEvNS and neutrino-electron s cattering DTSTART;VALUE=DATE-TIME:20210901T151000Z DTEND;VALUE=DATE-TIME:20210901T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15529@indico.ific.uv.es DESCRIPTION:Speakers: Dimitrios Papoulias (University of Ioannina)\nNuclea r and electron recoil measurements are a substantial tool for investigatin g novel neutrino physics phenomena at low-energies. In this talk I will di scuss the current constraints on non-standard interactions (NSIs) and elec tromagnetic neutrino properties\, obtained from the recent observation of coherent elastic neutrino-nucleus scattering (CEvNS) by COHERENT as well a s from the recent XENON1T excess of electron recoil events.\n\nhttps://ind ico.ific.uv.es/event/6178/contributions/15529/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15529/ END:VEVENT BEGIN:VEVENT SUMMARY:Novel Studies on Neutral Bremsstrahlung in Xenon Optical TPCs DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15712@indico.ific.uv.es DESCRIPTION:Speakers: Cristina M. B. Monteiro (University of Coimbra)\nWe have measured\, for the first time in pure Xe\, non-excimer-based secondar y scintillation\, Neutral Bremsstrahlung (NBrS)\, in a dedicated setup bas ed on a Gas Proportional Scintillation Counter. \nThe emission of NBrS by drifting electrons occurs even for electric field values below the gas exc itation threshold. We have shown the presence of NBrS in the NEXT-White TP C\, at present the largest optical HPXe-TPC in operation.\nMoreover\, for field values above 1 kV/cm/bar\, as typically employed for electroluminesc ence (EL)\, there is consistent evidence that NBrS is present with an inte nsity about two orders of magnitude lower than conventional\, excimer-base d\, EL.\nOur data show excellent agreement with calculations of NBrS yield . \nDespite fainter than EL\, in pure xenon\, this new source of emission has to be accounted for in Xe optical TPCs and may play an important role in future single-phase LXe TPCs.\n\nhttps://indico.ific.uv.es/event/6178/c ontributions/15712/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15712/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino Physics in XENONnT DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15706@indico.ific.uv.es DESCRIPTION:Speakers: Abigail Kopec (Purdue University\, XENON Collaborati on)\nThe XENONnT experiment is an ultra-low background liquid xenon Time P rojection Chamber at the Gran Sasso National Laboratory in Italy. Beyond its primary science goal to detect WIMP dark matter\, XENONnT will be high ly sensitive to a variety of rare neutrino processes. The previous XENON1T measured the half-life of the two-neutrino double-electron capture proces s of Xenon-124. In XENONnT\, with a few hundred kilograms of Xenon-136 in the fiducial volume\, we will search for hints of neutrinoless double beta decay. Several detector upgrades improve XENONnT's sensitivity to low-ene rgy interactions with neutrinos directly. Through coherent elastic neutrin o-nucleus scattering\, XENONnT will measure solar Boron-8 neutrinos and ne utrinos from a potential galactic supernova. A significant number of solar pp and Beryllium-7 neutrinos are also expected to produce electronic reco ils. In this talk\, I will give an overview of the impressive capability o f the XENONnT detector to observe rare neutrino phenomena.\n\nhttps://indi co.ific.uv.es/event/6178/contributions/15706/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15706/ END:VEVENT BEGIN:VEVENT SUMMARY:A deuterated liquid scintillator for supernova neutrino detection DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15627@indico.ific.uv.es DESCRIPTION:Speakers: Bhavesh Chauhan (Tata Institute of Fundamental Resea rch\, India)\nFor the next galactic supernova\, operational neutrino teles copes will measure the neutrino flux several hours before their optical co unterparts. Existing detectors\, relying mostly on charged current interac tions\, are mostly sensitive to $\\bar{\\nu}_e$ and to a lesser extent to $\\nu_e$. In order to measure the flux of other flavors ($\\nu_{\\mu}\,\\b ar{\\nu}_{\\mu}\,\\nu_{\\tau}\,\\text{and}~\\bar{\\nu}_{\\tau}$)\, we need to observe their neutral current interactions with the detector. Such a m easurement is not only crucial for overall normalization of the supernova neutrino flux but also for understanding the intricate neutrino oscillatio n physics. A deuterium based detector will be sensitive to all neutrino fl avors. In this talk\, I will present our proposal for a 1\\\,kton deuterat ed liquid scintillator (DLS) based detector that will see about 435 neutra l current events and 170 (108) charged current $\\nu_e$ ($\\bar{\\nu}_e$) events from a fiducial supernova at a distance of 10 kpc from Earth. We e xplore the possibility of extracting spectral information from the neutral current channel $\\overset{\\scriptscriptstyle(-)}{\\nu} d \\rightarrow \\overset{\\scriptscriptstyle(-)}{\\nu}np$ by measuring the quenched kinet ic energy of the proton in the final state\, where the neutron in the fina l state is tagged and used to reduce backgrounds.\n\nhttps://indico.ific.u v.es/event/6178/contributions/15627/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15627/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of Super-Kamiokande Gadolinium project DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15608@indico.ific.uv.es DESCRIPTION:Speakers: Motoyasu Ikeda (Kamioka Obs. ICRR. U of Tokyo)\nSupe r-Kamiokande (SK) is the world's largest underground water Cherenkov\ndete ctor. The latest phase of operations began in July 2020 when\, in order\nt o improve neutron detection efficiency\, about 13 tons of gadolinium (Gd)\ nsulfate octahydrate was dissolved into SK's pure water. Gd has a large\n thermal neutron capture cross section and emits visible gamma rays. This\n first loading marked the start of what is now called SK-Gd\, and stable\np hysics data taking has been ongoing since then.\nThis presentation will fo cus on details of the first Gd loading and the\ndetector status including detector calibrations. Also\, the future plan and\nthe prospect of observa tions with SK-Gd will be discussed.\n\nhttps://indico.ific.uv.es/event/617 8/contributions/15608/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15608/ END:VEVENT BEGIN:VEVENT SUMMARY:The Hyper-Kamiokande Experiment DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15572@indico.ific.uv.es DESCRIPTION:Speakers: Jeanne Wilson (King's College London)\nThe Hyper-Kam iokande experiment consists of a 260 kt underground water Cherenkov detect or with a fiducial volume more than 8 times larger than that of Super-Kami okande. It will serve both as a far detector of a long-baseline neutrino e xperiment and an observatory for astrophysical neutrinos and rare decays.\ nThe long-baseline neutrino experiment will detect neutrinos originating f rom the upgraded 1.3 MW neutrino beam produced at the J-PARC accelerator 2 95 km away. A near detector suite\, close to the accelerator\, will help c haracterise the beam and minimise systematic errors. The experiment is now under construction and due to start data taking in 2027.\nThe experiment will investigate neutrino oscillation phenomena (including CP-violation an d mass ordering) by studying accelerator\, solar and atmospheric neutrino s\, neutrino astronomy (solar\, supernova\, supernova relic neutrinos) and nucleon decays.\nIn this talk\, we will present an overview of the Hyper- Kamiokande experiment\, its physics goals and the current status.\n\nhttps ://indico.ific.uv.es/event/6178/contributions/15572/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15572/ END:VEVENT BEGIN:VEVENT SUMMARY:DUNE Physics Program and Status DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15571@indico.ific.uv.es DESCRIPTION:Speakers: Carmen Palomares (CIEMAT)\nThe Deep Underground Neut rino Experiment (DUNE) is a next-generation long-baseline neutrino experim ent with a 70-kt liquid argon detector at the Sanford Underground Research Facility (SURF) 1300 km from Fermilab. This programme includes studies of neutrino oscillations with a high-intensity muon-neutrino beam from Fermi lab\; as well as\, proton decay and supernova neutrino burst searches. DUN E will resolve the neutrino mass hierarchy to a precision of 5σ\, for all δCP values\, after 2 years of running with the nominal detector design a nd beam configuration. It has the potential to observe charge-parity viola tion in the neutrino sector to a precision of 3σ (5σ) after an exposure of 5 (10) years\, for 50% of all δCP values. The status and schedule of t he project will be also presented.\n\nhttps://indico.ific.uv.es/event/6178 /contributions/15571/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15571/ END:VEVENT BEGIN:VEVENT SUMMARY:RES-NOVA: archaeological Pb-based observatory for Supernova neutri no detection DTSTART;VALUE=DATE-TIME:20210901T154000Z DTEND;VALUE=DATE-TIME:20210901T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15565@indico.ific.uv.es DESCRIPTION:Speakers: Luca Pattavina (INFN-LNGS & TUM)\nRES-NOVA is a new proposed experiment for the hunt of neutrinos from core-collapse supernova e (SN) via coherent elastic neutrino-nucleus scattering (CEvNS) using an a rray of archaeological lead (Pb) based cryogenic detectors. The high CEvNS cross-section on Pb and the ultra-high radiopurity of archaeological Pb e nable the operation of a high statistics experiment equally sensitive to a ll neutrino flavors. Thanks to these unique features\, RES-NOVA will be as sensitive as super-size SN neutrino observatories\, while running a detec tor with a total active volume of only (60 cm)^3. RES-NOVA will be able to reconstruct the SN neutrino parameters with great accuracy (at the 10% le vel) and it will be sensitive to SN emissions from the entire Milky Way Ga laxy with 5 sigma statistical significance. During this conference\, the e xpected detector performance and sensitivity will be presented\, as well a s the first preliminary results of a prototype detector.\n\nhttps://indico .ific.uv.es/event/6178/contributions/15565/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15565/ END:VEVENT BEGIN:VEVENT SUMMARY:The Intermediate Water Cherenkov Detector for the Hyper-Kamiokande Experiment DTSTART;VALUE=DATE-TIME:20210901T152500Z DTEND;VALUE=DATE-TIME:20210901T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15555@indico.ific.uv.es DESCRIPTION:Speakers: Patrick de Perio (TRIUMF)\nHyper-Kamiokande (Hyper-K ) is a next-generation experiment for understanding the properties of neut rino mixing\, astrophysical neutrinos\, and searches for new physics throu gh processes such as nucleon decay. It will utilize a water Cherenkov dete ctor 8 times larger than the current Super-Kamiokande\, and will benefit f rom an upgraded 2.5 times higher intensity J-PARC beam than T2K. An Interm ediate Water Cherenkov Detector (IWCD) will help mitigate systematic uncer tainties to a level commensurate with this unprecedented statistical preci sion\, affording significant discovery potential of leptonic CP violation. This one kilotonne scale detector will be located around 1 km from the J- PARC neutrino source. The capability to move vertically for scanning off-a xis angles will improve the understanding of neutrino interactions and the ir energy dependence. Gadolinium loading will allow high efficiency measur ements of neutrons that accompany neutrino interactions\, providing furthe r knowledge towards Hyper-K physics analyses. A prototype water Cherenkov beam test experiment (WCTE) is planned at CERN to evaluate key technologie s\, including a new photosensor\, calibration systems\, and deep learning event reconstruction. This talk will summarize the WCTE and IWCD designs a nd physics programs.\n\nhttps://indico.ific.uv.es/event/6178/contributions /15555/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15555/ END:VEVENT BEGIN:VEVENT SUMMARY:JUNO Detector Design & Status DTSTART;VALUE=DATE-TIME:20210901T151000Z DTEND;VALUE=DATE-TIME:20210901T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15541@indico.ific.uv.es DESCRIPTION:Speakers: Zhimin Wang (IHEP\,CAS)\nThe Jiangmen Underground Ne utrino Observatory (JUNO) is a next-generation liquid-scintillator reactor neutrino experiment under construction in Southern China. It is a multi-p urpose experiment with a wide range of applications in neutrino physics\, ranging from a mass-ordering (MO) determination to solar\, geo-\, and atmo spheric neutrinos\, detecting of Supernova neutrinos\, and precision measu rement on oscillation parameters. The JUNO central detector (CD) designs t o an energy resolution of 3% at 1 MeV. The detector system will install in an over 50-meter-wide experimental hall\, which recently excavates under 700 m of granite overburden. The CD contains a 35.4-meter diameter acrylic vessel filled with 20-kt of LAB-based liquid scintillator\, making it the largest liquid-scintillator detector in the world. The scintillation ligh t will be read-out by 17612 20" PMTs and 25600 3" PMTs\, reaching a high p hotocathode coverage higher than 75%. The CD surrounds a water pool filled with ultrapure water equipped with 2400 PMTs\; on top of the CD\, a track er completes the JUNO veto system for cosmic muons detection. \nJUNO const ruction will complete in 2022. This talk presents the detector design and status of the experiment.\n\nhttps://indico.ific.uv.es/event/6178/contribu tions/15541/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15541/ END:VEVENT BEGIN:VEVENT SUMMARY:Testing Quantum Mechanics in the cosmic silence DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15991@indico.ific.uv.es DESCRIPTION:Speakers: Kristian Piscicchia (CREF\, LNF (INFN))\nThe VIP exp eriment aims to perform high sensitivity tests of the Pauli Exclusion Prin ciple (PEP) for electrons\, and look for a possible small violation.\nIn L ocal Quantum Field Theories approach any PEP violating transition is stron gly constrained by the Messiah Greenberg Superselection (MGS) rule\, which forbids superpositions of states with different symmetry. Such models can then be only tested with open systems. This condition is realised in VIP- 2 by introducing “new” electrons in a pre-existing system of electrons \, and then testing the resulting symmetry state. The data analyses result s from the newest VIP-2 Open Systems data taking will be presented.\nIt wa s recently shown that a large class of Quantum Gravity models embeds the v iolation of PEP\, violating the MSG rule\, as a consequence of the space-t ime non-commutativity. High sensitivity tests of PEP violation in closed s ystems turn then to be the better candidates to put strong experimental li mits on the energy scale of the non-commutativity emergence in Quantum Gra vity. The results of exploratory studies based a High Purity Germanium (HP Ge) Detecors and high radio-purity Roman Pb targets will be shown.\n\nThe extremely low background environment of LNGS is also suitable for investig ating one of the main mysteries of Quantum Mechanics Foundations: the meas urement problem. Dynamical collapse models consist in non-linear and stoch astic modifications to the Shroedinger dynamics\, which induce the collaps e with a rate proportional to the mass. The results of our analyses\, sett ing the strongest constrains on the dynamical collapse models\, will be pr esented.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15991/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15991/ END:VEVENT BEGIN:VEVENT SUMMARY:Jánossy Underground Research Laboratory DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15980@indico.ific.uv.es DESCRIPTION:Speakers: Edit Fenyvesi (Wigner Research Centre for Physics)\n https://indico.ific.uv.es/event/6178/contributions/15980/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15980/ END:VEVENT BEGIN:VEVENT SUMMARY:Studies of bulk 210Po/210Pb contamination in high purity copper fo r low-background detectors DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15941@indico.ific.uv.es DESCRIPTION:Speakers: Tomasz Mróz (Marian Smoluchowski Institute of Physi cs\, Jagiellonian Universit)\nSurface and bulk contamination with long-liv ed daughters of $^{222}$Rn is of great interest for most of the experiment s looking for rare events. These include detection of low energy solar neu trinos\, searches for neutrino-less double beta decay or searches for dark matter. Decays of $^{210}$Pb\, $^{210}$Bi and finally $^{210}$Po may cont ribute significantly to the experiments’ background directly by the gene rated radiation\, or indirectly through e.g. production of neutrons in the (α\,n) reactions. The latter is of special interest for the dark matter experiments as the interactions of neutrons are indistinguishable from the interactions of dark matter particles.\n\nDirect detection of the long-li ved part of the $^{238}$U chain is necessary because of possible disequili brium in the chain. One cannot conclude about the $^{210}$Pb-$^{210}$Po sp ecific activities form the $^{226}$Ra or $^{238}$U activities measured wit h high-sensitivity gamma-ray spectrometers or ICP-MS instruments\, respect ively.\n\nA method to measure $^{210}$Po in copper will be discussed. Copp er\, because of its high radio-purity\, is widely applied in low-backgroun d experiments as a shielding material and it is also often used to fabrica te support structures of sensitive detectors. By separation of $^{210}$Po from the bulk material and subsequent counting of its activity it is possi ble to achieve the detection limit at the level of 10 mBq/kg. For a select ed copper sample (material purchased for shielding of low-background gamma spectrometer) a relation between $^{226}$Ra (determined by application of high-sensitivity gamma spectrometry)\, $^{210}$Po and $^{210}$Pb (specifi c activity established form the $^{210}$Po decay profile) indicating a str ong radioactive disequilibrium\, will be discussed.\n\nhttps://indico.ific .uv.es/event/6178/contributions/15941/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15941/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent development of the radiopurity.org materials database DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15934@indico.ific.uv.es DESCRIPTION:Speakers: Christopher Jackson (Pacific Northwest National Labo ratory)\nThe radiopurity.org database has proven to be a valuable resource for the low background physics community as a tool to track and share ass ay results. This talk will describe recent collaborative efforts between t he Pacific Northwest National Laboratory and SNOLAB to modernize the datab ase for the community. Improvements to the search utility and data upload methods will be discussed. Installations to support individual physics col laborations (for example DUNE) and assay facilities will be described\, as well as ongoing plans to develop and support the database.\n\nhttps://ind ico.ific.uv.es/event/6178/contributions/15934/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15934/ END:VEVENT BEGIN:VEVENT SUMMARY:Radioactive Background Characterization of the Cryogenic Undergrou nd TEst Facility (CUTE) DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15932@indico.ific.uv.es DESCRIPTION:Speakers: Silvia Scorza (SNOLAB)\nThe Cryogenic Underground TE st Facility (CUTE) is fully operational in the low-radioactivity environme nt of the SNOLAB Underground Laboratory. Estimation of the background from radioactive processes via Geant4 simulation is crucial in informing the b ackground budget for the facility. The radioactive background characteriza tion of the CUTE facility will be presented along with the background mode l validation through comparison with recently acquired data.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15932/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15932/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurements and Simulation of background radiation for rare event search experiments at an underground laboratory DTSTART;VALUE=DATE-TIME:20210902T154000Z DTEND;VALUE=DATE-TIME:20210902T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15931@indico.ific.uv.es DESCRIPTION:Speakers: Sayan Ghosh (Saha Institute of Nuclear Physics)\nRar e event search experiments mostly placed inside underground laboratories d emand very accurate measurements of ambient radiation contribution from ch arged cosmic particles from radioactive decay and nuclear processes in the surrounding rock components. Therefore careful analysis of rock component s and specific background measurement experiments along with simulation st udies form the first foundation of these types of experiments. To begin wi th\, an underground laboratory for rare event search experiments is set up at 555 m vertical depth inside a mine in India. Gamma rays and neutrons f rom the environmental rocks\, penetrating cosmic muons and secondary parti cles are the major causes of concern. In this work\, we have experimentall y measured the fluxes of cosmic muons\, ambient gamma rays and the environ mental neutrons inside the laboratory. We have also performed detailed sim ulations using the tracking toolkit of GEANT4 and environmental data to es timate the measured fluxes and related numbers. Very good agreements with the measured fluxes in almost all the cases are found. Based on our studie s\, we find that while comparing the experimental and the GEANT4 results\, it is important to include multiple scattering events to obtain reliable results. Experimental results\, simulation strategies followed and the res ults obtained will be presented.\n\nhttps://indico.ific.uv.es/event/6178/c ontributions/15931/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15931/ END:VEVENT BEGIN:VEVENT SUMMARY:A Radioacitivity Survey of Commercially Available PTFE from Europe an Suppliers DTSTART;VALUE=DATE-TIME:20210902T152500Z DTEND;VALUE=DATE-TIME:20210902T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15926@indico.ific.uv.es DESCRIPTION:Speakers: Daniel Baur (University of Freiburg)\nDue to its opt ical and electrical properties polytetrafluoroethylene (PTFE) is an import ant construction material for many rare event searches. The radioactive co ntamination of PTFE thus needs to be as low as possible. We present a cros s-sectional study investigating the radioactive contamination of PTFE samp les from major European suppliers of raw PTFE. The bulk contaminations of the samples were measured utilizing ICP-MS and HPGe gamma spectrometry\; t he radon surface emanation was assessed with an electrostatic radon detect or that was recently commissioned in Freiburg.\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15926/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15926/ END:VEVENT BEGIN:VEVENT SUMMARY:The LUNA project at Gran Sasso : new results about the early Uni verse and future perspectives DTSTART;VALUE=DATE-TIME:20210902T151000Z DTEND;VALUE=DATE-TIME:20210902T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15925@indico.ific.uv.es DESCRIPTION:Speakers: Sandra Zavatarelli (INFN - Genova)\nIn the cosmic si lence of the Gran Sasso Underground Laboratory\, where 1400 m of rock shie ld the experimental halls from external radiation\, the LUNA experiment is able to recreate the processes that occurred during Big Bang Nucleosynthe sis (BBN) and the ones that still occur in stars today. Among the reactio ns recently studied at LUNA there is a key process of BBN: the reaction b y which a proton and a nucleus of deuterium fuse together to form $^{3}$He \, in symbols: D($p\,\\gamma$)$^{3}$He. The measurement of this cross sect ion was carried out with a precision of 3% at the energies of interest for the BBN and allowed for a deeper knowledge of the deuterium destruction p rocess and a better evaluation of its primordial abundance. Thanks to thi s study\, it was possible to refine the calculations of the primordial nuc leosynthesis and to obtain an accurate determination of the density of ord inary (or “baryonic”) matter\, thus providing support to the standard cosmological model.\nPresently the LUNA collaboration is continuing its sc ientific activity at the 400 KV accelerator but\, in the next years\, a ne w window will be opened by the acquisition with the new LUNA-MV facility\, under installation at LNGS. The new accelerator will be able to provide h ydrogen\, helium and carbon high current beams up to an accelerating volta ge of 3.5 MV and it will allow to explore the helium and carbon burning pr ocesses\, by studying the key reactions shaping the evolution of massive s tars such as $^{12}$C+$^{12}$C\, $^{13}$C($\\alpha\,n$)$^{16}$O and $^{22} $Ne($\\alpha\,n$)$^{25}$Mg.\nThe present contribution is aimed to summaris e the most recent results achieved by LUNA Collaboration\, in particular a bout the D($p\,\\gamma$)$^{3}$He process\, and to highlight the rich exper imental program connected to the new facility.\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15925/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15925/ END:VEVENT BEGIN:VEVENT SUMMARY:A lab-scale experiment for keV sterile neutrino search from tritiu m beta decay spectrum DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15709@indico.ific.uv.es DESCRIPTION:Speakers: YongChang Lee (IBS\, SNU)\nWe developed a simple sma ll-scale detection method for beta decay\nspectrum of 3H. This research is motivated to investigate the presence\nof sterile neutrinos in keV region . In our experiment\, tritium nuclei\nare embedded in a 1x1x1 cm^3 LiF cry stal from 6Li(n\,3H)4He reaction.\nThe beta energy spectrum is measured wi th an MMC sensor\, one of the\nhigh-resolution microcalorimeters operating at mK temperatures. We\npresent the method for the sample preparation and the experiment\ntogether with the physics result from the first measureme nt set.\nMoreover\, an expected sensitivity to search for the heavy neutri no is\ndiscussed for one year measurement with the setup.\n\nhttps://indic o.ific.uv.es/event/6178/contributions/15709/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15709/ END:VEVENT BEGIN:VEVENT SUMMARY:Separation of the U-235 and Pu-239 Prompt Energy Spectra in NEOS-I I DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15704@indico.ific.uv.es DESCRIPTION:Speakers: Jinyu Kim (Institute for Basic Science\, Sejong Univ ersity)\nThe NEOS aims to search for sterile neutrinos by detecting reacto r antineutrinos at a very short baseline in Korea. The NEOS detector (1 to n GdLS) is deployed at the tendon gallery of the Hanbit reactor unit 5 (2. 8 GW thermal power)\, 24 m away from the reactor core. In NEOS-I\, the pro mpt energy spectrum from inverse-beta-decay was measured using 180 days of reactor-on data\, where the "5 MeV excess" was clearly observed. To under stand the origin of the "5 MeV excess"\, NEOS-II has taken 500 (60) days o f reactor-on(-off) data from September 2018 to October 2020\, covering a w hole burnup cycle of the reactor. In this talk\, we present a preliminary result on the extraction of the U-235 and Pu-239 prompt energy spectra for the whole burnup cycle\, which may shed light on the origin of the "5MeV excess".\n\nhttps://indico.ific.uv.es/event/6178/contributions/15704/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15704/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for non-unitary neutrino oscillations in the present T2K and NO$\\nu$A data DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15695@indico.ific.uv.es DESCRIPTION:Speakers: Ushak Rahaman (University of Johannesburg)\nThe mixi ng of three active neutrino flavors is parameterized by the unitary PMNS m atrix. If there are more than three neutrino flavors and if the extra gene rations are heavy iso-singlets\, the effective $3\\times 3$ mixing matrix for the three active neutrinos will be non-unitary. We have analyzed the l atest T2K and NO$\\nu$A data with the hypothesis of non-unitary mixing of the active neutrinos. We found that the 2019 NO$\\nu$A data slightly (at $ \\sim 1\\\, \\sigma$ C.L.) prefer the non-unitary mixing over unitary mixi ng. In fact\, allowing the non-unitary mixing brings the NO$\\nu$A best-fi t point in the $\\sin^2\\theta_{23}-\\delta_{\\rm CP}$ plane closer to the T2K best-fit point. The 2019 T2K data\, on the other hand\, cannot rule o ut any of the two mixing schemes. A combined analysis of the NO$\\nu$A and T2K 2019 data prefers the non-unitary mixing at $1\\\, \\sigma$ C.L.. We derive constraints on the non-unitary mixing parameters using the best-fit to the combined NO$\\nu$A and T2K data. These constraints are weaker than previously found. The latest 2020 data from both the experiments prefer n on-unitarity over unitary mixing at $1\\\, \\sigma$ C.L. The combined anal ysis prefers non-unitarity at $2\\\, \\sigma$ C.L. The stronger tension\, which exists between the latest 2020 data of the two experiments\, also ge ts reduced with non-unitary analysis.\n\nhttps://indico.ific.uv.es/event/6 178/contributions/15695/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15695/ END:VEVENT BEGIN:VEVENT SUMMARY:PROSPECT's Latest Results DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15596@indico.ific.uv.es DESCRIPTION:Speakers: Manoa Andriamirado (Illinois Institute of Technology )\nThe Precision Reactor Oscillation and SPECTrum experiment\, PROSPECT\, is a reactor antineutrino experiment located at the High Flux Isotope Reac tor (HFIR). The detector is deployed on surface with minimal overburden at very short baseline from the highly enriched uranium reactor core. With t his configuration\, PROSPECT detector can be used to explore different var iety of physics topics\, from reactor to BSM physics.\n\nThis talk will su mmarize PROSPECT’s latest results\, including recent sterile neutrino os cillation analyses\, measurement of the $^{235}$U antineutrino spectrum\, and a dedicated search for boosted sub-GeV dark matter. It will also discu ss future plans to perform improved physics measurements with a second-gen eration detector\, called PROSPECT-II.\n\nhttps://indico.ific.uv.es/event/ 6178/contributions/15596/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15596/ END:VEVENT BEGIN:VEVENT SUMMARY:The STEREO search for a sterile neutrino at the ILL reactor with f ull data sample DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15595@indico.ific.uv.es DESCRIPTION:Speakers: Loïc-René Labit (Univ Grenoble Alpes\, Univ Savoie Mont Blanc)\nLoïc-René LABIT\, on behalf of the STEREO collaboration\nD uring the last decades\, several parameters describing the neutrino oscill ation phenomenon have been characterized thanks to reactor neutrino experi ments\, in particular the precise measurement of the last-to-be-measured m ixing angle $\\theta_{13}$.\nFollowing a reactor antineutrino flux re-esti mation in 2011\, a ∼6% deficit between observed and predicted reactor an tineutrino fluxes\, known as the Reactor Antineutrino Anomaly\, has been o bserved.\nThe Reactor Antineutrino Anomaly could be explained by an oscill ation toward an additional non-interacting\, (thus “sterile”) neutrino . The parameters that best explain the RAA are a mixing angle value of $\\ sin^{2}(2\\theta)$ =0.17 and a mass splitting value of $\\Delta m^{2}_{41} $ =2.3 $\\textrm{eV}^{2}$.\nAdditionally\, a discrepancy between the measu red and predicted antineutrino energy spectrum taking the form of an exces s of events around 5 MeV has been observed by several reactor neutrino exp eriments. This discrepancy has yet to be fully understood but could be cau sed by incorrect predictions of the neutrino spectra.\nThe STEREO experime nt\, located at Institut Laue-Langevin in Grenoble (France)\, was designed to test the above mentioned oscillation hypothesis independently of shape and rate predictions. The segmented detector\, located at ~10 m of a comp act reactor core\, allows for a measurement of the antineutrino energy spe ctrum at various baselines\, sensitive to the oscillation toward a sterile neutrino that would distort the spectrum differently at each baseline.\nT he experiment could also help to disentangle isotopic contributions to the neutrino energy spectrum by providing a measurement of the spectrum shape and rate originating from a core with highly enriched (93%)235U.\nThe exp eriment took data between November 2016 and November 2020. This talk will present the latest limits set in the oscillation parameter space with the full data sample\, amounting to 334 (544) days of reactor-on (off)\, as we ll as the updated rate and spectrum shape measurements.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15595/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15595/ END:VEVENT BEGIN:VEVENT SUMMARY:Antineutrino spectrometer DANSS - 5 years of running DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15579@indico.ific.uv.es DESCRIPTION:Speakers: Igor Alekseev (ITEP)\nSolid scintillator reactor ant ineutrino detector DANSS is placed on a\nmovable platform below 3.1 GW ind ustrial reactor of the Kalininskaya Nuclear\nPower Plant. The distance bet ween the detector and the center of\nthe reactor core is frequently change d in the range 10.9 - 12.9 m. The\nreactor materials provide overburden of about 50 m.w.e.\nThe one-cubic-meter sensitive volume of the detector is assembled\nfrom 2500 polystyrene scintillation strips and surrounded\nby a multilayer passive and active shielding. A dual readout\nby silicon photo multipliers (individually) and by convention PMTs\n(in groups of 50 strip s) is used to achieve both high detector\ngranularity and low noise trigge r.\n\nIn the position closest to the reactor core up to 5000 inverse\nbeta -decay events per day are collected with cosmic muons induced\nbackground below 2%. The talk covers 5 years of the detector operation\,\nresults of our search for light sterile neutrinos as well as plans for\nthe detector upgrade.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15579/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15579/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of the Short-Baseline Near Detector at Fermilab DTSTART;VALUE=DATE-TIME:20210831T152500Z DTEND;VALUE=DATE-TIME:20210831T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15568@indico.ific.uv.es DESCRIPTION:Speakers: José I. Crespo-Anadón (CIEMAT)\nThe Short-Baseline Near Detector (SBND) will be one of three liquid Argon Time Projection Ch amber (LArTPC) neutrino detectors positioned along the axis of the Booster Neutrino Beam (BNB) at Fermilab\, as part of the Short-Baseline Neutrino (SBN) Program. The detector is currently in the construction phase and is anticipated to begin operation in the second half of 2022.  SBND is char acterised by superb imaging capabilities and will record over a million ne utrino interactions per year. Thanks to its unique combination of measurem ent resolution and statistics\, SBND will carry out a rich program of neut rino interaction measurements and novel searches for physics beyond the St andard Model (BSM). It will enable the potential of the overall SBN steril e neutrino program by performing a precise characterisation of the unoscil lated event rate\, and by constraining BNB flux and neutrino-Argon cross-s ection systematic uncertainties. In this talk\, the physics reach\, curren t status\, and future prospects of SBND are discussed.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15568/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15568/ END:VEVENT BEGIN:VEVENT SUMMARY:Reactor antineutrino anomaly in light of recent flux model refinem ents DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15567@indico.ific.uv.es DESCRIPTION:Speakers: Zhao Xin ()\nWe study the status of the reactor anti neutrino anomaly in light of new reactor flux models from both conversion and summation methods. We find that both the reactor rate and fuel evoluti on data are consistent with the predictions both from the conversion model of Kopeikin et al. and the summation model of Estienne et al. The converg ence of both model predictions indicates the rebustness for the solution t o the reactor anomaly in terms of flux model refinements.\n\nhttps://indic o.ific.uv.es/event/6178/contributions/15567/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15567/ END:VEVENT BEGIN:VEVENT SUMMARY:Seach for supernova relic neutrinos at KamLAND DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15725@indico.ific.uv.es DESCRIPTION:Speakers: Shuhei Obara (Tohoku University)\nWe report a search for electron antineutrinos at KamLAND with an energy range of 8.3--30.8 M eV via the inverse beta decay.\nIn 4528 days of KamLAND data\, we found 18 event candidates and no significant excess over estimated backgrounds.\nF rom data interpretation\, with the assumption of some supernova relic neut rino spectrum predictions\, we give upper flux limits of $60$--$110\\\,{\\ mathrm{cm}^{-2}\\mathrm{s}^{-1}}$ ($90\\%$ CL) in the analysis range and p resent a model-independent flux.\nThese upper limits are the most stringen t for 8.3--12 MeV region to date.\nWe also improve on the upper probabilit y limit of $^8$B solar neutrinos converting into antineutrinos via the Res onant Spin Flavor Precession with the neutrino magnetic moment.\nBesides\, we could set limits on the annihilation cross section for light dark matt er pairs to neutrino pairs.\n\nhttps://indico.ific.uv.es/event/6178/contri butions/15725/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15725/ END:VEVENT BEGIN:VEVENT SUMMARY:KM3NeT: Status and perspectives for neutrino astronomy from the Me V to the PeV DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15628@indico.ific.uv.es DESCRIPTION:Speakers: Silvia Celli (Sapienza Università di Roma)\nKM3NeT is a multi-purpose neutrino observatory currently being deployed at the bo ttom of the Mediterranean Sea. It consists of two detectors: ORCA and ARCA (for Oscillation and Astroparticle Research with Cosmics in the Abyss). A RCA will instrument 1 Gton of seawater\, with the primary goal of detectin g cosmic neutrinos with energies between several tens of GeV and PeV. Due to its position in the Northern Hemisphere\, ARCA will provide an optimal view of the Southern sky including the Galactic Center. This month\, a maj or step has be taken in the construction of ARCA\, bringing the total numb er of detection lines from one to six. ORCA\, also currently running in a 6-line configuration\, is a smaller (~ few Mtons) and denser array\, optim ized for the detection of atmospheric neutrinos in the 1 - 100 GeV. It can also study low-energy neutrino astronomy\, such as MeV-scale core-collaps e supernova.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15628/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15628/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for neutrino counterparts of LIGO/Virgo gravitational-wave events DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15623@indico.ific.uv.es DESCRIPTION:Speakers: Islam Unatlokov (BNO INR RAS)\nThe LIGO/Virgo collab orations have reported the results of their searches for gravitational-wav es from the first half of their third observing run. 39 events were added to the first Gravitational-Wave Transient Catalog (GWTC-1)\, reaching the total number of 50. Thus\, an additional search for counterparts is necess ary. The data from Baksan Underground Scintillation Telescope (BUST) are u sed to search for neutrino counterparts. The BUST detections of muons from the lower hemisphere in the zenith angles >100° are used. The angular un certainty of muon neutrinos and antineutrinos from the lower hemisphere is ~5°. The energy threshold is 1 GeV. If no counterparts found the integra l fluxes of muon neutrinos and antineutrinos are calculated. This work pre sents the description of data processing and the limits on integral fluxes from the gravitational-wave localization regions.\n\nhttps://indico.ific. uv.es/event/6178/contributions/15623/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15623/ END:VEVENT BEGIN:VEVENT SUMMARY:JUNO Non-oscillation Physics DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15618@indico.ific.uv.es DESCRIPTION:Speakers: Giulio Settanta (Forschungszentrum Jülich GmbH\, Nu clear Physics Institute IKP-2\, Jülich\, Germany)\nThe JUNO observatory\, a 20 kt liquid scintillator detector to be completed in 2022 in China\, b elongs to the next-generation of neutrino detectors\, which share the comm on features of having a multi-ton scale and an energy resolution at unprec edented levels. \nBeside the ambitious goal of neutrino mass ordering dete rmination\, the JUNO Collaboration plans also to perform a wide series of other measurements in the neutrino and astroparticle fields\, rare process es and searches for new physics. The detector characteristics will allow t he detection of neutrinos from many sources\, like supernovae\, the Sun\, atmospheric and geoneutrinos. Other potential studies accessible to JUNO i nclude the search for exotic processes\, such as nucleon decays\, Dark Mat ter and magnetic monopoles interactions\, light sterile neutrinos producti on.\nThis talk will review the potential of JUNO about non-oscillation phy sics\, highlighting the unique contributions that the experiment will give to the various fields in the forthcoming years.\n\nhttps://indico.ific.uv .es/event/6178/contributions/15618/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15618/ END:VEVENT BEGIN:VEVENT SUMMARY:SNEWS2.0: The Multi-Messenger Supernova Early Warning System DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15617@indico.ific.uv.es DESCRIPTION:Speakers: Marta Colomer Molla (APC/IFIC)\nCore collapse supern ovae (CCSN) are among the most precious multi-messenger events of the extr eme Universe. These events are extremely rare\, and it will be crucial to gather all the physics possible from the data of the next event. The SNEWS public alert system was designed to provide an early alert to astronomers and other observers about the observation of neutrinos from a Galactic CC SN\, which are produced minutes to hours before the electromagnetic radiat ion. SNEWS has been operating for more than two decades\, searching for a coincident signal between neutrino experiments from all around the world. In the current era of multi-messenger astrophysics\, there are new opportu nities for SNEWS to optimize the science reach from the next Galactic supe rnova beyond the simple early alert. In this talk\, the upgrades and new c apabilities of SNEWS2.0 will be discussed.\n\nhttps://indico.ific.uv.es/ev ent/6178/contributions/15617/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15617/ END:VEVENT BEGIN:VEVENT SUMMARY:Astroparticle physics in DUNE with the X-Arapuca detectors DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15566@indico.ific.uv.es DESCRIPTION:Speakers: Claudia Brizzolari ()\nDUNE is a long-baseline accel erator experiment currently in construction at Fermilab and SURF (South Da kota). \nThe science objectives of DUNE include a comprehensive investigat ion of long-baseline neutrino oscillations and\, in particular\, the study of CP violation in the neutrino sector and the identification of the neut rino mass hierarchy\, along with high-sensitivity rare event searches like the observation of supernova neutrino bursts and the search for proton de cay.\nThe Far Detector consists of four Liquid Argon TPCs located deep und erground\,\nwhich represents a unique observatory for astroparticle physic s. The DUNE physics reach in such a field is remarkably enhanced by the DU NE Photon Detection System (PDS) that is based on a novel light trapping t echnology (X-Arapuca).\nIn this talk\, we will present the latest results obtained by the PDS Consortium in terms of light efficiency and cryo-relia bility of the X-Arapuca\, together with the most important technological a chievements to cover the large surface of the DUNE anodes. We will also di scuss the role of the PDS for the study of supernova neutrino bursts and t he search for proton decay. Finally\, we will present the latest developme nt of this technique\, based on a new class of photon downshifting polymer ic material and the impact on the physics reach of DUNE.\n\nhttps://indico .ific.uv.es/event/6178/contributions/15566/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15566/ END:VEVENT BEGIN:VEVENT SUMMARY:Modeling neutrino emission for different gamma-ray burst productio n scenarios DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15534@indico.ific.uv.es DESCRIPTION:Speakers: Tetyana Pitik (Niels Bohr International Academy)\nGa mma ray-bursts (GRBs) are among the least understood and most powerful tra nsients occurring in our Universe. Different dissipation and emission proc esses have been proposed over the years to interpret their origin. However \, we still lack an exhaustive theoretical explanation due to the failure of existing models in addressing all observations in the spectral and temp oral domains. GRBs are also candidate sources of high energy neutrinos det ected by IceCube Neutrino Observatory. I will discuss the neutrino emissio n in different dissipation scenarios\, and show that the neutrino predicti on strongly depends on the adopted jet model\, highlighting the importance of neutrinos in pinpointing the GRB emission mechanism in the case of suc cessful neutrino detection.\nBased on Pitik\, Tamborra\, and Petropoulu\, arXiv:2102.02223\n\nhttps://indico.ific.uv.es/event/6178/contributions/155 34/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15534/ END:VEVENT BEGIN:VEVENT SUMMARY:Fast Flavor Ocillations of Supernova neutrinos in three flavors DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15528@indico.ific.uv.es DESCRIPTION:Speakers: Madhurima Chakraborty (IIT Guwahati)\nNeutrinos emit ted from a core-collapse supernova (SN) may undergo fast flavor\nconversio ns almost immediately above the core\, resulting in drastic\nconsequences for the supernova explosion mechanism and nucleosynthesis.\nThese fast fla vor oscillation dynamics are independent of the neutrino mass\,\ngrowing a t the scale of the large neutrino-neutrino interaction strength (10^5 km^ −1\n) of the dense core which is extremely fast\, in comparison to the u sual ‘slow’\ncollective modes driven by much smaller vacuum oscillatio n frequencies (10^0\nkm^−1 ). The necessary condition for the existence of these fast instabilities is the\npresence of a zero-crossing in the ang ular distribution of the neutrino lepton\nnumber. The previous literature on fast conversions have focussed on an\neffective two-flavor analysis\, w here the zero crossing in electron lepton number\n(ELN) was crucial since the assumption of similar number density of the the\nheavy lepton neutrino s lead to similar angular spectra. However\, motivated\nfrom the recent su pernova simulations with muon production in the accretion\nphase\, we perf orm the first non-linear simulations of fast conversions in the\npresence of all the three neutrino flavors. Our results show the significance of\nm uon and tau lepton number angular distributions\, along with the tradition al\nelectron lepton number ones and strengthen the need to further investi gate the\noccurrence of fast conversions in supernova simulation data\, in cluding the\ndegeneracy breaking of mu and tau neutrinos.\n\nhttps://indic o.ific.uv.es/event/6178/contributions/15528/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15528/ END:VEVENT BEGIN:VEVENT SUMMARY:Visible Decay of Astrophysical Neutrinos at IceCube DTSTART;VALUE=DATE-TIME:20210830T154000Z DTEND;VALUE=DATE-TIME:20210830T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15526@indico.ific.uv.es DESCRIPTION:Speakers: Peter Denton (Brookhaven National Laboratory)\nNeutr ino decay modifies neutrino propagation in a unique way\; not only is ther e flavor changing as there is in neutrino oscillations\, there is also ene rgy transport from initial to final neutrinos. The most sensitive direct p robe of neutrino decay is currently IceCube which can measure the energy a nd flavor of neutrinos traveling over extragalactic distances. For the fir st time we calculate the flavor transition probability for the cases of vi sible and invisible neutrino decay\, including the effects of the expansio n of the universe\, and consider the implications for IceCube. As an examp le\, we demonstrate how neutrino decay addresses a tension in the IceCube data.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15526/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15526/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrinos : from the r-process to the diffuse supernova neutrino background DTSTART;VALUE=DATE-TIME:20210830T152500Z DTEND;VALUE=DATE-TIME:20210830T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15525@indico.ific.uv.es DESCRIPTION:Speakers: Maria Cristina Volpe (APC and CNRS)\nNeutrinos play an important role in astrophysical and cosmological environments. \nIn thi s talk I will discuss recent progress in neutrino flavor evolution in dens e media\, including core-collapse supernovae and binary neutron star merge rs remnants. I will remind decoherence effects in vacuum and then discuss neutrino decoherence and other effects due to strong gravitational fields\ , nearby compact objects. I will highlight the implications of these aspec ts and/or of non-standard physics on observations\, in particular in relat ion with the r-process and the GW170817 event\, and with the diffuse supe rnova neutrino background\, whose detection is expected soon.\n\nhttps://i ndico.ific.uv.es/event/6178/contributions/15525/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15525/ END:VEVENT BEGIN:VEVENT SUMMARY:Primordial Black Hole Dark Matter evaporating on the Neutrino Floo r DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15524@indico.ific.uv.es DESCRIPTION:Speakers: Roberta Calabrese (Università degli studi di Napoli "Federico II")\nPrimordial black holes hypothetically generated in the fi rst instants of life of the Universe are potential dark matter candidates. Focusing on Primordial Black Holes masses in the range $[5 \\times10^{14} - 5 \\times 10^{15}]$g\, we point out that the neutrinos emitted by Primo rdial Black Holes evaporation can interact through the coherent elastic ne utrino-nucleus scattering producing an observable signal in multi-ton Dark Matter direct detection experiments. We show that with the high exposures envisaged for the next-generation facilities\, it will be possible to set bounds on the fraction of Dark Matter composed by Primordial Black Holes improving the existing neutrino limits obtained with Super-Kamiokande. We also quantify to what extent a signal originating from a small fraction of Dark Matter in the form of Primordial Black Holes would modify the so-cal led "neutrino floor"\, the well-known barrier towards detection of weakly interacting massive particles as the dominant Dark Matter component.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15524/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15524/ END:VEVENT BEGIN:VEVENT SUMMARY:Revealing the Majorana nature of neutrinos through a precision mea surement of the CP phase DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15604@indico.ific.uv.es DESCRIPTION:Speakers: Alberto Gago Medina (Pontificia Universidad Católic a del Perú)\nWe show that it is possible to reveal the nature of neutrin o by measuring the Majorana phase at the DUNE experiment. The Majorana pha se is activated in the neutrino oscillation framework ($\\nu \\rightarrow \\nu$ and and $\\bar{\\nu}\\rightarrow \\bar{\\nu}$) due to the introduct ion of a decoherence environment. Being that depending on the value of the Majorana phase and the intensity of decoherence\, the measurement of the Dirac \\textit{CP} violation phase $\\delta_{\\mathrm{CP}}$ can be highly spoiled. We will notice the latter by comparing the measurements of the CP phases that will take place in DUNE and T2HK. Finally\, we will also ass es the possibility of the measurement of the Majorana phase at DUNE.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15604/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15604/ END:VEVENT BEGIN:VEVENT SUMMARY:Model-independent test of T violation in neutrino oscillations DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15601@indico.ific.uv.es DESCRIPTION:Speakers: Alejandro Segarra Tamarit (IFIC (CSIC-Univ Valencia) )\nWe propose a method to establish time reversal symmetry violation at fu ture neutrino oscillation experiments in a largely model-independent way. We introduce a general parametrization of flavour transition probabilities which holds under weak assumptions and covers a large class of new-physic s scenarios. This can be used to search for the presence of T-odd componen ts in the transition probabilities by comparing data at different baseline s but at the same neutrino energies. We show that this test can be perform ed already with experiments at three different baselines and might be feas ible with experiments under preparation/consideration.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15601/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15601/ END:VEVENT BEGIN:VEVENT SUMMARY:NOvA's latest three-flavor neutrino oscillations results DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15594@indico.ific.uv.es DESCRIPTION:Speakers: Ashley Back (Indiana University)\nNOvA is a leading long-baseline neutrino experiment thanks to the powerful - nearly 700 kW - NuMI beam\, which directs predominantly muon neutrinos from Fermilab\, Il linois towards Ash River\, in northern Minnesota. The experiment consists of two detectors placed 809 km apart\, both about 14 mrad off-axis from th e beam center. The detectors\, one near and one far\, were each formed fro m plastic extrusions filled with a liquid scintillator\, making them funct ionally identical\, which largely cancels key flux and cross-section syste matic uncertainties. The three-flavor long-baseline search probes undeterm ined physics such as the neutrino mass hierarchy (ordering)\, CP violation in the lepton sector\, and the octant of $\\theta_{23}$ (the large mixing angle). The analysis to extract these parameters studies neutrino interac tions in each detector to observe the disappearance of muon neutrinos and the appearance of electron neutrinos\, due to oscillations. I will present the latest results from NOvA\, based on the combined neutrino and antineu trino beam mode datasets\, collected up to March 2020\, and briefly discus s the future reach of the experiment.\n\nhttps://indico.ific.uv.es/event/6 178/contributions/15594/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15594/ END:VEVENT BEGIN:VEVENT SUMMARY:Latest Results from the Daya Bay Reactor Neutrino Experiment DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15591@indico.ific.uv.es DESCRIPTION:Speakers: Zeyuan Yu (Institute of High Energy Physics\, CAS)\n Utilizing six powerful nuclear reactors as antineutrino sources and eight identically designed underground detectors for a near-far relative measure ment\, the Daya Bay Reactor Neutrino Experiment has achieved unprecedented precision in measuring the neutrino mixing angle θ13 and the neutrino ma ss squared difference |Δm231|. With the largest sample of reactor antineu trino interactions ever collected to date\, Daya Bay has also performed ma ny measurements of reactor antineutrinos\, such as the determination of to tal reactor antineutrino flux and spectrum\, the extraction of individual antineutrino flux and spectra of the two dominant isotopes (235U and 239Pu ). On Dec. 12\, 2020\, the experiment stopped data taking. The decommissio ning is going smoothly. In this talk\, I will present the latest results f rom Daya Bay.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15591/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15591/ END:VEVENT BEGIN:VEVENT SUMMARY:T2K Status and plans DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15575@indico.ific.uv.es DESCRIPTION:Speakers: Maria Antonova (IFIC (CSIC-Univ Valencia))\nT2K is a long baseline experiment providing world-leading measurements of the para meters governing neutrino oscillation. T2K data enable the first 3 sigma e xclusion for some intervals of the CP-violating phase \\delta_{CP} and pre cision measurements of the atmospheric parameters \\Delta_m^{2}{32}\, sin^ 2(\\theta{23}).\nT2K exploits a beam of muon neutrinos and antineutrinos a t the Japan Particle Accelerator Research Centre (JPARC) and it measures o scillations by comparing neutrino rates and spectra at a near detector com plex\, located at JPARC\, and at the water-Cherenkov detector Super Kamiok ande\, located 295 Km away. The T2K beam will be upgraded with increased p ower in 2022 and an upgrade of the ND280 near detector\, located 2.5 degre es off-axis\, is being assembled to exploit the increased statistics. More over\, the Super Kamiokande detector has been loaded with 0.02% of Gadolin ium in 2020\, enabling enhanced neutron tagging. \nIn preparation for the exploitation of such data\, the T2K collaboration is working on an updated oscillation analysis to improve the control of systematic uncertainties A new beam tuning has been developed\, based on an improved NA61/SHINE meas urements on a copy of the T2K target and including a refined modelling of the beam line materials. New selections are being developed at ND280\, w ith proton and photon tagging\, and at Super Kamiokande\, extending pion t agging to muon neutrino samples. After reviewing the latest measurements o f oscillation parameters\, the status of such new analysis developments an d the plan to deploy the beam and ND280 upgrade will be presented.\n\nhttp s://indico.ific.uv.es/event/6178/contributions/15575/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15575/ END:VEVENT BEGIN:VEVENT SUMMARY:DUNE long-baseline oscillation physics sensitivity DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15570@indico.ific.uv.es DESCRIPTION:Speakers: Callum Wilkinson (Lawrence Berkeley National Laborat ory)\nThe Deep Underground Neutrino Experiment (DUNE) is a next generation \, long-baseline neutrino oscillation experiment which will utilize high-i ntensity $\\nu_{\\mu}$ and $\\bar{\\nu}_{\\mu}$ with peak neutrino energie s of ~2.5 GeV produced at Fermilab\, over a 1285 km baseline\, to carry ou t a detailed study of neutrino mixing. The neutrino beam has an initial de sign intensity of 1.2 MW\, but has a planned upgrade to 2.4 MW. The unosci llated neutrino flux will be sampled with a near detector complex at Fermi lab\, and oscillated at the DUNE far detector at the Sanford Underground R esearch Facility\, which will ultimately consist of four modules each cont aining a total liquid argon mass of 17 kt.\n\nHere\, the long-baseline neu trino oscillation sensitivity of DUNE is determined\, using a full simulat ion\, reconstruction\, and event selection of the far detector and a full simulation and parameterized analysis of the near detector. Detailed uncer tainties due to the flux prediction\, neutrino interaction model\, and det ector effects are included. DUNE is able to resolve the neutrino mass orde ring to a 5$\\sigma$ precision\, for all values of the CP-phase\, after a 66 kiloton-megawatt-year exposure (kt-MW-yr). It has the potential to obse rve charge-parity violation in the neutrino sector to a precision of 3$\\s igma$ (5$\\sigma$) after an exposure of 197 (646) kt-MW-yrs\, for 50% of a ll values of the CP-violating phase. DUNE's sensitivity to other oscillati on parameters of interest have been explored.\n\nhttps://indico.ific.uv.es /event/6178/contributions/15570/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15570/ END:VEVENT BEGIN:VEVENT SUMMARY:JUNO Oscillation Physics DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15552@indico.ific.uv.es DESCRIPTION:Speakers: Jinnan Zhang (Institute of High Energy Physics)\nThe Jiangmen Underground Neutrino Observatory is a 20 kton and 3\\%/$\\sqrt{E ({\\rm MeV})}$ multi-purpose liquid scintillator detector located at a 70 0 m underground laboratory in the south of China (Jiangmen city\, Guangdon g province). The exceptional energy resolution and the massive fiducial vo lume of the JUNO detector offer great opportunities for addressing many es sential topics in neutrino and astroparticle physics. JUNO's primary goals are to determine the neutrino mass ordering and precisely measure the rel ated neutrino oscillation parameters. With six years of data taking with r eactor anti-neutrinos\, JUNO can determine the mass ordering at a 3-4$\\si gma$ significance and the neutrino oscillation parameters $\\sin^2\\theta_ {12}$\, $\\Delta m^2_{21}$\, and $|\\Delta m^2_{31}|$ to a precision of be tter than 0.6\\%. In addition\, the atmospheric neutrino and solar neutrin o measurement at JUNO can also provide complementary and important informa tion for neutrino oscillation physics.\n\nThis talk will focus on the osci llation physics of JUNO\, which includes measurement and analysis of the r eactor neutrinos\, the atmospheric neutrinos\, and the solar neutrinos. Wi th the delicate energy response calibration and event reconstruction poten tial\, JUNO will make a world-leading measurement on the neutrino oscillat ion parameters and neutrino mass ordering in the near future.\n\nhttps://i ndico.ific.uv.es/event/6178/contributions/15552/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15552/ END:VEVENT BEGIN:VEVENT SUMMARY:Improving Hyper-Kamiokande sensitivity to CP violation with high p recision near detector electron neutrino cross-section measurements DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15551@indico.ific.uv.es DESCRIPTION:Speakers: Charlie Naseby (Imperial College London)\nThe next g eneration long-baseline neutrino oscillation experiment\, Hyper-Kamiokande \, will consist of a 260 kt underground water Cherenkov detector\, placed 295 km from the neutrino source at J-PARC. This is generated by a 1.3 MW p roton beam striking a target. In addition\, a suite of near detectors\, bo th on and off-axis will be used. With this\, Hyper-Kamiokande aims to perf orm precision measurements of the parameters governing neutrino oscillatio ns\, the observation of CP violation being one of the main aims of the exp eriment. To achieve these goals\, Hyper-Kamiokande will require smaller sy stematic uncertainties than in any previous long-baseline experiment. \n\ nMany of these systematic uncertainties are related to neutrino-nucleus in teractions\, and can be constrained by a detector placed close to the beam production point. For this\, the Hyper-Kamiokande long-baseline programme includes an Intermediate Water Cherenkov Detector\, the IWCD. This is a 5 00 tonne water Cherenkov detector located 1 km from the beam production po int. This detector is able to move within a vertical shaft and span a rang e of off-axis angles relative to the beam\, from 1 to 4 degrees. The combi nation of large target mass\, precise water Cherenkov reconstruction and o ff-axis angle flux dependence allows for high purity and high statistics e lectron neutrino and electron antineutrino samples. In this talk I will de scribe how this detector can be used to constrain the major systematic unc ertainty affecting the measurement of CP violation at Hyper-Kamiokande: th e electron neutrino and antineutrino interaction cross section.\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15551/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15551/ END:VEVENT BEGIN:VEVENT SUMMARY:CPT violation in neutrino oscillations DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15533@indico.ific.uv.es DESCRIPTION:Speakers: Christoph Andreas Ternes (INFN\, Sezione di Torino)\ nIn this talk I consider CPT violating neutrino oscillations in its most g eneral form\, i.e. assuming different oscillation parameters for neutrinos and antineutrinos. In this scenario the measurement of oscillation parame ters is much more difficult than in the standard case. I will discuss the implication on the recent CP measurements in T2K and NOvA\, and also discu ss how well current experiments can bound different neutrino and antineutr ino parameters. Finally\, I will discuss how well the upcoming DUNE experi ment might improve the current bounds.\n\nhttps://indico.ific.uv.es/event/ 6178/contributions/15533/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15533/ END:VEVENT BEGIN:VEVENT SUMMARY:New unitarity constraints on the tau row DTSTART;VALUE=DATE-TIME:20210830T154000Z DTEND;VALUE=DATE-TIME:20210830T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15532@indico.ific.uv.es DESCRIPTION:Speakers: Julia Gehrlein (Brookhaven National Laboratory)\nTes ting the unitarity of the PMNS matrix can give insights into the existence of additional neutrino generations which would render the 3x3 leptonic mi xing matrix non-unitarity. Current oscillation data mostly constrains the electron and muon row of the mixing matrix whereas the tau row still allow s for large unitarity violation. Here we will focus on new unitary constra ints on the tau row coming from previously overlooked experimental data.\n \nhttps://indico.ific.uv.es/event/6178/contributions/15532/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15532/ END:VEVENT BEGIN:VEVENT SUMMARY:Non-standard neutrino oscillations: perspective from unitarity tri angles DTSTART;VALUE=DATE-TIME:20210830T152500Z DTEND;VALUE=DATE-TIME:20210830T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15531@indico.ific.uv.es DESCRIPTION:Speakers: Poonam Mehta (Jawaharlal Nehru University)\nWe formu late an alternative approach based on unitarity triangles to describe neut rino oscillations in presence of non-standard interactions (NSI). Using pe rturbation theory\, we derive the expression for the oscillation probabili ty in case of NSI and cast it in terms of the three independent parameters of the leptonic unitarity triangle (LUT). The form invariance of the prob ability expression (even in presence of new physics scenario as long as th e mixing matrix is unitary) facilitates a neat geometric view of neutrino oscillations in terms of LUT. We examine the regime of validity of perturb ative expansions in the NSI case and make comparisons with approximate exp ressions existing in literature. We uncover some interesting dependencies on NSI terms while studying the evolution of LUT parameters and the Jarlsk og invariant. Interestingly\, the geometric approach based on LUT allows u s to express the oscillation probabilities for a given pair of neutrino fl avours in terms of only three (and not four) degrees of freedom which are related to the geometric properties (sides and angles) of the triangle. Mo reover\, the LUT parameters are invariant under rephasing transformations and independent of the parameterization adopted.\n\nhttps://indico.ific.uv .es/event/6178/contributions/15531/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15531/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct measurement of topological information using HUNI-ZICOS det ector for 96Zr neutrinoless double beta decay experiment DTSTART;VALUE=DATE-TIME:20210831T154000Z DTEND;VALUE=DATE-TIME:20210831T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15466@indico.ific.uv.es DESCRIPTION:Speakers: Yoshiyuki Fukuda (Miyagi University of Education)\nA liquid scintillator containing a tetrakis (isopropyl acetoacetato) zircon ium (Zr(iPrac)$_{4}$) has been developed for ZICOS experiment which will s earch for neutrinoless double beta decay (0$\\nu\\beta\\beta$) events usin g $^{96}$Zr isotope. The liquid scintillator has 10wt.% concentration of Z r(iPrac)$_{4}$\, which corresponds to 1.4wt.% of natural zirconium.\n In o rder to investigate a half-life of 0$\\nu\\beta\\beta$ over 10$^{27}$ year s\, which corresponds to neutrino mass less than 0.01eV\, we have to use t ons scale of $^{96}$Zr isotope\, and have to reduce 95% of backgrounds fro m $^{208}$Tl beta decay whose energy overlaps with the signal region. \n F or latter case\, we have developed new technique to use Cherenkov light in order to reduce those backgrounds using the topology of location for phot omultipliers received Cherenkov light\, and have obtained that 93% of $^{2 08}$Tl decay events could be reduced with 78% efficiency for 0$\\nu\\beta\ \beta$ events. In order to realize this technique\, we have developed the pulse shape discrimination to extract Cherenkov signal among scintillation \, and have measured those topology using the hemisphere detector HUNI-ZIC OS.\n Here we report recent progress from those measurements\, explain the status of demonstration of background reduction using UNI-ZICOS detector\ , and discuss about prototype ZICOS detector which will measure signal fro m 2$\\nu\\beta\\beta$ as physics program.\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15466/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15466/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing the dark matter of a three-loop radiative neutrino mass ge neration model with the Cherenkov Telescope Array DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15917@indico.ific.uv.es DESCRIPTION:Speakers: Talal Ahmed Chowdhury (University of Dhaka)\nWe inve stigate the prospect of detecting the dark matter (DM) candidate in the th ree-loop radiative neutrino mass generation model extended with large elec troweak multiplets of the Standard Model (SM) gauge group\, at the future imaging atmospheric Cherenkov telescope known as the Cherenkov Telescope A rray (CTA). We find that the addition of such large electroweak multiplets leads to a sizable Sommerfeld enhanced annihilation of the DM with an O(T eV) mass\, into the SM gauge bosons\, which results in continuum- and line -like spectra of very high-energy (VHE) gamma rays\, and therefore becomes observable for the CTA. We determine the viable models by setting the upp er limit on the SU(2)L isospin of the multiplets from the partial-wave uni tarity constraints and the appearance of a low-scale Landau pole in the ga uge coupling. Afterwards\, by considering the continuum VHE gamma rays pro duced from the DM annihilation at the Galactic Center\, we probe the param eter space of the model using the sensitivity reach of the CTA.\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15917/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15917/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for dark matter signals toward the irregular dwarf galaxy W LM with H.E.S.S. DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15896@indico.ific.uv.es DESCRIPTION:Speakers: Celine Armand (Astronomy department\, University of Geneva)\nCosmological and astrophysical probes suggest that dark matter (D M) makes up for 85% of the total matter of the Universe. The determination of its nature\, however\, remains one of the greatest challenges of funda mental Physics. In the DM indirect detection framework\, Weakly Interactin g Massive Particles (WIMPs) particles would produce signals by self-annihi lating and creating SM products such as γ rays\, which might be detected by ground-based telescopes. Dwarf irregular galaxies represent promising t argets for the search for DM as they are assumed to be dark matter dominat ed. These dwarf irregular galaxies are rotationally supported with relativ ely simple and well measured kinematics which lead to small uncertainties on their dark matter distribution profiles. In 2018\, the H.E.S.S. telesco pes observed the irregular dwarf galaxy Wolf-Lundmark-Melotte (WLM) for 18 hours. These observations are the very first ones made by an imaging air Cherenkov telescope toward this kind of objects. We search for a DM signal looking for excess of γ rays towards WLM dwarf galaxy. We perform the fi rst analysis of this source in stereoscopy using the data taken by the fiv e H.E.S.S. telescopes. We present the new results on the observations of W LM interpreted in terms of velocity-weighted cross section for DM self-ann ihilation ⟨σv⟩ as a function of DM particle mχ mass for eight annihi lation channels: b ̄b\, W+W−\, τ+τ−\, Z+Z−\, e+e−\, μ+μ−\, tt ̄as continuum spectra and the prompt emission γγ .\n\nhttps://indico .ific.uv.es/event/6178/contributions/15896/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15896/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for gamma-ray line emission from Dark Matter annihilation i n the Galactic Centre with the MAGIC telescopes DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15892@indico.ific.uv.es DESCRIPTION:Speakers: Tomohiro Inada (ICRR\, UTokyo)\nWe present the searc h for dark matter (DM) spectral lines in the Galactic centre (GC) region w ith the MAGIC telescopes. The MAGIC telescopes\, located on the Canary isl and of La Palma (Spain)\, are sensitive to photons in the energy range fro m 50 GeV to 50 TeV with low zenith angle observations. MAGIC has performed indirect DM searches with various astrophysical targets. Since the MAGIC telescopes are located in the northern hemisphere\, the GC is visible only at high zenith angles. Observations at high zenith angles significantly i ncrease the telescopes' effective collection area\, which boosts sensitivi ty for gamma rays in the TeV regime. We report the results obtained with m ore than 200 hours of high zenith angle observations of the GC region with MAGIC.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15892/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15892/ END:VEVENT BEGIN:VEVENT SUMMARY:Multi-messenger lifetime constraints on heavy decaying dark matter DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15886@indico.ific.uv.es DESCRIPTION:Speakers: Rasmi Enrique Hajjar Muñoz (SSM (Università di Nap oli) - IFIC (CSIC-UV))\nDark matter is one of the cornerstones of the stan dard cosmological model although we do not know its fundamental nature. Hu ge effort has been made in order to perform a direct detection of this dar k matter component but up to now we have only seen it interacting gravitat ionally. In this regard the indirect detection is a promising method to se arch for dark matter\, where we try to look at signatures of the dark matt er on the astrophysical messengers. \nOne of the best known astrophysical messengers are the gamma-rays. At very-high energies gamma-rays suffer fro m absorption\, leaving the galactic prompt gamma-ray component as the domi nant one. In this work we will adopt the prompt flux as the total one.\nHe avy dark matter with $m_\\mathrm{DM}>10^7~\\mathrm{GeV}$ leads to higher f luxes in the decaying scenario rather than the annihilating one. In this w ork we focus on heavy decaying dark matter particles and we revisit the da rk matter lifetime bounds placed by the gamma-ray measurements by means of the spectra provided by the recent code HDMSpectra. We provide lifetime l imits for dark matter particles with $m_\\mathrm{DM}=[10^7-10^{15}]~\\math rm{GeV}$ for a set of decay scenarios\, where we include the current measu rements that provide upper limits on the gamma-ray flux.\n\nhttps://indico .ific.uv.es/event/6178/contributions/15886/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15886/ END:VEVENT BEGIN:VEVENT SUMMARY:Shedding light on low-mass subhalo survival with numerical simulat ions DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15852@indico.ific.uv.es DESCRIPTION:Speakers: Alejandra Aguirre-Santaella (IFT UAM-CSIC)\nIn this work\, we carry out a suite of specially-designed numerical simulations th at employ a supercluster computational power to shed further light on dark matter (DM) subhalo survival at mass scales relevant for gamma-ray DM sea rches\, a topic subject to intense debate nowadays. Specifically\, we have employed a GPU N-body code to study the evolution of low-mass subhalos in side a Milky Way-like halo with unprecedented accuracy\, paying particular attention to subhalos at the solar galactocentric radius. We have simulat ed subhalos with varying mass\, concentration\, and orbital properties\, a nd considered the effect of the gravitational potential of the Milky-Way g alaxy itself. These results provide detailed predictions that will aid cur rent and future quests for the nature of dark matter.\n\nhttps://indico.if ic.uv.es/event/6178/contributions/15852/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15852/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for dark matter subhalos with the Fermi-LAT DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15836@indico.ific.uv.es DESCRIPTION:Speakers: Javier Coronado-Blázquez (IFT UAM CSIC)\nΛCDM pred icts the existence of dark matter (DM) subhalos\, most of them not massive enough to retain gas (i.e.\, baryons) and become visible. If DM is compos ed of Weakly Interacting Massive Particles (WIMPs)\, we expect them to ann ihilate in subhalos\, producing gamma rays which can be detected with the Large Area Telescope (LAT) onboard the Fermi satellite\, and appearing as unidentified sources (unIDs) in the gamma-ray sky. We characterize the LAT sensitivity to DM and compare the sample of unIDs in LAT catalogs - previ ously filtered according to the expected DM annihilation signal - to predi ctions from the Via Lactea II (VL-II) N-body cosmological simulation\, rep opulated with low-mass subhalos below its mass resolution limit. This exer cise allows us to place conservative and robust constraints on the annihil ation cross section vs. WIMP mass parameter space. A spectral and spatial dedicated analysis is then performed for the best DM subhalo candidates\, using a decade of Fermi-LAT data. Finally\, we also quantify whether spati al extension is\, as often claimed\, a “smoking gun” for DM subhalo de tection\, by simulating the LAT response to extended subhalos. This talk w ill be based on [1906.11896\, 1910.14429] and ongoing work within the Ferm i-LAT collaboration.\n\nhttps://indico.ific.uv.es/event/6178/contributions /15836/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15836/ END:VEVENT BEGIN:VEVENT SUMMARY:A search for dark matter using sub- PeV gamma-rays observed by Tib et ASγ DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15824@indico.ific.uv.es DESCRIPTION:Speakers: Tarak Maity (Centre for High Energy Physics\, Indian Institute of Science\, Bengaluru\, Karnataka 560012\, India)\nThe discove ry of diffuse sub-PeV gamma-rays by the Tibet ASγ​ collaboration promis es to revolutionize our understanding of the high-energy astrophysical uni verse. It has been shown that this data broadly agrees with prior theoreti cal expectations. We study the impact of this discovery on a well-motivate d new physics scenario: PeV-scale decaying dark matter (DM). Considering a wide range of final states in DM decay\, a number of DM density profiles\ , and numerous astrophysical background models\, we find that this data pr ovides the most stringent limit on DM lifetime for various Standard Model final states. In particular\, we find that the strongest constraints are d erived for DM masses in between a few PeV to few tens of PeV. Near future data of these high-energy gamma-rays can be used to discover PeV-scale dec aying DM.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15824/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15824/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for dark matter annihilation signals from unidentified Ferm i-LAT objects with H.E.S.S. DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15811@indico.ific.uv.es DESCRIPTION:Speakers: Alessandro Montanari (CEA Saclay / Irfu-DPhP - Unive rsité Paris Saclay)\nMilky Way-sized galaxies harbor a population of unme rged dark matter subhalos\, as shown from cosmological N-body simulations. These subhalos could shine in gamma-rays and be eventually detected as un identified sources in gamma-ray surveys. From a thorough selection of unid entified Fermi-LAT Objects (UFOs)\, we observe four UFOs with H.E.S.S. and we search for very high-energy (VHE\, E ≥ 100 GeV) gamma-ray emission. Considering dark matter masses above a few hundred GeV\, the observed UFOs could be identified as dark matter subhalos\, given their hard gamma-ray spectra in the few-ten-to-hundred GeV energy range. Since no significant v ery-high-energy gamma-ray emission is detected in any of the four UFOs dat aset nor in the combined one\, we derive constraints on the product of the velocity-weighted annihilation cross-section by the J-factor for the dar k matter models. We derive 95% CL upper limits on J in W$^+$W$^-$ and $\\t au^+$$\\tau^-$ annihilation channels for the TeV dark matter particles. Co nsidering thermal WIMPs\, we derive constraints on the J-factors from the H.E.S.S. observations. Assuming model-dependent predictions from cosmologi cal N-body simulations on the J-factor distribution for Milky Way-sized ga laxies\, the dark matter models with masses greater than 0.3 TeV for the U FO emissions can be ruled out at high confidence level.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15811/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15811/ END:VEVENT BEGIN:VEVENT SUMMARY:Multi-messenger constraints on the dark matter interpretation of t he Fermi-LAT Galactic center excess DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15806@indico.ific.uv.es DESCRIPTION:Speakers: Mattia Di Mauro (INFN Torino)\nThe excess of gamma r ays in the data measured by the Fermi Large Area Telescope from the Galact ic center region is one of the most intriguing mysteries in Astroparticle Physics. This Galactic center excess (GCE)\, has been measured with respec t to different interstellar emission models\, source catalogs\, data selec tions and techniques. Although several proposed interpretations have appea red in the literature\, there are no firm conclusions as to its origin. Th e main difficulty in solving this puzzle lies in modeling a region of such complexity and thus precisely measuring the characteristics of the GCE. I n this presentation I will show the results obtained for the GCE by using 11 years of Fermi-LAT data\, state of the art interstellar emission models \, and the newest 4FGL source catalog to provide precise measurements of t he energy spectrum\, spatial morphology\, position\, and sphericity of the GCE. I will also present constraints for the interpretation as dark matte r particle interactions using the GCE\, a gamma-ray analysis of dwarf sphe roidal galaxies with LAT data and AMS-02 cosmic-ray antiprotons and positr ons flux data.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15806 / LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15806/ END:VEVENT BEGIN:VEVENT SUMMARY:Integral X-ray constraints on sub-GeV dark matter DTSTART;VALUE=DATE-TIME:20210902T154000Z DTEND;VALUE=DATE-TIME:20210902T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15805@indico.ific.uv.es DESCRIPTION:Speakers: Elena Pinetti (University of Turin\, INFN & Sorbonne University)\nDark matter (DM) in cosmic structures is expected to produce signals originating from its particle physics nature\, among which the el ectromagnetic emission represents a relevant opportunity. One of the major candidates for DM are weak-scale particles\, however no convincing signal of them has been observed so far. For this reason\, alternative candidate s are getting increasing attention\, notably sub-GeV particles\, which are the subject of our work. The challenge in indirect detection of sub-GeV D M is that there is scarcity of competitive experiments in the energy range between 1 MeV and hundreds of MeV\, hence we need to find alternative way s to study DM candidates with mass in this energy window. In our work we p roposed to look at energies much lower than the mass of the sub-GeV DM par ticles by including the contribution from Inverse-Compton scattering in th e total flux. In particular\, the electrons and positrons produced by DM p articles give rise to X-rays by upscattering the low-energy photons of the radiation fields in the Galaxy (CMB\, infrared from dust\, optical starli ght). These X-rays fall in the energy range covered by the INTEGRAL data\, which we used to determine conservative bounds on the DM annihilation cro ss-section. We considered three annihilation channels: electron\, muon and pion. As a result\, we derived competitive constraints for DM particles w ith a mass between 150 MeV and 1.5 GeV.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15805/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15805/ END:VEVENT BEGIN:VEVENT SUMMARY:Dynamical mass measurements and the local dark matter density—re cent developments and challenges DTSTART;VALUE=DATE-TIME:20210902T152500Z DTEND;VALUE=DATE-TIME:20210902T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15803@indico.ific.uv.es DESCRIPTION:Speakers: Axel Widmark (Niels Bohr Institute\, Copenhagen Univ ersity)\nDynamical mass measurements inform us of the local dark matter de nsity\, which is a crucial quantity for direct and indirect dark matter se arches. Thanks to the Gaia mission\, the kinematics of the Milky Way are m apped with a greater depth and precision than ever before. Despite this\, a strong consensus has not emerged regarding our galaxy’s gravitational potential and matter density distribution. Gaia has highlighted non-statio nary dynamics that bias traditional methods that are based on the assumpti on of a steady state (e.g. Jeans modelling). Furthermore\, uncertainties o f the baryonic distribution are still significant. We review recent progre ss and challenges in this field. We also highlight a couple of alternative methods that are not contingent on the assumption of stationarity\, for e xample a new method for weighing the galactic disk using the phase-space s piral that was discovered with Gaia. A better understanding and modelling of the Milky Way’s time-varying dynamics will improve the precision and accuracy of local dark matter density determinations.\n\nhttps://indico.if ic.uv.es/event/6178/contributions/15803/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15803/ END:VEVENT BEGIN:VEVENT SUMMARY:Circular polarisation of gamma rays as a probe of dark matter-cosm ic ray electron interactions DTSTART;VALUE=DATE-TIME:20210902T151000Z DTEND;VALUE=DATE-TIME:20210902T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15788@indico.ific.uv.es DESCRIPTION:Speakers: Marina Cermeño Gavilán (UCLouvain (CP3))\nDark Mat ter (DM) constitutes most of the matter in the presently accepted cosmolog ical model for our Universe. However\, despite the increased sensitivity o f direct and indirect DM searches\, and the latest LHC run at 13 TeV centr e of mass energy\, no signal from DM particles has been detected so far\, leading to exclusion limits on the parameter space of DM models. Conventio nal indirect searches look for an excess in the electromagnetic emission f rom the sky that cannot be attributed to known astrophysical sources\, but polarisation is so far not being explored.\n\nIn this talk\, I will argue that the photon polarisation is an important feature to understand new ph ysics interactions. In particular\, circular polarisation can be generated from Beyond the Standard Model (BSM) interactions if they violate parity and there is an asymmetry in the number of particles which participate in the interaction. I will consider a simplified model for fermionic (Majoran a) DM and study the circularly polarised gamma rays below 10 GeV from DM c osmic ray electron interactions. I will study the differential flux of pos itive and negative polarised photons from the Galactic Centre and show tha t the degree of circular polarization can reach up to 90%. Finally\, I wil l discuss the detection prospects of this signal in future experiments.\n\ nhttps://indico.ific.uv.es/event/6178/contributions/15788/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15788/ END:VEVENT BEGIN:VEVENT SUMMARY:Paleo-Detectors - Digging for Dark Matter (and Neutrinos) DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15916@indico.ific.uv.es DESCRIPTION:Speakers: Sebastian Baum (Stanford University)\nPaleo-Detector s are natural minerals which record damage tracks from nuclear recoils ove r geological timescales. Minerals commonly found on Earth are as old as a billion years\, and modern microscopy techniques may allow to reconstruct damage tracks with nanometer scale spatial resolution. Thus\, paleo-detect ors would constitute a technique to achieve keV recoil energy threshold wi th exposures comparable to a kiloton-scale conventional "real-time" detect or. In this talk\, I will discuss the potential of paleo-detectors for the direct detection of dark matter as well as for detecting low-energy neutr inos as are e.g. emitted by core collapse supernovae or our Sun. Furthermo re\, the age of the minerals provides the ability to look back across Gyr- timescales\, giving paleo detectors the unique ability to probe changes in the cosmic ray rate or the galactic supernova rate over such timescales a s well as dark matter substructure Earth might have encountered during its past few trips around our Galaxy.\n\nhttps://indico.ific.uv.es/event/6178 /contributions/15916/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15916/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark Matter Search with the Nuclear Isomer Ta-180m DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15900@indico.ific.uv.es DESCRIPTION:Speakers: Bjoern Lehnert (Berkeley Lab)\nThere is compelling c osmological and astrophysical evidence of dark matter comprising 27% of th e energy budget of the Universe. However\, dark matter has never been obse rved in direct detection experiments. The long-time favorite model of Weak ly Interacting Massive Particles saw a large experimental effort with stea dy progress over recent decades. Since also these large-scale searches rem ain unsuccessful to date\, it is compelling to look at more exotic dark ma tter models which can be constrained with new approaches and much less sci entific resources. Using nuclear isomers is one of these approaches.\n\nTa -180m is the rarest known isotope and the longest-lived meta-stable state whose half-life limits are on the order of $10^{16}$ yr. We investigate ho w strongly interacting dark matter collides with Ta-180m\, leading to its de-excitation. The energy stored in the meta-stable state is released in t he transition\, which becomes the signature for thermalized dark matter i n a well-shielded underground experiment.\n\nWe report on a direct detecti on experiment searching for these dark-matter-induced decay signatures. Th is search has further constrained open parameter space of cross-section\, mass\, and component fraction of strongly interacting dark matter. We also propose an indirect geological experiment to search for decay products of Ta-180m in tantalum minerals accumulated over 1 billion years.\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15900/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15900/ END:VEVENT BEGIN:VEVENT SUMMARY:Atomic Compton scattering effect on direct dark matter detection DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15884@indico.ific.uv.es DESCRIPTION:Speakers: Chang-Hao Fang (Sichuan University)\nAtomic Compton scattering effect significantly contributes to low-energy electronic recoi ls below its k-shell energy for the direct dark matter detection. Searches on ADM models\, dark photon models\, leptophilic dark matter models as we ll as the conventional WIMPs for background understandings are vitally req uired to clarify the effect. We employed the relativistic impulse approxim ation (RIA) together with the ab initio Multiple-configuration Dirac-Fock theory to obtain the atomic Compton scattering [1] for Germanium (Ge) Sili con (Si) and Xenon(Xe) atoms. Comparisons on low momentum transfer regions with our calculations for Ge and Si are achieved. [2] In addition\, milli charged dark matter particles estimated by RIA in the atomic ionization fo r Ge and Xe has been evaluated. [3] A factor-of-two discrepancy on the inc oherent-scattering factor(Scattering Function) near 100 eV momentum transf er with the Ge system between our calculation and the latest version of Ge ant4 simulation data is observed. Plans on the experimental verification a nd the perspectives of the atomic Compton scattering effect for the direct detections will be discussed. \n\n[1]C.K.Qiao et al.\, Journal of Physics B: Atomic\, Molecular and Optical Physics\, 53(07)\, 075002 (2020)\n[2] C .K.Qiao et al.\, Journal of Physics G 47\, 4\, 045202(2020)\n[3] C.K.Qiao et al.\, Journal of High Energy Physics\, 03\, 184 (2021)\n\nhttps://indic o.ific.uv.es/event/6178/contributions/15884/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15884/ END:VEVENT BEGIN:VEVENT SUMMARY:Atomic Many-body Approaches for Constraining DM-electron Interacti ons DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15881@indico.ific.uv.es DESCRIPTION:Speakers: Chih-Pan Wu (Université de Montréal)\nDetectors wi th low thresholds for electron recoil (ER) open a new window to direct sea rches of sub-GeV dark matter (DM) candidates. These experimental studies n eed important theory inputs: the DM scattering rates at detectors through some assumed DM-electron interactions. In this talk\, I will present the r esults of our study on DM-atom scattering through DM-electron interactions at leading order in the context of effective field theory. Our atomic man y-body approach is properly benchmarked by atomic data involving not only bound but also continuum states\, with a conservative 20% error estimate f or DM-xenon and DM-germanium scattering with ER above 12 and 80 eV\, respe ctively. Compared with conventional approaches based on non-relativistic\, independent-particle frameworks\, the importance of relativistic effects and many-body correlation will be highlighted and discussed.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15881/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15881/ END:VEVENT BEGIN:VEVENT SUMMARY:Crystal responses to general dark matter-electron interactions DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15873@indico.ific.uv.es DESCRIPTION:Speakers: Einar Urdshals (Chalmers)\nIn this work we develop a formalism to describe the scattering of dark matter (DM) particles by ele ctrons bound in crystals for general forms of non-relativistic DM-electron interactions. Our novel response to the study of DM-electron interactions allows probing DM with mass down to a fraction of an MeV in a model indep endent way. \n\nUsing a state of the art DFT calculation we apply our form alism to the cases of silicon and germanium\, materials currently being us ed in direct detection experiments. We are thus able to predict the rate o f electron excitations to the conduction band\, and use this to compute ex clusion limits for the strength of DM-electron interactions based on the n ull-results of the SENSEI and EDELWEISS experiments.\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/15873/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15873/ END:VEVENT BEGIN:VEVENT SUMMARY:Solar reflection of sub-GeV dark matter DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15869@indico.ific.uv.es DESCRIPTION:Speakers: Timon Emken (Stockholm University)\nDirect detection experiments are searching for rare interactions between dark matter (DM) particles and ordinary matter. If the mass of these dark particles is too low\, their kinetic energy does not suffice to trigger these detectors lea ving them incapable to observe DM. Processes that boost DM particles can t herefore extend the observational reach of direct DM searches to lower mas ses. I will discuss the mechanism and phenomenology of solar reflection\, where DM particles get accelerated via a collision with a solar electron o r nucleus. Compared to standard halo DM\, solar reflection not only allows to probe lighter masses\, a solar reflection signal would also feature a novel modulation signature.\n\nhttps://indico.ific.uv.es/event/6178/contri butions/15869/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15869/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct detection of non-galactic light dark matter DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15864@indico.ific.uv.es DESCRIPTION:Speakers: Gonzalo Herrera (Technical University of Munich\, Ma x-Planck Institute for Physics)\nA fraction of the dark matter in the sola r neighborhood might be composed of non-galactic particles with speeds lar ger than the escape velocity of the Milky Way. The non-galactic dark matte r flux would enhance the sensitivity of direct detection experiments\, due to the larger momentum transfer to the target.\n\nIn this note\, we calcu late the impact of the dark matter flux from the Local Group and the Virgo Supercluster diffuse components in nuclear and electron recoil experiment s. The enhancement in the signal rate can be very significant\, especially for experiments searching for dark matter induced electron recoils.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15864/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15864/ END:VEVENT BEGIN:VEVENT SUMMARY:The impact of operator interference in dark matter direct detectio n experiments DTSTART;VALUE=DATE-TIME:20210902T154000Z DTEND;VALUE=DATE-TIME:20210902T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15849@indico.ific.uv.es DESCRIPTION:Speakers: Anja Brenner (Max-Planck-Institut für Physik and TU M)\nThe non-relativistic effective theory of WIMP-nucleon interactions dep ends on 28 coupling strengths. Due to the vast parameter space of the effe ctive theory\, most direct detection experiments interpret the results of their searches assuming that only one of the coupling strengths is non-zer o. On the other hand\, dark matter models generically lead in the non-rela tivistic limit to several interactions which interfere with one another\, therefore\, the published limits cannot be straightforwardly applied to mo del predictions. We present a method to determine a rigorous upper limit o n the WIMP-nucleon interaction strength including all possible interferenc es among operators. We illustrate the method using the null search results from the XENON1T and the PICO collaborations\; for some interactions\, th e limits on the coupling strengths are relaxed up to one order of magnitud e. We also present a method that allows to combine the results from differ ent experiments\, thus exploiting the synergy between different targets in exploring the parameter space of WIMP-nucleon interactions.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15849/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15849/ END:VEVENT BEGIN:VEVENT SUMMARY:DM-like anomaly in neutron multiplicity spectra DTSTART;VALUE=DATE-TIME:20210902T152500Z DTEND;VALUE=DATE-TIME:20210902T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15843@indico.ific.uv.es DESCRIPTION:Speakers: Wladyslaw Henryk Trzaska (University of Jyvaskyla)\n A new experiment collects data\, since November 2019\, at a depth of 210 m .w.e. in the Callio Lab [1] in the Pyhasalmi mine [2] in Finland. The setu p\, called NEMESIS (New EMma Experiment Searching for Indirect Signals)\, incorporates infrastructure from the EMMA experiment [3] with neutron and large-area plastic scintillator detectors of the MAZE system [4]. The expe riment's primary aim is to combine muon tracking with position-sensitive n eutron detection to measure precision yields\, multiplicities\, and latera l distributions of high-multiplicity neutron events induced by cosmic muon s in various materials. The data are relevant for background evaluation of the deep-underground searches for Dark Matter (DM)\, neutrino-less double beta decay\, etc. \n\nPreliminary analysis revealed anomalies in muon-sup pressed neutron multiplicity spectra collected during a 349-day run (live time) with a 565 kg Pb target. The spectra\, well described by a power-law fit\, show three peaks at high multiplicities. Although still at a low st atistical significance\, these small excesses match the outcome of an earl ier measurement [5]. The nature of the anomalies remains unclear\, but\, i n principle\, they may be a signature of self-annihilation of a WIMP with a mass close to 10 GeV/c2 [6]. With that assumption\, the expected cross- section would be around 10^-42 cm2 for Spin Dependant and 10^-46 cm2 for S pin Independent interactions. We propose verifying this hypothesis with an upgraded NEMESIS experiment\, able to collect an order of magnitude more data than this measurement. Based on the statistical uncertainty\, analysi s of the event rate indicates that cross-section limits for DM mass range of approximately 3-40 GeV/c2 can be investigated with such a setup.\n\n1. Callio\, https://callio.info \n2. W.H. Trzaska et al.\, (2018)\, https://a rxiv.org/abs/1810.00909 \n3. P. Kuusiniemi et al.\, AP 102(2018)67 https:/ /www.sciencedirect.com/science/article/abs/pii/S092765051730333X \nM. Kasz telan et al.\, (2006) Proc. the 20th ECRS\, Lisbon\nhttps://www.lip.pt/eve nts/2006/ecrs/proc/ecrs06-s0-92.pdf\n5. T. Ward\, private communication an d AIP Conference Proceedings 842\, 1103 (2006)\; https://doi.org/10.1063/1 .2220467 \n6. T.E. Ward et al.\, APS April Meeting 2019\, https://meetings .aps.org/Meeting/APR19/Session/G17.1\n\nhttps://indico.ific.uv.es/event/61 78/contributions/15843/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15843/ END:VEVENT BEGIN:VEVENT SUMMARY:WimPyDD: an object-oriented Python code for WIMP-nucleus scatterin g direct detection in virtually any scenario DTSTART;VALUE=DATE-TIME:20210902T151000Z DTEND;VALUE=DATE-TIME:20210902T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15841@indico.ific.uv.es DESCRIPTION:Speakers: Gaurav Tomar (Technical University of Munich)\nWe in troduce WimPyDD\, a modular\, object–oriented and customisable Python co de that accurately predicts the expected WIMP-nucleus scattering rates in WIMP direct–detection experiments including the response of the detector . WimPyDD utilises the framework of Galilean–invariant non–relativisti c effective theory\, allowing to handle an arbitrary number of effective o perators\, and can perform the calculation of the excepted rate in virtual ly any scenario\, including inelastic scattering\, WIMPs with an arbitrar y spin\, and a generic velocity distribution in the Galactic halo. The pow er and flexibility of WimPyDD will be discussed in some explicit examples as well as in several published results.\n\nhttps://indico.ific.uv.es/even t/6178/contributions/15841/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15841/ END:VEVENT BEGIN:VEVENT SUMMARY:Indirect Dark Matter searches towards the Sun with ANTARES neutrin o telescope DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15912@indico.ific.uv.es DESCRIPTION:Speakers: Chiara Poirè (UPV)\nDark matter particles\, produce d in astrophysical sources and gravitationally captured in massive celesti al objects\, can be indirectly detected through their annihilation into St andard Model particles.\nThe centre of those massive objects is\, therefor e\, a place where to look for a possible neutrino excess from dark matter annihilations\, using neutrino telescopes.\nThe deep-sea neutrino telescop e ANTARES\, located in the Mediterranean Sea\, has shown to be very compet itive on the quest for dark matter WIMPs produced in the Galactic Center.\ nThe closest promising DM source is the Sun\, where it is possible to have a very clean signal since the background from astrophysical sources is no t expected.\nIn this work we show the results on the search for dark matte r WIMPs from the Sun\, using 13 years of data collected by ANTARES.\n\nhtt ps://indico.ific.uv.es/event/6178/contributions/15912/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15912/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraining Dark Matter Annihilation with Cosmic Ray Antiprotons using Neural Networks DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15861@indico.ific.uv.es DESCRIPTION:Speakers: Kathrin Nippel (RWTH Aachen University)\nThe interpr etation of indirect detection experiments searching for dark matter annihi lations requires computationally expensive simulations of cosmic-ray propa gation. We present a new method based on Recurrent Neural Networks (RNNs) that significantly accelerates simulations of secondary and dark matter co smic ray antiprotons. This approach allows for an efficient marginalizatio n over the nuisance parameters of a cosmic ray propagation model in order to perform parameter scans for a wide range of dark matter models. We pres ent resulting constraints using the most recent AMS-02 antiproton data on dark matter WIMP models. The speed-up achieved with our method results in a runtime two orders of magnitude below a conventional MCMC approach\, on ce the neural network has been trained.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15861/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15861/ END:VEVENT BEGIN:VEVENT SUMMARY:The GAPS experiment - Searching for Dark Matter using Cosmic-ray A ntinuclei DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15847@indico.ific.uv.es DESCRIPTION:Speakers: Riccardo Munini (INFN - Trieste)\nThe General Antipa rticle Spectrometer (GAPS) is a balloon-borne detector designed to search for dark matter search by measuring low-energy (\n\nhttps://indico.ific.uv .es/event/6178/contributions/15847/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15847/ END:VEVENT BEGIN:VEVENT SUMMARY:Perspectives for anti deuteron search in cosmic rays with an heliu m calorimeter DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15830@indico.ific.uv.es DESCRIPTION:Speakers: Francesco Nozzoli (Istituto Nazionale Fisica Nuclear e (INFN) - TIFPA)\nLow energy anti-deuterons in cosmic rays are considered a golden channel for the search of Dark matter annihilations in the Galax y.\nAnti Deuteron Helium Detector (ADHD) project is aiming to study the si gnature offered by an high pressure Helium target for the identification o f anti-deuterons in cosmic rays.\nIn particular exotic atoms are produced by stopping anti-protons/anti-deuterons in the gas and the captured partic le can orbit the Helium nucleus for microseconds before the annihilation. This meta-stability is a unique feature for the Helium target and the char acteristic delayed annihilation is a distinctive signature to identify the antimatter nature of the stopping particle. \nA possible configuration fo r ADHD space/balloon detector consists of a pressurized helium calorimeter surrounded by scintillator layers for velocity measurement.\nAnti-deutero ns are identified by combining the spectrometric measurement of the stoppi ng particle (velocity/energy) with the delayed emission of outgoing charge d pions caused by the annihilation.\nA prototype of the pressurized calori meter\, filled by 200 Bar Helium acting as a scintillator\, has been chara cterized with cosmic muons and with 70-240 MeV proton beam in the INFN-TIF PA laboratory.\nSensitivity of the possible Anti-Deuteron-Helium-Detector for the measurement of low energy anti-deuterons and anti-protons in cosmi c rays will be summarized and the results of the measured performance of t he helium calorimeter prototype will be shown.\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15830/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15830/ END:VEVENT BEGIN:VEVENT SUMMARY:Underground detections of an extra gauge interacting sterile neutr ino dark matter DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15828@indico.ific.uv.es DESCRIPTION:Speakers: Osamu Seto ()\nWe show that decay products from ster ile neutrino dark mater in extra U(1) models are detectable in both direct dark matter detection experiments and neutrino telescope. The sterile neu trino dark matter interacts with a light gauge boson and decays into neutr inos. Those neutrinos could scatter off nuclei with a large enough recoil energy in direct dark matter detection experiments as WIMPs do.\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15828/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15828/ END:VEVENT BEGIN:VEVENT SUMMARY:New Ideas of Probing Sterile Neutrino Dark Matter DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15823@indico.ific.uv.es DESCRIPTION:Speakers: Yue Zhang (Carleton University)\nSterile neutrino is a simple and elegant dark matter candidate. In its minimal incarnation\, the original Dodelson-Widrow mechanism that explains the relic abundance h as been in strong tension with the indirect detection limits. I present th e self interacting neutrino scenario\, mediated by a Majoron-like scalar o r vector boson\, as a novel solution to the above tension. It can accommod ate new production mechanisms for sterile neutrino dark matter\, open up a wide parameter space\, and result in a number of testable signatures from laboratory to the cosmos.\n\nhttps://indico.ific.uv.es/event/6178/contrib utions/15823/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15823/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for WIMPs in the Large Magellanic Cloud DTSTART;VALUE=DATE-TIME:20210901T152500Z DTEND;VALUE=DATE-TIME:20210901T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15807@indico.ific.uv.es DESCRIPTION:Speakers: Marco Regis (University of Torino and INFN)\nWe pres ent a radio search for WIMP dark matter in the Large Magellanic Cloud (LMC ). We make use of a recent deep image of the LMC obtained from observation s of the Australian Square Kilometre Array Pathfinder (ASKAP)\, taken as p art of the Evolutionary Map of the Universe (EMU) survey. LMC is an extre mely promising target for WIMP searches at radio frequencies because of th e large J-factor and the presence of a substantial magnetic field. We det ect no evidence for emission arising from WIMP annihilations and derive st ringent bounds. This analysis excludes the thermal cross section for mass es below 480 GeV and annihilation into quarks\, setting one of the most st ringent bounds on WIMPs from indirect searches.\n\nhttps://indico.ific.uv. es/event/6178/contributions/15807/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15807/ END:VEVENT BEGIN:VEVENT SUMMARY:Antimatter Cosmic-Ray Nuclei and Dark Matter DTSTART;VALUE=DATE-TIME:20210901T151000Z DTEND;VALUE=DATE-TIME:20210901T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15804@indico.ific.uv.es DESCRIPTION:Speakers: Ilias Cholis (Oakland University)\nAntimatter cosmic -ray measurements can advance our understanding of high-energy astrophysic al phenomena in our own Galaxy. Over the last years\, satellite experiment s as the Alpha Magnetic Spectrometer on board the International Space Stat ion measure antimatter cosmic ray fluxes\, including antiprotons and recen tly antimatter nuclei. These measurements provide a novel probe to search for new physics including annihilations of dark matter in the Milky Way. I will discuss recent studies of the cosmic-ray antiproton-to-proton ratio that have identified an excess of ∼10–20 GeV antiprotons relative to t he predictions of standard astrophysical models. Intriguingly\, the proper ties of this excess are consistent with the same range of dark matter mode ls that can account for the long-standing excess of γ-rays observed from the Galactic Center. Such dark matter candidates can also produce signific ant fluxes of anti-deuterium and anti-helium nuclei \, which I will also p resent.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15804/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15804/ END:VEVENT BEGIN:VEVENT SUMMARY:Light Collection for the Scintillating Bubble Chamber (SBC) DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16019@indico.ific.uv.es DESCRIPTION:Speakers: Hector Hawley Herrera (Queen's University)\nThe ongo ing search for dark matter continues to evolve\, and the quest to reach lo wer cross-sections is leading to novel techniques. A novel low-background technology for the detection of low energy nuclear recoils involves the us e of a bubble chamber which employs noble elements (such as argon and xeno n) as the active mass to collect additional scintillation data simultaneou sly. With recent developments in bubble chambers and the added scintillati on channel\, the scintillating bubble chamber (SBC) collaboration plans to achieve a threshold as low as 100eV and a projected WIMP-sensitivity of 3 .0x10-43 cm2\, for a WIMP mass of 0.7 GeV/c2. SBC is currently constructin g a 10-liter LAr spiked with 100 ppm of LXe chamber at Fermilab with opera tion scheduled to start mid-2022. One of the most important tasks is to ma ximize light collection which requires the characterization of 32 Hamamats u VUV4 SiPMs (silicon photomultipliers). The characterization includes the dark noise rate\, photo detection efficiency\, and crosstalk as a functio n of temperature and breakdown voltage. This talk will focus on the scinti llation collection system\, the current progress of the off-situ character ization of the SiPM array\, and preliminary results.\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/16019/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16019/ END:VEVENT BEGIN:VEVENT SUMMARY:The MIGDAL experiment : Towards observation and measurement of the Migdal effect to help low mass WIMPs searches DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15922@indico.ific.uv.es DESCRIPTION:Speakers: Pawel Majewski (STFC/Rutherford Appleton Laboratory) \nThe Migdal in Galactic Dark mAtter expLoration (MIGDAL) experiment aims to make the first observation of the Migdal effect from fast neutron scatt ering using intense DT and DD generators\, allowing the effect to be inves tigated over a wide range of nuclear recoil energies.\nThe experiment will use an Optical Time Projection Chamber equipped with glass-GEMs operating in 50-Torr CF4 based gas mixture \, with light and change readout provide d by a CMOS camera\, a photomultiplier tube\, and a 120 strip anode. This will allow precise three-dimensional reconstruction of the ionization trac ks from electron and nuclear recoils. \nA Migdal event will be identified by two ionization tracks sharing the same vertex\, one belonging to a nucl ear recoil and the other to a Migdal electron. Low pressure gas will enab le the reconstruction of low energy tracks of electrons down to energies o f 5 keV. \nWe will present the simulations of the events from electrons a nd nuclear recoils and report on the status of construction of the experim ent at the Neutron Irradiation Laboratory for Electronics (NILE) of the Ru therford Appleton Laboratory\, UK.\n\nhttps://indico.ific.uv.es/event/6178 /contributions/15922/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15922/ END:VEVENT BEGIN:VEVENT SUMMARY:Reaching the neutrino floor for sub-GeV dark matter with spherical proportional counters fully electroformed underground DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15918@indico.ific.uv.es DESCRIPTION:Speakers: Kostas Nikolopoulos (University of Birmingham)\nThe NEWS-G collaboration has demonstrated the ability to competitively search for light Dark Matter (DM) using spherical proportional counters. SNOGLOBE \, the current 1.4 m in diameter detector\, was constructed with 99.99% pu re copper (C10100). A 500μm ultra-pure copper layer was electroplated to the detector’s inner surface to further suppress backgrounds. Building o n this experience\, the collaboration is now undertaking the underground c onstruction of entire detectors for unparalleled radiopurity. ECUME\, a 1. 4 m in diameter detector\, will be fully electroformed (EF) in SNOLAB\, su ppressing both Pb-210 contamination and cosmogenic activation. The constru ction of a 30 cm in diameter scale model at PNLL will begin imminently\, w hile the construction of ECUME is expected to begin later in 2021. The pro totype construction\, design and physics potential of ECUME will be discus sed. Furthermore\, the physics potential of DarkSPHERE\, a 3 m in diameter spherical proportional counter currently at the conceptual design stage\, will be presented. An improved shielding is foreseen for this detector to reduce external backgrounds to a level matching that of EF copper. New de velopments in the read-out technology will facilitate operation at higher pressure and potentially provide track reconstruction capabilities. These improvements\, along with the increased detector volume\, operating pressu re\, and use of light (H\, He\, C) gas targets\, will enable sensitivity d own to the neutrino floor in the sub-GeV DM mass range.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15918/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15918/ END:VEVENT BEGIN:VEVENT SUMMARY:The Search for Light Dark Matter with the NEWS-G Detector DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15905@indico.ific.uv.es DESCRIPTION:Speakers: Daniel Durnford (University of Alberta)\nThe NEWS-G direct dark matter search experiment uses spherical proportional counters (SPC) with light noble gases to explore low WIMP masses. The first results obtained with an SPC prototype operated with Ne gas at the Laboratoire So uterrain de Modane (LSM) have already set competitive results for low-mass WIMPs. The forthcoming next phase of the experiment consists of a large 1 40 cm diameter SPC installed at SNOLAB with a new sensor design\, lots of improvements in detector performance and data quality. Before its installa tion at SNOLAB\, the detector was commissioned with pure methane gas at th e LSM\, with a temporary water shield\, offering a hydrogen-rich target an d reduced backgrounds. After giving an overview of the several improvement s of the detector\, preliminary results of this campaign will be presented \, including UV laser and Ar-37 calibration data.\n\nhttps://indico.ific.u v.es/event/6178/contributions/15905/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15905/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent status and prospects of CDEX at China Jinping Underground L aboratory DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15871@indico.ific.uv.es DESCRIPTION:Speakers: Litao Yang (Tsinghua University)\nThe CDEX program p ursues the direct detection of light dark matter candidates with an array of germanium detectors since 2009 at the deepest operating underground sit e located in Sichuan\, China. Searches of modulation effect of light WIMPs [1]\, WIMPs-nucleus interaction via Midgal effect [2]\, dark photon model [3]\, solar axions and axion-like particles [4] as well as the effective- Field-theory-involved interactions [5] have been recently carried out base d on the CDEX-1 and CDEX-10 experiments. An upgraded dark matter experimen t of the CDEX-50dm is proposed and on-going together with the R&D programs on the key low radioactivity technologies including electroformed copper at the underground site\, fabrication and the extra-low-background front-e nds of the various germanium detector types\, operations of a germanium de tector with its bare crystal immersed in liquid nitrogen\, possible hybrid Anti-Compton detectors of the mixed PEN and liquid/solid argon as well as radon mitigation of a 1725 meter cube liquid nitrogen tank. Results and t he prospects of the CDEX dark matter program will be described and discuss ed.\n\n1. L. T. Yang et al.\, (CDEX Collaboration) Light WIMPs Search by A nnual Modulation Analysis with a Point-Contact Germanium Detector at the C hina Jinping Underground Laboratory\, Phys. Rev. Lett. 123\, 221301 (2019) \n2. Z. Z. Liu et al.\, (CDEX Collaboration) Constraints on spin-independ ent nucleus scattering with sub-GeV WIMP dark matter from the CDEX-1B Expe riment at CJPL\, Phys. Rev. Lett. 123 161301 (2019)\n3. Z. She et al.\, (C DEX Collaboration) “Direct Detection Constraints on Dark Photons with CD EX-10 Experiment at the China Jinping Underground Laboratory” Phys. Rev. Lett. 124\, 111301 (2020)\n4. Y. Wang et al. (CDEX Collaboration) “Impr oved limits on solar axions and bosonic dark matter from the CDEX-1B exper iment using profile likelihood ratio method” Phys. Rev. D 101\, 052003 ( 2020)\n5. Y. Wang et al.\, (CDEX Collaboration)\, First experimental const raints on WIMP couplings in the effective field theory framework from CDEX \, Sci. China-Phys. Mech. Astron. 64\, 281011 (2021)\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/15871/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15871/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct Dark Matter search with CRESST-III Experiment DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15860@indico.ific.uv.es DESCRIPTION:Speakers: Lucia Canonica (Max Planck Institut for Physics)\nCR ESST (Cryogenic Rare Event Search with Superconducting Thermometers ) is a direct dark matter search experiment located at the Gran Sasso Underground Laboratory (Italy) that uses scintillating cryogen ic calorimeters as target material for elastic DM-nucleus scattering. The current phase of the experiment\, CRESST-III\, is optimized for low-energy nuclear recoil detection. It has reached an unprecedented val ue of 30 eV for nuclear recoil energy thresholds on a CaWO_4 target\, allo wing the exploration of low-mass dark matter candidates down to 0.16 GeV/c ^{2}. At higher masses the sensitivity is currently limited by a rising ev ent rate (from threshold up to few hundreds of eV) from a so-far unknown o rigin. Currently dedicated measurements with upgraded detectors — includ ing different target materials — are being performed at the Gran Sasso U nderground Laboratory\, with the goal of investigating and identifying the origin of the event excess. In this contribution\, the current stage of t he CRESST-III experiment\, together with the most recent dark matter res ults\, will be presented. The potential of the current data taki ng phase and the sensitivity projections of the next phase of the exper iment will be also discussed.\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15860/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15860/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter search with a SuperCDMS low-threshold silicon device DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15859@indico.ific.uv.es DESCRIPTION:Speakers: Valentina Novati (Northwestern University)\nThe Supe r Cryogenic Dark Matter Search (SuperCDMS) experiment uses high-sensitivit y silicon and germanium detectors to directly search for interactions from galactic dark matter (DM). New 1-gram silicon devices instrumented with u ltra-high-resolution phonon sensors can be operated both with no electrica l bias in the crystal\, measuring the recoil energy\, and with an applied electric field\, which amplifies the recoil events through the Neganov-Tro fimov-Luke effect. In this talk\, I will present results from a new search for sub-GeV DM candidates using a modest 0.19 gram-day exposure\, acquire d with a device characterized by a 9.2 eV trigger threshold. I will also p resent a study of an unexpected low-energy event excess observed in the si licon device\, comparing 0V data to a high voltage data set acquired with the same device. The observed excess is consistent with a Cherenkov/scinti llation hypothesis and we expect to be able to mitigate it significantly f or the next science campaign\, extending the sensitivity to low-mass DM.\n \nhttps://indico.ific.uv.es/event/6178/contributions/15859/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15859/ END:VEVENT BEGIN:VEVENT SUMMARY:WIMP dark matter searches with CDEX and TEXONO experiments DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15857@indico.ific.uv.es DESCRIPTION:Speakers: Hau-Bin Li (Institute of Physics\, Academia Sinica\, Taipei)\nWe present results on light weakly interacting massive particle (WIMP) searches with time-integrated (TI) and annual modulation (AM) analy sis on data from a 1-kg mass p-type point-contact germanium detector of th e CDEX-1B experiment at the China Jinping Underground Laboratory. Limits f rom WIMP-nucleus with Migdal effect and WIMP-electrons interactions with e arth scattering correction will be discussed. We also present results from spin-independent WIMP-nucleus scattering of TEXONO experiment at earth's surface\, which is able to explore parameters space that is blind to under ground experiment due to earth scattering.\n\nhttps://indico.ific.uv.es/ev ent/6178/contributions/15857/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15857/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of the DAMIC-M dark matter experiment DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15834@indico.ific.uv.es DESCRIPTION:Speakers: Danielle Norcini (University of Chicago/KICP)\nDAMIC -M is a low-energy threshold dark matter experiment using skipper charge-c oupled devices (skipper CCDs) at the Laboratoire Souterrain de Modane (LSM ) in France. The kg-scale detector is designed to search for both nuclear and electronic recoils from low-mass WIMP and hidden photon scatters on si licon within the large CCD array. The skipper amplifier readout allows for several non-destructive measurements of individual pixel charge\, reducin g the detection resolution to single electrons and thus pushing the energy threshold to the eV-scale. We will report the status of the DAMIC-M exper iment\, including results of recent CCD performance and calibration studie s.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15834/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15834/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct search for low mass dark matter with DarkSide-LowMass DTSTART;VALUE=DATE-TIME:20210901T154000Z DTEND;VALUE=DATE-TIME:20210901T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15821@indico.ific.uv.es DESCRIPTION:Speakers: Shawn Westerdale (INFN Cagliari)\nDarkSide-LowMass i s a tonne-scale liquid argon time projection chamber being planned by the Global Argon Dark Matter Collaboration (GADMC) to search for WIMP-like dar k matter with masses below 10 GeV/c^2\, achieving low thresholds with a de sign optimized for an electron-counting analysis. Building upon the succes s of DarkSide-50's light dark matter search\, DarkSide-LowMass will aim to achieve sensitivity to the solar neutrino floor with a tonne-year exposur e. This talk will present sensitivity projections for the DarkSide-LowMass experiment\, based on simulations of expected backgrounds.\n\nhttps://ind ico.ific.uv.es/event/6178/contributions/15821/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15821/ END:VEVENT BEGIN:VEVENT SUMMARY:Improving the sensitivity to light dark matter with the Migdal eff ect DTSTART;VALUE=DATE-TIME:20210901T152500Z DTEND;VALUE=DATE-TIME:20210901T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15814@indico.ific.uv.es DESCRIPTION:Speakers: Grilli di Cortona Giovanni (INFN - Laboratori Nazion ali di Frascati)\nThe search for dark matter (DM) weakly interacting massi ve particles with noble elements has probed masses down and below a GeV/c^ 2. The ultimate limit is represented by the experimental threshold on the energy transfer to the nuclear recoil. Currently\, the experimental sensit ivity has reached a threshold equivalent to a few ionization electrons. In these conditions\, the contribution of a Bremsstrahlung photon or a so-ca lled Migdal electron due to the sudden acceleration of a nucleus after a c ollision might be sizeable. We present a recent work where\, using a Bayes ian approach\, we studied how these effects can be exploited in experiment s based on liquid argon detectors. In particular we develop a simulated ex periment to show how the Migdal electron and the Bremsstrahlung photon all ow to push the experimental sensitivity down to masses of 0.1 GeV/c^2\, ex tending the search region for dark matter particles of previous results. F or these masses we estimate the effect of the Earth shielding that\, for s trongly interacting dark matter\, makes any detector blind. Finally\, give n the relevance of the Migdal electrons to the search for low mass DM\, we discuss some new ideas on how to possibly measure such an effect with det ectors based on a Time Projection Chamber exposed to an high neutron flux. \n\nhttps://indico.ific.uv.es/event/6178/contributions/15814/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15814/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter search results from DAMIC at SNOLAB DTSTART;VALUE=DATE-TIME:20210901T151000Z DTEND;VALUE=DATE-TIME:20210901T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15813@indico.ific.uv.es DESCRIPTION:Speakers: Romain Gaior (LPNHE\, Sorbonne Université)\nThe DAM IC experiment employs large area\, thick charge-coupled devices (CCDs) to search for the interactions of low-mass dark matter (DM) particles in the galactic halo with silicon atoms in the CCD target. The low pixel noise pr ovides DAMIC with sensitivity to ionization signals of only a few charges\ , for a remarkably low energy threshold. From 2017 to 2019\, DAMIC collect ed dark-matter search data with a seven-CCD array (40-gram target) install ed in a low radiation environment in the SNOLAB underground laboratory. Re sults include the search for hidden-sector DM particles with masses as sma ll as a few MeV/$c^2$ from their scattering with electrons. Recently\, we performed a search for nuclear recoils from the scattering of WIMPs with G eV/c$^2$-scale masses in a 11 kg day exposure (PRL 125 241803). Our result stands out compared to other experimental searches for low-mass WIMPs bec ause the response to the WIMP signal has been directly calibrated (PRD 94 082007). We probe with the same nuclear target parameter space that corres ponds to the WIMP-signal interpretation of the CDMS anomaly (PRL 111 25130 1)\, and report a conspicuous excess of events below 200 eV$_{\\rm ee}$.\n \nhttps://indico.ific.uv.es/event/6178/contributions/15813/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15813/ END:VEVENT BEGIN:VEVENT SUMMARY:The simplest scoto-seesaw model: WIMP dark matter phenomenology an d Higgs vacuum stability DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15911@indico.ific.uv.es DESCRIPTION:Speakers: Sanjoy Mandal (IFIC (CSIC-Univ Valencia))\nWe have e xamined the consistency of electroweak breaking\, neutrino and dark matter phenomenology within the minimal scoto-seesaw mechanism. The model provid es a simple picture where the ''atmospheric'' mass scale arises from the t ree-level ''missing partner'' seesaw\, while the ``solar'' scale is induce d radiatively by the dark sector\, hence neutrino mass generation is intim ately connected with dark matter. The model can have both fermionic or sca lar dark matter candidate. We have studied various prospects such as reli c abundance\, direct detection and indirect detection for scalar dark matt er case. In addition we have studied the issue of vacuum stability and for this purpose we have derived the full two-loop RGEs for the relevant para meters\, such as the quartic Higgs self-coupling $\\lambda$ of the Standar d Model. The new scalars present in the scoto-seesaw mechanism improve the stability properties of the electroweak vacuum. We have also explored the consistency of the underlying dark symmetry.\n\nhttps://indico.ific.uv.es /event/6178/contributions/15911/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15911/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for pseudo-Nambu-Goldstone boson dark matter production in association with top quarks DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15901@indico.ific.uv.es DESCRIPTION:Speakers: Stefan Schulte (Max Planck Institute for Physics (Mu nich))\nPseudo-Nambu-Goldstone bosons (pNGBs) are attractive dark matter ( DM) candidates since they are coupled to the Standard Model (SM) predomina ntly through derivative interactions. Thereby\, they naturally evade the s trong existing limits inferred from DM direct detection experiments. Worki ng in an effective field theory that includes both derivative and non-deri vative DM-SM operators\, we perform a detailed phenomenological study of t he Large Hadron Collider reach for pNGB DM production in association with top quarks. Drawing on motivated benchmark scenarios as examples\, we comp are our results to other collider limits as well as the constraints impose d by DM (in)direct detection experiments and the relic abundance. Furtherm ore\, we explore implications on the viable parameter space of pNGB DM. In particular\, we demonstrate that the sensitivity of DM direct detection e xperiments can be achieved via loop-induced interactions. The search strat egies we discuss can serve as a starting point for dedicated experimental analyses by the ATLAS and CMS collaborations.\n\nhttps://indico.ific.uv.es /event/6178/contributions/15901/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15901/ END:VEVENT BEGIN:VEVENT SUMMARY:Thermal WIMPs and the scale of new physics DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15867@indico.ific.uv.es DESCRIPTION:Speakers: Felix Kahlhoefer (RWTH Aachen University)\nThe non-o bservation of conclusive dark matter signals raises the question whether W IMPs can still account for the dark matter of the universe. In this talk I will present results from a global analysis of effective field theory ope rators describing the interactions between WIMPs and Standard Model partic les. In this bottom-up approach\, the global fitting framework GAMBIT is u sed to simultaneously vary the coefficients of 14 such operators\, along w ith the WIMP mass\, the scale of new physics and several nuisance paramete rs. The likelihood functions include the latest data from Planck\, direct and indirect detection experiments\, and the LHC. Although the observed re lic density can be reproduced in large regions of parameter space\, there cannot be a large hierarchy between the dark matter mass and the scale of new physics\, which raises concerns about the validity of the effective fi eld theory. I will discuss possible ways to address this issue in order to consistently interpret the latest results from WIMP searches at the LHC.\ n\nhttps://indico.ific.uv.es/event/6178/contributions/15867/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15867/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter from a complex scalar singlet: The role of dark CP and other discrete symmetries DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15866@indico.ific.uv.es DESCRIPTION:Speakers: Carlos Faubel (IFIC (CSIC-Univ Valencia))\nIn this t alk I will study the case where dark matter emerges from a complex scalar field charged under a U(1) global symmetry\, which is spontaneously broken . Our analysis considers different explicit symmetry breaking terms motiva ted by discrete symmetries. I will show results which demonstrate that in some regions of the parameter space these scenarios may be distinguished b y combining different observables\, such as direct detection and collider signatures. Finally we discuss the case where the stabilising symmetry may be broken\, as well as an effective operator approach valid in the pseudo -Nambu-Goldstone limit.\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15866/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15866/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter in a charged variant of the Scotogenic model DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15853@indico.ific.uv.es DESCRIPTION:Speakers: Miguel Puerta (IFIC (CSIC-Univ Valencia))\nScotogen ic models are among the most popular possibilities to link dark matter\nan d neutrino masses. In this work we discuss a variant of the Scotogenic mod el\nthat includes charged fermions and a doublet with hypercharge 3/2. Neu trino\nmasses are induced at the one-loop level thanks to the states belon ging to the dark sector. However\, in contrast to the standard Scotogenic model\, only the scalar dark matter candidate is viable in this version. A fter presenting the model and explaining some particularities about neutri no mass generation\, we concentrate on its dark matter phenomenology. We s how that the observed dark matter relic density can be correctly reproduce d in the usual parameter space regions found for the standard Scotogenic m odel or the Inert Doublet model. In addition\, the presence of the charged fermions may open up new regions\, provided some tuning of the parameters is allowed.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15853/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15853/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing light dark scalars with future laboratory experiments DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15825@indico.ific.uv.es DESCRIPTION:Speakers: Marco Taoso (INFN Torino)\nWe investigate a dark sec tor containing a pair of light non-degenerate scalar particles\, with mass es in the MeV-GeV range\, coupled to the visibile sector through heavier m ediators. The heaviest dark state is long-lived\, and its decays offer ne w testable signals. We analyze the prospects for detection with the propos ed beam-dump facility SHiP\, and the proposed LHC experiments FASER and MA THUSLA. Moreover\, we consider bounds from the beam-dump experiment CHARM and from colliders (LEP\, LHC and BaBar). We present our results both in terms of an effective field theory\, where the heavy mediators have been i ntegrated out\, and of a simplified model containing a vector boson m ediator\, which can be heavy O(1) TeV\, or light O(10) GeV. We sh ow that future experiments can test large portions of the paramet er space currently unexplored\, and that they are complementary to future High-Luminosity LHC searches.\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15825/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15825/ END:VEVENT BEGIN:VEVENT SUMMARY:Studying dark matter with MadDM: Lines and loops DTSTART;VALUE=DATE-TIME:20210831T154000Z DTEND;VALUE=DATE-TIME:20210831T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15810@indico.ific.uv.es DESCRIPTION:Speakers: Daniele Massaro (Dipartimento di Fisica e Astronomia (DIFA)\, Alma Mater Studiorum - Università di Bologna\; Centre for Cosmo logy\, Particle Physics and Phenomenology (CP3)\, Université catholique d e Louvain)\nAutomated tools for the computation of amplitudes and cross se ctions have become the backbone of phenomenological studies beyond the sta ndard model. We present the latest developments in MadDM\, a calculator of dark-matter observables based on MadGraph5_aMC@NLO. The new version enabl es the fully automated computation of loop-induced annihilation processes\ , relevant for indirect detection of dark matter. Of particular interest i s the electroweak annihilation into $\\gamma X$\, where $X=\\gamma$\, $Z$\ , $h$ or any new unstable particle even under the dark symmetry. These pro cesses lead to the sharp spectral feature of monochromatic gamma lines: a smoking-gun signature for dark matter annihilation in our Galaxy. MadDM pr ovides the predictions for the respective fluxes near Earth and derives co nstraints from the gamma-ray line searches by Fermi-LAT and HESS. As an ap plication\, we present the implications for the parameter space of the Ine rt Doublet model and a top-philic $t$-channel mediator model.\n\nhttps://i ndico.ific.uv.es/event/6178/contributions/15810/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15810/ END:VEVENT BEGIN:VEVENT SUMMARY:Supernova constraints on dark flavoured sectors DTSTART;VALUE=DATE-TIME:20210831T152500Z DTEND;VALUE=DATE-TIME:20210831T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15800@indico.ific.uv.es DESCRIPTION:Speakers: Jorge Terol Calvo (Instituo de Astrofísica de Canar ias (IAC))\nI will present a recent application of the SN 1987A cooling bo und to set a constraint on dark flavoured sectors. This is possible thanks to the fact that the protoneutron stars are hot and dense environments wh ere hyperons can be efficiently produced. Therefore a decay of the form $ Λ→nX^0$\, where $X^0$ is a new bosonic dark particle\, will be severely constrained. I will explain the ingredients required and the application to flavoured (massless) dark photons\, axions and ALPs.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15800/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15800/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter freeze-in from semi-production DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15791@indico.ific.uv.es DESCRIPTION:Speakers: Maxim Laletin (NCBJ)\nWe study a novel dark matter p roduction mechanism based on the freeze-in through semi-production\, i.e. the inverse semi-annihilation processes. A peculiar feature of this scenar io is that the production rate is suppressed by a small initial abundance of dark matter and consequently creating the observed abundance requires m uch larger coupling values than for the usual freeze-in. We provide a conc rete example model exhibiting such production mechanism and study it in de tail\, extending the standard formalism to include the evolution of dark m atter temperature alongside its number density and discuss the importance of this improved treatment. Finally\, we confront the relic density constr aint with the limits and prospects for the dark matter indirect detection searches. We show that\, even if it was never in full thermal equilibrium in the early Universe\, dark matter could\, nevertheless\, have strong eno ugh present-day annihilation cross section to lead to observable signals.\ n\nhttps://indico.ific.uv.es/event/6178/contributions/15791/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15791/ END:VEVENT BEGIN:VEVENT SUMMARY:MADMAX: A QCD Dark Matter Axion Direct-Detection Experiment DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15889@indico.ific.uv.es DESCRIPTION:Speakers: Chang Lee (MPI for Physics)\nAxions emerge naturally from the Peccei-Quinn (PQ) mechanism which addresses the absence of CP vi olation in the strong interaction\, and they can make up the cold dark mat ter in the universe. If PQ symmetry breaking had occurred after inflation\ , the axion mass would likely range from ∼ 40 μeV to ∼ 1 meV\, w hich is yet to be explored experimentally.\n\nThe MAgnetized Disc And Mirr or Axion eXperiment is designed to reach sensitivity in the axion mass ran ge of 40 to 400 µeV\, a range inaccessible by previous axion experiments. This is reached by applying the dielectric haloscope approach\, exploitin g the axion to photon conversion at dielectric surfaces within a strong ma gnetic field. For MADMAX a system of  movable dielectric discs  inside a n approximately 9 T magnetic field is foreseen.\n\nThe design\, realizatio n and timescale of MADMAX will be discussed along with prospects of the MA DMAX prototype as well as first proofs of concept guiding the way towards the final experiment and the first physics run.\n\nhttps://indico.ific.uv. es/event/6178/contributions/15889/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15889/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraining the diffuse supernova axion-like-particle background with high-latitude Fermi-LAT data DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15888@indico.ific.uv.es DESCRIPTION:Speakers: Christopher Eckner (CNRS/LAPTh)\nCore-collapse super novae (SNe) have been identified as a promising target to probe the existe nce of axion-like-particles (ALPs). The cumulative signal from all past SN e events would contain an ALP component and create a diffuse flux with ene rgies $\\mathcal{O}(50)$ MeV. We update the calculation of this flux by in cluding SNe with different masses following the expected mass distribution \, instead of using the spectrum obtained by using a single reference mass . Due to their coupling to photons and the related Primakoff process\, the diffuse SNe ALP flux is converted into a diffuse gamma-ray flux while tra versing the magnetic field of the Milky Way. The spatial morphology of thi s signal is expected to follow the shape of the Galactic magnetic field li nes.\nWe perform a template-based analysis to constrain the ALP parameter space via the spatial structure of this ALP-induced diffuse gamma-ray flux using Fermi-LAT data from 12 years and an energy range from 50 MeV to 500 GeV. We find an improvement of the upper limit on the ALP-photon coupling constant $g_{a\\gamma}$ about an order of magnitude compared to a previou s analysis solely based on the spectral shape of the signal. Our results a re robust against variations in the modelling of high-latitude Galactic di ffuse emission and systematic uncertainties of the LAT.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15888/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15888/ END:VEVENT BEGIN:VEVENT SUMMARY:Ultralight dark matter searches with KAGRA gravitational wave tele scope DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15882@indico.ific.uv.es DESCRIPTION:Speakers: Yuta Michimura (Department of Physics\, University o f Tokyo)\nAmong various dark matter candidates\, bosonic ultralight fields with masses below 1 eV are well motivated by cosmology because they behav e as classical wave fields\, rather than individual particles. Recently\, a number of novel ideas have been proposed to search for ultralight dark m atter candidates using laser interferometers at various scales. Those incl ude our proposals to search for axion-like particles (ALPs) and vector fie lds with laser interferometric gravitational wave detectors. ALPs can be s earched for by measuring the oscillating polarization rotation of laser be am. Massive vector field weakly coupled to the standard model sector can a lso be searched for by measuring the oscillating forces acting on the susp ended mirrors of the interferometers. Within the KAGRA collaboration\, the analysis of data from the KAGRA's observing run in 2020 to search for vec tor dark matter\, and the installation of polarization optics to the arm c avity transmission ports of the interferometer to search for ALPs are unde rway. In this talk\, we will report the status of such efforts to search f or ultralight dark matter with KAGRA gravitational wave telescope.\n\nhttp s://indico.ific.uv.es/event/6178/contributions/15882/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15882/ END:VEVENT BEGIN:VEVENT SUMMARY:A Novel Search Technique for Ultralight Dark Matter Using Green Ba nk Telescope Data DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15880@indico.ific.uv.es DESCRIPTION:Speakers: Aya Keller (UC Berkeley)\nMost of the matter in the universe is widely thought to be non-baryonic and composed of unknown suba tomic particles referred to as dark matter. While significant attention ha s been paid to a few specific candidates such as the WIMP and axion\, in f act the nature and mass of dark matter is poorly constrained\, and thus a broad observational approach may yield useful clues for its ultimate detec tion. We have developed a novel approach which utilizes the recent Breakth rough Listen public data release of three years of observation with the Gr een Bank Telescope to execute a broad search for an axion signal across bi llions of independent frequency channels simultaneously. This method is mo del-independent and only assumes that there is a decay or annihilation of virialized dark matter leading to a quasi-monochromatic radio line\, and a dditionally that the line exhibits a Doppler shift with position according to the solar motion through a static galactic halo. This approach has bee n tested on a subset of L-band data\, and the analysis of the full L-\, S- \, C- and X-band dataset (25\,000 spectra\, 1.1–11.6 GHz) is currently u nderway. This work was supported by a grant from the Heising-Simons Founda tion.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15880/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15880/ END:VEVENT BEGIN:VEVENT SUMMARY:First observation and analysis of DANCE: Dark matter Axion search with riNg Cavity Experiment DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15865@indico.ific.uv.es DESCRIPTION:Speakers: Yuka Oshima (Department of Physics\, University of T okyo)\nDark matter Axion search with riNg Cavity Experiment (DANCE) was pr oposed. To search for axion-like dark matter\, we aim to detect the rotati on and oscillation of optical linear polarization caused by axion-photon c oupling with a bow-tie ring cavity. DANCE can improve the sensitivity to t he axion-photon coupling constant for axion mass $\n\nhttps://indico.ific. uv.es/event/6178/contributions/15865/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15865/ END:VEVENT BEGIN:VEVENT SUMMARY:Using cryogenic Penning trap LC detection circuits to search for a xion-like dark matter. DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15848@indico.ific.uv.es DESCRIPTION:Speakers: Jack Devlin (CERN)\nWe present recent limits set by the BASE collaboration on the coupling between any dark matter axion-like particles (ALPs) and photons\, measured using the superconducting resonant single particle detection circuit of a cryogenic Penning trap. To search for ALPs\, we investigated the noise spectrum of our fixed-frequency reson ant circuit for peaks caused by axion-to-photon conversion in the strong m agnetic field of the Penning trap magnet. Uniquely\, we used a single anti proton interacting with our detection circuit to measure the detector nois e temperature. Our analysis constrained the coupling of ALPs with masses a round 2.7906-2.7914 neV/c$^{2}$ to photons to be $g_{a\\gamma}2000 times b roader mass range at improved sensitivity.\n\nhttps://indico.ific.uv.es/ev ent/6178/contributions/15848/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15848/ END:VEVENT BEGIN:VEVENT SUMMARY:Beyond the Standard Model Searches with the MAJORANA DEMONSTRATOR Experiment DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15827@indico.ific.uv.es DESCRIPTION:Speakers: Wenqin Xu (University of South Dakota)\nThe MAJORANA DEMONSTRATOR experiment operated two modular arrays of p-type point conta ct high purity germanium (HPGe) detectors\, of which 30 kg is enriched to 88% in Ge-76\, to search for neutrinoless double beta decay. The data-taki ng campaign for double beta decay with enriched detectors was successfully concluded in March 2021\, and data-taking with natural detectors is still ongoing. The DEMONSTRATOR has achieved excellent energy performance in a wide dynamic range covering 1 keV to 10 MeV. The extra-low background leve l and excellent energy performance achieved by the DEMONSTRATOR makes it c ompetitive in various searches of physics beyond the Standard Model. \n\nI f there is an axion-photon coupling\, axions can be produced by the Primak off conversion of photons in the Sun. Solar axions can inversely generate photon signals in germanium crystals\, which can be coherently enhanced wh en the Bragg condition is satisfied. The DEMONSTRATOR is searching for sol ar axions with a novel method to correlate and leverage its high number of HPGe detectors. In this talk\, we will discuss the status and results of recent searches for new physics with the DEMONSTRATOR\, including the firs t reporting of a solar axion search.\n\nhttps://indico.ific.uv.es/event/61 78/contributions/15827/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15827/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching For Axion Dark Matter with the South Pole Telescope DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15801@indico.ific.uv.es DESCRIPTION:Speakers: Kyle Ferguson (UCLA)\nAxions and other axion-like pa rticles (ALPs) remain compelling dark matter candidates with a wealth of p ossible detection methods. A photon traveling through an axion field will experience a rotation in its polarization proportional to the difference in axion field value at photon emission and photon absorption. Thus the a pparent polarization of a static astrophysical source will oscillate in ti me as the local axion dark matter field oscillates (with a frequency propo rtional to the axion mass). The cosmic microwave background (CMB) is pola rized\, well-studied\, and extremely static\, making it an ideal source wi th which to search for this effect. We present the status of such a searc h for ultra-light ALPs with masses roughly between $10^{-21}$ and $10^{-19 }$ eV using data from the South Pole Telescope (SPT)\, a millimeter-band t elescope with arcminute resolution that is located at the geographic South Pole and designed to observe the CMB.\n\nhttps://indico.ific.uv.es/event/ 6178/contributions/15801/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15801/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraints on Axion-like Particles from a Hard X-ray Observation of Betelgeuse DTSTART;VALUE=DATE-TIME:20210831T154000Z DTEND;VALUE=DATE-TIME:20210831T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15793@indico.ific.uv.es DESCRIPTION:Speakers: Mengjiao Xiao (MIT)\nAxion-like particles (ALPs) can be produced in stellar plasmas via the Primakoff process due to the photo n-ALP coupling. Light ALPs produced in this way can easily escape the star and reconvert back into photons in the Galactic magnetic field. Betelgeus e (α-Orionis\, spectral type M2Iab)\, a nearby red supergiant star\, prov ides an excellent laboratory for ALP searches\, as it (i) has a hot core\, and thus is potentially a copious producer of ALPs that\, after re-conver sion\, produces a photon signal peaked in the hard X-ray (E>10 keV) range\ , (ii) is in region of Hertzsprung-Russel diagram where no stable corona i s expected\, and thus has essentially zero standard astrophysical X-ray ba ckground\, and (iii) is nearby\, at a distance d~200 pc\, and thus in a re gion of the local magnetic field that is relatively easier to constrain wi th future observations.\nWe use the first observation of Betelgeuse in har d X-rays to perform a novel search for ALPs. With a 50 ks observation by t he NuSTAR satellite telescope\, we find no significant excess of events ab ove the expected background and set a stringent upper limit on the ALP-pho ton coupling. In this contribution\, I will detail this work while focusin g on the data analysis\, results and impact\, and emphasizing the uncertai nty introduced by the stellar evolution model and the Galactic magnetic fi eld.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15793/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15793/ END:VEVENT BEGIN:VEVENT SUMMARY:Axion-Photon Conversion in Magnetospheres: The Role of the Plasma DTSTART;VALUE=DATE-TIME:20210831T152500Z DTEND;VALUE=DATE-TIME:20210831T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15789@indico.ific.uv.es DESCRIPTION:Speakers: Samuel Witte (GRAPPA Institute\, Univ Amsterdam)\nTh e most promising indirect search for the existence of axion dark matter us es radio telescopes to look for narrow spectral lines generated in the mag netospheres of neutron stars. Unfortunately\, a large list of theoretical uncertainties has prevented this search strategy from being accepted as ro bust. In this talk I will present a novel end-to-end pipeline that traces individual photon trajectories from their point of genesis in the magnetos phere to asymptotic distances. This method allows one assess many of the o utstanding uncertainties\, including: (1) do refraction and reflection ind uce strong inhomogeneous features in the flux\, (2) can refraction induce premature axion-photon de-phasing\, (3) what is the expected width of the line\, (4) does the flux have a strong time-dependence\, and (5) can these radio photons be efficiently absorbed.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15789/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15789/ END:VEVENT BEGIN:VEVENT SUMMARY:Axion Quasiparticles for Axion Dark Matter Detection DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15787@indico.ific.uv.es DESCRIPTION:Speakers: Jan Schütte-Engel (University of Illinois Urbana-Ch ampaign)\nIt has been suggested that certain antiferromagnetic topological insulators contain axion quasiparticles (AQs)\, and that such materials c ould be used to detect axion dark matter (DM). In the first part of this t alk we show that one can detect AQs with transmission spectroscopy. The tr ansmission coefficients including material losses are computed by applying appropriate boundary conditions. We show that by comparing our signal cal culation to future THz transmission experiments the existence of AQs can b e proven. Furthermore\, the comparison can be used to fully characterize t he material parameters.\nIn the second part of this talk we show that AQs can be used for axion DM detection. The dispersion relation and boundary c onditions permit resonant conversion of axion DM into THz photons. The res onance frequency is tunable with an external B-field. A parameter study fo r axion DM detection is performed\, computing boost amplitudes and bandwid ths using realistic material properties including loss. The proposal could allow for detection of axion DM in the mass range between 1 and 10 meV us ing current and near future technology.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15787/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15787/ END:VEVENT BEGIN:VEVENT SUMMARY:The SABRE South Experiment at the Stawell Underground Physics Labo ratory DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15913@indico.ific.uv.es DESCRIPTION:Speakers: William Dix (Univ Melbourne)\nThe SABRE (Sodium-iodi de with Active Background REjection) experiments aim to detect an annual r ate modulation from dark matter interactions in ultra-high purity NaI(Tl) crystals. The SABRE south experiment is located at the Stawell Underground Physics Laboratory (SUPL)\, Australia\, the first deep underground labora tory in the Southern Hemisphere\, due to be completed in late 2021. SABRE South is designed to disentangle seasonal or site-related effects from the dark matter-like modulated signal first observed by DAMA/LIBRA in the Nor thern Hemisphere. It is a partner to the SABRE North effort at the Gran Sa sso National Laboratory (LNGS).\n\nSABRE South is instrumented with ultra high purity NaI(Tl) crystals immersed in a linear alkyl benzene based liqu id scintillator veto\, further surrounded by passive steel and polyethylen e shielding and a plastic scintillator muon veto. The SABRE South experim ent is under construction\, and will be commissioned from late 2021 to ear ly 2022. In this presentation we will present the final design of SABRE So uth\, the status of its construction\, its expected background\, and its s ensitivity to a DAMA/LIBRA like modulation. We will also present recent qu enching factor measurements of sodium nuclear recoils in NaI(Tl) crystals measured with the ANU Heavy Ion Accelerator Facility\, and a report on the status of SUPL.\n\nhttps://indico.ific.uv.es/event/6178/contributions/159 13/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15913/ END:VEVENT BEGIN:VEVENT SUMMARY:Quenching Factor consistency across several NaI(Tl) crystals DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15893@indico.ific.uv.es DESCRIPTION:Speakers: David Cintas González (Universidad de Zaragoza)\nTe sting the DAMA/LIBRA annual modulation result independently of dark matter particle and halo models has been a challenge for twenty years. Using sam e target material\, NaI(Tl)\, is required and presently two experiments\, ANAIS-112 and COSINE-100\, are running for such a goal. However\, a precis e knowledge of the detector response to nuclear recoils is mandatory becau se this is the channel where the dark matter signal is expected. The emitt ed light is quenched with respect to the gamma-calibrated energy by a fact or that has to be measured experimentally. However\, current quenching fac tor measurements show a disagreement within the energy region of interest for dark matter searches. To disentangle whether this discrepancy is due t o intrinsic differences in the light response among different NaI(Tl) crys tals\, or has its origin in unaccounted for systematic effects will be key in the comparison among the different experiments. We present measurement s of the quenching factors for several small NaI(Tl) crystals performed in the same experimental setup to control systematics. Nuclear recoils were produced by quasi-monoenergetic neutrons\, and triggering was done by the scattered neutron interacting in one of the 17 liquid scintillator backing detectors placed at different angles from the NaI(Tl) crystal. This trigg ering avoids threshold effects that could have affected some of the previo us experimental results. In this talk\, we will present the results of our experiment and a comparison with those available in the literature. We wi ll also analyze their effect on the annual modulation interpretation.\n\nh ttps://indico.ific.uv.es/event/6178/contributions/15893/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15893/ END:VEVENT BEGIN:VEVENT SUMMARY:Skipper CCDs for the search of daily modulation of Dark Matter sig nal in the DMSQUARE experiment DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15891@indico.ific.uv.es DESCRIPTION:Speakers: Nicolás Avalos (CONICET)\nThe Dark Matter Daily Mod ulation experiment (DMSQUARE) seeks for dark matter interactions with a Sk ipper CCD. It is currently running at surface level in Bariloche\, Argenti na\, and will be moved to a shallow underground site at Sierra Grande\, Ar g\, in September 2021. The low threshold achieved by Skipper CCDs allows t o search for electron recoil events with an ionization energy down to 1.2 eV. In order to extract a potential dark matter signal from noise at the s ingle electron level\, we propose to search for a diurnal modulation of ev ents\, resulting from the potential interaction of the dark matter wind th rough the Earth. Depending on the model\, mass and cross-section\, this mo dulation can be maximum at 40deg of latitude in the Southern Hemisphere\, where DMSQUARE is operated. In this talk we will present the experiment\, report preliminary results with Skipper CCDs taking data at surface level and comment on future prospects for the experiment.\n\nhttps://indico.ific .uv.es/event/6178/contributions/15891/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15891/ END:VEVENT BEGIN:VEVENT SUMMARY:Directionality and 3D tracks in the (sub)keV range with the MIMAC detector DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15887@indico.ific.uv.es DESCRIPTION:Speakers: Cyprien Beaufort (LPSC / CNRS)\nThe detection of a d ark matter (DM) particle would deeply contribute to the understanding of t he Universe and would shine light on new Physics. The WIMP is an extensive ly studied DM candidate that would induce nuclear recoils inside a detecto r. The largest direct projects searching for WIMPs will soon reach the “ neutrino floor”\, a boundary beyond which a WIMP signal cannot be distin guished from the irreducible background due to neutrinos. The only known p rinciple to overpass this background is to measure the direction of the in duced recoils and to correlate it with the expected incoming direction of the WIMPs. This is the principle of directional detection. \n\nIn this tal k we will introduce MIMAC\, a directional detector that measures simultane ously the energy of a particle and reconstructs its track in 3D in an adap table energy range [150 eV \, 30 MeV]. MIMAC is a gaseous µ-TPC in which one can adapt the experimental conditions (target mass\, spin\, pressure\, etc.) to particular DM candidates phenomenology.\n\nWe will focus on the study of directionality in the keV-range for which there is a lack of expe rimental data. In this low energy region\, the lengths of the WIMP-induced nuclear recoils lie in the sub-millimeter range. We will show that the di ffusion of the primary electrons\, usually considered as a limiting phenom enon\, improve our directional performances for sub-millimeter tracks! Mea suring low-energy recoils implies to operate at high-gain\, for which many ions are produced in the avalanche process. We have developed SimuMimac\, a simulation tool that investigates the influence of the ions on the sign al formation and the 3D reconstruction. SimuMimac agrees with the measurem ents and shines light on possible deconvolutions of the signal induced by the ions. \n\nLow-energy electrons are of interest to understand the backg round but also\, for instance\, to search for Axion-Like Particles. In thi s talk we will present 3D tracks of electrons down to 150eV. At these ener gies\, only a few primary electrons are generated by the ionization proces s. We will show that MIMAC is sensitive to the fluctuation of the number o f primary electrons and that we can use this phenomenon to determine the g ain per primary electrons.\n\nhttps://indico.ific.uv.es/event/6178/contrib utions/15887/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15887/ END:VEVENT BEGIN:VEVENT SUMMARY:The ASTAROTH Project: enhanced low-energy sensitivity to Dark Matt er annual modulation DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15883@indico.ific.uv.es DESCRIPTION:Speakers: Andrea Zani (INFN Milano)\nASTAROTH is a novel R&D p roject which aims at improving the physics reach of future direct dark mat ter detection experiments based on NaI(Tl) scintillating crystals. \nThere is a strong need to test the long standing DAMA positive observation of a n annual modulation that could be due to Dark Matter\, with the same targe t material and in a model independent way.\nASTAROTH aim is to enhance the sensitivity to the annual modulation signal\, compared to the present tec hnology\, by lowering the detection energy threshold\, making it possible for the first time to observe sub-keV recoils. \nThis can be achieved by r eading the scintillation light from the NaI(Tl) crystals with arrays of Si licon PhotoMultipliers (SiPM)\, and placing the detectors in a cryogenic e nvironment. \nIndeed\, SiPMs feature lower dark noise than photomultiplier tubes at T\n\nhttps://indico.ific.uv.es/event/6178/contributions/15883/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15883/ END:VEVENT BEGIN:VEVENT SUMMARY:COSINUS: Cryogenic NaI detectors for direct dark matter search DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15862@indico.ific.uv.es DESCRIPTION:Speakers: Florian Reindl (HEPHY (ÖAW) & TU Wien\, Vienna)\nTo day\, the situation in direct dark matter detection is puzzling: The DAMA/ LIBRA experiment observes an annual modulation signal at high statistical significance and fitting to the expectation of a cold dark matter halo in the milky way. However\, in the so-called standard scenario on dark matter halo and dark matter interaction properties\, the DAMA/LIBRA signal contr adicts the null-results of numerous other experiments.\n\nCOSINUS aims for a model-independent cross-check of the DAMA/LIBRA signal. To be immune to potential dependencies on the target material\, COSINUS will use NaI targ et crystals\, the same material as DAMA/LIBRA. Several experimental effort s with NaI targets are planned or already ongoing. COSINUS is the only exp eriment operating NaI as a cryogenic detector\, which yields several disti nctive advantages: Discrimination between electronic interactions and nucl ear recoils off sodium and iodine on an event-by-event basis\, a lower nuc lear recoil energy threshold\, and a better energy resolution.\n\nIn this contribution\, we will sketch the current status of the COSINUS experiment \, from the development of the cryogenic NaI detectors to the construction of the experimental facility at the LNGS underground laboratory.\n\nhttps ://indico.ific.uv.es/event/6178/contributions/15862/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15862/ END:VEVENT BEGIN:VEVENT SUMMARY:Machine-learning techniques applied to three-year exposure of ANAI S−112 DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15858@indico.ific.uv.es DESCRIPTION:Speakers: Iván Coarasa (Universidad de Zaragoza)\nANAIS (Annu al modulation with NaI(Tl) Scintillators) is a direct dark matter detectio n experiment aiming at the confirmation or refutation of the DAMA/LIBRA po sitive annual modulation signal in the low energy detection rate\, using t he same target and technique. ANAIS−112\, located at the Canfranc Underg round Laboratory in Spain\, is operating an array of 3×3 ultrapure NaI(Tl ) crystals with a total mass of 112.5 kg since August\, 2017. The trigger rate in the region of interest (1-6 keV) is dominated by non-bulk scintill ation events. In order to discriminate these noise events from bulk scinti llation events\, robust filtering protocols have been developed. Although this filtering procedure works very well above 2 keV\, the measured rate f rom 1 to 2 keV is about 50% higher than expected by our background model\, and we cannot discard non-bulk scintillation events as responsible of tha t excess. In order to improve the rejection of noise events\, a Boosted De cision Tree (BDT) has been developed and applied. With this new PMT-relate d noise rejection algorithm\, the ANAIS−112 background between 1 and 2 k eV is reduced by almost 30%\, leading to an increase in sensitivity to the annual modulation signal. In this talk\, the reanalysis of the three year s of ANAIS−112 data taking with this technique will be presented.\n\nhtt ps://indico.ific.uv.es/event/6178/contributions/15858/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15858/ END:VEVENT BEGIN:VEVENT SUMMARY:Characterization of an ultra-high purity NaI(Tl) crystal scintilla tor with the SABRE Proof-of-Principle detector DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15846@indico.ific.uv.es DESCRIPTION:Speakers: Ambra Mariani (Princeton University)\nThe SABRE (Sod ium-iodide with Active Background REjection) experiment aims to detect the annual modulation of the dark matter interaction rate by means of ultra-h igh purity NaI(Tl) crystals immersed in a liquid scintillator (LS) active veto. It focuses on the achievement of a very low background to carry out a model-independent test of the long-standing DAMA/LIBRA result with suffi cient sensitivity using the same target material. The two hemispheres appr oach\, one detector placed at the Gran Sasso National Laboratory (LNGS)\, in Italy\, and the other at the Stawell Underground Physics Laboratory (SU PL)\, in Australia\, allows to disentangle seasonal or site-related effect s from the dark matter annually modulated signal. The SABRE experiment has recently completed a Proof-of-Principle (PoP) phase\, which was devoted t o assess the radiopurity of the crystals as well as the efficiency of the LS veto. In this talk\, the new results on the radiopurity of a 3.4-kg NaI (Tl) crystal scintillator grown within the SABRE Collaboration\, and opera ted underground in the SABRE-PoP setup\, will be presented and discussed. The amount of potassium content in the crystal\, determined by direct coun ting of $^{40}$K\, is found to be \n\nhttps://indico.ific.uv.es/event/6178 /contributions/15846/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15846/ END:VEVENT BEGIN:VEVENT SUMMARY:KDK: Measuring the unique third forbidden electron capture decay o f K-40 for backgrounds in rare-event searches DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15842@indico.ific.uv.es DESCRIPTION:Speakers: Matthew Stukel (Queen's University)\nPotassium-40 (K -40) is a long-lived\, naturally occurring radioactive isotope. The decay products are prominent backgrounds for many rare event searches\, especial ly those involving NaI-based scintillators (ex. DAMA\, ANAIS-112\, COSINE- 100\, SABRE\, COSINUS etc.). The branching ratio of the electron capture d irectly to the ground state of Argon-40 has never been experimentally meas ured and presents an unknown background directly in the 2-6 keV energy reg ion. This is the same region where the DAMA/LIBRA experiment observes thei r unique annual modulation. Knowledge of this branching ratio can place co nstraints on the allowed modulation fraction observed by the DAMA experime nt. In addition\, this branching ratio has important implications for nucl ear physics and geochronology. KDK (Potassium (K) Decay (DK)) is an intern ational collaboration dedicated to the measurement of this branching ratio . The experiment is performed using a silicon drift detector with a therma lly deposited\, enriched K-40 source inside the Modular Total Absorption S pectrometer (MTAS\, Oak Ridge National Laboratory). MTAS is a large NaI de tector whose high gamma-ray efficiency enables the proper discrimination b etween ground and excited state electron capture events. This setup has be en characterized in terms of energy calibration and dead time\, and a tagg ing efficiency of 97.89(6) % has been demonstrated (arXiv:2012.15232 submi tted to NIM). We report on the analysis method and sensitivity for a 44-da y K-40 physics run.\n\nhttps://indico.ific.uv.es/event/6178/contributions/ 15842/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15842/ END:VEVENT BEGIN:VEVENT SUMMARY:Directionality for nuclear recoils in a liquid argon Time Projecti on Chamber DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15829@indico.ific.uv.es DESCRIPTION:Speakers: Xinran Li (Lawrence Berkeley National Laboratory)\nL iquid argon (LAr) is one of the most promising targets for the search of W IMP-like dark matter. LAr dual-phase time projection chamber (LAr TPC) is a leading technology\, able to detect both the scintillation and ionizatio n signals. The correlation in the two signal channels provides a possible handle to measure the recoil direction of the nuclei: if confirmed\, this would allow inferring the incident direction of potential dark matter cand idates.\n\nPrevious work from SCENE resulted in a hint of the existence of a directional effect\, which can potentially pave the way for a tonne sca le directional WIMP search with LAr TPC. To validate this hypothesis\, we conducted the Recoil Directionality (ReD) experiment to measure this corre lation in 70 keV nuclear recoils to the highest precision.\n\nThe ReD TPC was carefully calibrated then irradiated with a neutron beam at the INFN L aboratori Nazionali del Sud\, Catania\, Italy. A model based on directiona l modulation in charge recombination was developed to explain the correlat ion. In this contribution\, we describe the experimental setup\, the theor etical model\, and the preliminary results from data analysis.\n\nhttps:// indico.ific.uv.es/event/6178/contributions/15829/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15829/ END:VEVENT BEGIN:VEVENT SUMMARY:Directional Dark Matter searches with the CYGNO/INITIUM project DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15817@indico.ific.uv.es DESCRIPTION:Speakers: Elisabetta Baracchini (Gran Sasso Science Institute) \nWe are going to present the CYGNO project for the development of an high precision optical readout gaseous TPC for directional Dark Matter search and solar neutrino spectroscopy\, to be hosted at Laboratori Nazionali del Gran Sasso. CYGNO (a CYGNus TPC with Optical readout) fits into the wider context of the CYGNUS proto-collaboration\, for the development of a Gala ctic Nuclear Recoil Observatory at the ton scale with directional sensitiv ity. CYGNO peculiar features are the use of sCMOS cameras and PMTs coupled to GEMs amplification of an Helium-based gas mixture at atmospheric press ure\, in order to achieve 3D tracking with head tail capability and backgr ound rejection down to few keV energy and boost sensitivity to low WIMP ma sses. We will discuss the latest R&D results within the CYGNO project and the prospect for the upcoming underground installation of a 50 L prototype in Fall 2021\, soon to be followed by a O(1) m$^3$ experiment in 2023-202 4. We will illustrate the synergy with the ERC Consolidator Grant project INITIUM aimed at realising negative ion drift operation within the CYGNO 3 D optical approach and how the reduced diffusion could boost the chosen ap proach towards large scale detectors.\n\nhttps://indico.ific.uv.es/event/6 178/contributions/15817/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15817/ END:VEVENT BEGIN:VEVENT SUMMARY:PICOLON dark matter search project DTSTART;VALUE=DATE-TIME:20210831T154000Z DTEND;VALUE=DATE-TIME:20210831T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15815@indico.ific.uv.es DESCRIPTION:Speakers: Ken-Ichi Fushimi (Tokushima University)\nCOSINE-100 and ANAIS-112 are rejecting the annual modulating signal of DAMA/LIBRA. Ho wever\, their background is higher than that of DAMA/LIBRA.\nIt is essenti al to verify the seasonal variations using NaI(Tl) detectors\, which have a lower background than DAMA/LIBRA.\n\nPICOLON (Pure Inorganic Crystal Obs ervatory for LOw-energy Neutr(al)ino) aims to search for cosmic dark matte r by high purity NaI(Tl) scintillator.\nWe developed a highly pure NaI(Tl) crystal by hybrid purification method. \nOur purification method was the optimized combination of recrystallization and resin methods.\nThe recent result of $^{210}$Pb in our NaI(Tl) is less than 5.7 $\\mu$Bq/kg.\n\nThe l ow-background measurement with highly radiopure NaI(Tl) is ongoing in Kami oka Underground Laboratory\, Tohoku University.\nThe present detector cons ists of two prototype detectors\, each mass is 1.3 kg.\nThe NaI(Tl) detect or was installed into the pure copper shield and lead shield.\n\nThe sensi tivity for annual modulating signals and finding dark matter particles wil l be discussed.\n\nReference: K.Fushimi et al.\, Prog. Theor. Exp. Phys. 2 021\, 043F01\, DOI: 10.1093/ptep/ptab020\n\nhttps://indico.ific.uv.es/even t/6178/contributions/15815/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15815/ END:VEVENT BEGIN:VEVENT SUMMARY:Directional Dark Matter Search with NEWSdm DTSTART;VALUE=DATE-TIME:20210831T152500Z DTEND;VALUE=DATE-TIME:20210831T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15795@indico.ific.uv.es DESCRIPTION:Speakers: Artem Golovatiuk (Univ Naples Federico II and INFN)\ nIn spite of the extensive search for the detection of the dark matter (DM )\, experiments have so far yielded null results: they are probing lower a nd lower cross-section values and are touching the so-called neutrino floo r. A way to possibly overcome the limitation of the neutrino floor is a di rectional sensitive approach: one of the most promising techniques for dir ectional detection is nuclear emulsion technology with nanometric resoluti on. The NEWSdm experiment\, located in the Gran Sasso underground laborato ry in Italy\, is based on novel nuclear emulsion acting both as the Weakly Interactive Massive Particle (WIMP) target and as the nanometric-accuracy tracking device. This would provide a powerful method of confirming the G alactic origin of the dark matter\, thanks to the cutting-edge technology developed to readout sub-nanometric trajectories. In this talk we discuss the experiment design\, its physics potential\, the performance achieved i n test beam measurements and the near-future plans. After the submission o f a Letter of Intent\, a new facility for emulsion handling was constructe d in the Gran Sasso underground laboratory which is now under commissionin g. A Conceptual Design Report is in preparation and will be submitted in S ummer 2021.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15795/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15795/ END:VEVENT BEGIN:VEVENT SUMMARY:The Dark-PMT: A Novel Direction Light Dark Matter Detector Based o n Vertically-Aligned Carbon Nanotubes DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15792@indico.ific.uv.es DESCRIPTION:Speakers: Francesco Pandolfi (INFN Rome)\nWe present the lates t results on the development of the Dark-PMT\, a novel light Dark Matter ( DM) detector. The detector is designed to be sensitive to DM particles wit h mass between 1 MeV and 1 GeV. The detection scheme is based on DM-electr on scattering inside a target made of vertically-aligned carbon nanotubes. Vertically-aligned carbon nanotubes have vanishing density in the directi on of the tube axes\, therefore the scattered electrons can leave the targ et without being reabsorbed only if their momentum is parallel to the tube s\, which is what happens when the tubes are parallel to the DM wind. This grants directional sensitivity to the detector\, a unique feature in this DM mass range. We will report on the construction of the first Dark-PMT p rototype\, on the establishment of a state-of-the-art carbon nanotube grow ing facility in Rome\, and on the characterizations of the nanotubes perfo rmed in Rome with XPS and angular-resolved UPS spectroscopy.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15792/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15792/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino and Axion Astronomy with Dark Matter Experiments DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15910@indico.ific.uv.es DESCRIPTION:Speakers: Volodymyr Takhistov (Kavli IPMU\, U. Tokyo)\nBeyond their unprecedented sensitivity to dark matter (DM)\, as I will demonstrat e\, large direct detection experiments constitute impressive neutrino tele scopes. This opens a new window into astronomy\, leading to possible insig hts into major problems such as the origin of supermassive black holes. Fu rthermore\, DM experiments can be exploited as novel tools in multi-messen ger astronomy for exploration of new physics. I will discuss detection of relativistic axions from transient astrophysical sources (e.g. axion star explosions)\, which can lead to new insights into the fundamental axion po tential.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15910/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15910/ END:VEVENT BEGIN:VEVENT SUMMARY:Radio-frequency Dark Photon Dark Matter across the Sun DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15906@indico.ific.uv.es DESCRIPTION:Speakers: Jia Liu (Peking University)\nDark photon as an ultra light dark matter candidate can interact with the Standard Model particles via kinetic mixing. We propose to search for the ultralight dark photon d ark matter using radio telescopes with solar observations. The dark photon dark matter can efficiently convert into photons in the outermost region of the solar atmosphere\, the solar corona\, where the plasma mass of phot ons is close to the dark photon rest mass. Due to the strong resonant conv ersion and benefiting from the short distance between the Sun and the Eart h\, the radio telescopes can lead the dark photon search sensitivity in th e mass range of $4 \\times 10^{-8} - 4\\times 10^{-6} \\\, \\rm{eV}$\, co rresponding to the frequency $10 - 1000 \\\, {\\rm MHz}$. As a promising e xample\, the operating radio telescope LOFAR can reach the kinetic mixing $\\epsilon \\sim 10^{-13}$ ($10^{-14}$) within 1 (100) hour solar observ ations. The future experiment SKA phase 1 can reach $\\epsilon \\sim 10^{ -16} - 10^{-14}$ with $1$ hour solar observations.\n\nhttps://indico.ific. uv.es/event/6178/contributions/15906/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15906/ END:VEVENT BEGIN:VEVENT SUMMARY:Stellar Shocks from Dark Matter DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15903@indico.ific.uv.es DESCRIPTION:Speakers: Anirban Das (SLAC National Accelerator Laboratory)\n Macroscopic dark matter is almost unconstrained over a wide ``asteroid-lik e'' mass range\, where it could scatter on baryonic matter with geometric cross section. When such an object travels through a star\, it produces sh ock waves which reach the stellar surface\, leading to a distinctive trans ient optical\, UV and X-ray emission. I shall talk about how this signatur e can be searched for on a variety of stellar types and locations. In a de nse globular cluster\, such events occur far more often than flare backgro unds. Existing UV telescopes\, like Hubble\, could probe orders of magnitu de in dark matter mass in one week of dedicated observation.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15903/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15903/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for a Dark Matter with the PADME experiment DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15835@indico.ific.uv.es DESCRIPTION:Speakers: Isabella Oceano (Salento U. and INFN\, Lecce)\nThe e vidence for the existence of dark matter\, so far is based on its gravitat ional effects. Nevertheless\, many theoretical models assume other non-gra vitational very-weak interactions between dark matter and ordinary matter\ , and to test this hypothesis\, different experiments are trying to direct ly detect dark matter signals at particle accelerators. \nPADME (Positron Annihilation into Dark Matter Experiment) is peculiar since is searching f or dark matter candidates\, and in particular a dark photon\, in the produ cts of the annihilation of a positron beam with the electrons of an active target. This technique only requires that the dark photon couples to the ordinary one allowing to investigate its existence independently from its decay modes.\nThe experiment was build and commissioned at the Laboratori Nazionali di Frascati of INFN at the end of 2018 beginning of 2019\, and c ollected in 2020 $\\sim$ 5×10$^{12}$ positrons on target at 430 MeV.\nThe dark photon signal is searched by studying the missing-mass spectrum of s ingle-photon final states resulting from the annihilation process. PADME i s expected to reach a sensitivity up to $10^{-6}$ in $\\epsilon^2$ (kineti c mixing coefficient) for low-mass dark photons ($\\sim$ 20.MeV). Here we present the performance of the detector and the preliminary results of the ongoing analyses on SM final states: $\\gamma \\gamma$-events and positro n Bremsstrahlung. Prospects for sensitivity to different dark sector candi dates\, ALPs and dark Higgs\, will be also given.\n\nhttps://indico.ific.u v.es/event/6178/contributions/15835/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15835/ END:VEVENT BEGIN:VEVENT SUMMARY:Studying QCD modeling of uncertainties in particle spectra from da rk-matter annihilation into jets DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15833@indico.ific.uv.es DESCRIPTION:Speakers: Adil Jueid (Konkuk University)\nMotivated by various excesses observed by Fermi-LAT and AMS\, we perform a detailed analysis o f QCD uncertainties on particle spectra from dark-matter annihilation (or decay) into jets. When annihilated to SM particles\, the final-state produ cts undergo various complicated processes such as QED and QCD bremsstrahlu ng\, hadronization\, and hadron decays. These processes contain some intri nsic uncertainties which are usually difficult to model and which are negl ected in physical analyses. First\, we perform several re-tunings of the f ragmentation function parameters. Then\, we estimate two kinds of uncertai nties: *(i)* perturbative from QCD showers and *(ii)* non-perturbative fro m hadronization function. The results are tabulated for a wide range of da rk matter masses and annihilation channels. They can be found on Zenodo\; https://doi.org/10.5281/zenodo.3764809\n\nhttps://indico.ific.uv.es/event/ 6178/contributions/15833/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15833/ END:VEVENT BEGIN:VEVENT SUMMARY:Signatures of Primordial Black Holes in theories of Large Extra Di mensions DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15826@indico.ific.uv.es DESCRIPTION:Speakers: Avi Friedlander (Queen's University)\nThe addition o f spatial dimensions compactified to submillimeter scales serves as an ele gant solution to the hierarchy problem. As a consequence of the extra-dime nsional theory\, primordial black holes can be created by high-energy part icle interactions in the early universe. While four-dimensional primordial black holes have been extensively studied\, they have received little att ention in the context of extra-dimensions. We adapt and extend previous an alyses of four-dimensional primordial black holes for the purpose of study ing the impact extra-dimensions have on cosmology. We find new constraints on both extra-dimensional primordial black holes\, and the fundamental ex tra-dimensional theories by combining an analysis of Big Bang Nucleosynthe sis\, the Cosmic Microwave Background\, the Cosmic X-ray Background\, and the galactic centre gamma-rays. With these constraints we explore to what extent these extra-dimensional primordial black holes can comprise the dar k matter in our universe.\n\nhttps://indico.ific.uv.es/event/6178/contribu tions/15826/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15826/ END:VEVENT BEGIN:VEVENT SUMMARY:Signatures of primordial black hole dark matter at DUNE and THEIA DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15812@indico.ific.uv.es DESCRIPTION:Speakers: Valentina De Romeri (IFIC (CSIC-Univ Valencia))\nPri mordial black holes (PBHs) are a potential dark matter candidate whose mas ses can span over many orders of magnitude. If they have masses in the 10^ 15 − 10^17 g range\, they can emit sizeable fluxes of MeV neutrinos thro ugh evaporation via Hawking radiation. We explore the possibility of detec ting light (non-)rotating PBHs with future neutrino experiments DUNE and T HEIA. We will show that they will be able to set competitive constraints o n PBH dark matter\, thus providing complementary probes in a part of the P BH parameter space currently constrained mainly by photon data.\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15812/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15812/ END:VEVENT BEGIN:VEVENT SUMMARY:Low Mass Black Holes from Dark Core Collapse DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15809@indico.ific.uv.es DESCRIPTION:Speakers: Ranjan Laha (Indian Institute of Science\, Bengaluru \, India)\nUnusual masses of black holes being discovered by gravitational wave experiments pose fundamental questions about the origin of these bla ck holes. Black holes with masses smaller than the Chandrasekhar limit $\\ approx$ 1.4  M$_\\odot$ are essentially impossible to produce through stellar evolution. We propose a new channel for production of low mass bla ck holes: stellar objects catastrophically accrete nonannihilating dark ma tter\, and the small dark core subsequently collapses\, eating up the host star and transmuting it into a black hole. The wide range of allowed dark matter masses allows a smaller effective Chandrasekhar limit and thus sma ller mass black holes. We point out several avenues to test our proposal\, focusing on the redshift dependence of the merger rate. We show that reds hift dependence of the merger rate can be used as a probe of the transmute d origin of low mass black holes.\n\nhttps://indico.ific.uv.es/event/6178/ contributions/15809/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15809/ END:VEVENT BEGIN:VEVENT SUMMARY:The Earth as a transducer for dark-photon dark-matter detection DTSTART;VALUE=DATE-TIME:20210830T154000Z DTEND;VALUE=DATE-TIME:20210830T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15802@indico.ific.uv.es DESCRIPTION:Speakers: Saarik Kalia (Stanford University)\nIn this talk\, I will propose the use of the Earth as a transducer for ultralight dark-mat ter detection. In particular I will point out a novel signal of kinetical ly mixed dark-photon dark matter: a monochromatic oscillating magnetic fie ld generated at the surface of the Earth. Similar to the signal in a labo ratory experiment in a shielded box (or cavity)\, this signal arises becau se the lower atmosphere is a low-conductivity air gap sandwiched between t he highly conductive interior of the Earth below and ionosphere or interpl anetary medium above. At low masses (frequencies) the signal in a laborat ory detector is usually suppressed by the size of the detector multiplied by the dark-matter mass. Crucially\, in our case the suppression is by th e radius of the Earth\, and not by the (much smaller) height of the atmosp here. The magnetic field signal exhibits a global vectorial pattern that is spatially coherent across the Earth\, which enables sensitive searches for this signal using unshielded magnetometers dispersed over the surface of the Earth. I will summarize the results of such a search using a publi cly available dataset from the SuperMAG collaboration. The constraints fr om this search are complementary to existing astrophysical bounds. Future searches for this signal may improve the sensitivity over a wide range of ultralight dark-matter candidates and masses.\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15802/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15802/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing light dark matter particles with astrophysical experiments DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15796@indico.ific.uv.es DESCRIPTION:Speakers: Tanmay Kumar Poddar (Physical Research Laboratory)\n Strong bounds from direct detection experiment put stringent limit on the dark matter mass which forces us to go beyond WIMP model of dark matter. I n recent years the light mass dark matter particles gain lots of attention among the particle physicists. In this talk I will discuss about light ga uge bosons motivated from U(1) extension of standard model and axions whic h can be a possible dark matter candidates and its detection in several as trophysical experiments.\n\nhttps://indico.ific.uv.es/event/6178/contribut ions/15796/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15796/ END:VEVENT BEGIN:VEVENT SUMMARY:Precision Measurement of Cosmic Ray Deuterons with the Alpha Magne tic Spectrometer DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15758@indico.ific.uv.es DESCRIPTION:Speakers: Diego Mauricio Gomez Coral (University of Hawaii at Manoa)\nDeuterons are the most abundant of secondary cosmic rays and repre sent a few percent of the single-charged cosmic-ray nuclei. Cosmic-ray deu terons are expected to be produced by fragmentation of primary cosmic-ray Helium with the interstellar medium. Therefore\, a good knowledge of the d euteron abundance and energy dependence provides essential information to verify and constrain cosmic-ray propagation models. Precision measurements of deuteron flux in the rigidity range from 2 to 20 GV as well as deutero n-to-proton flux ratio performed by the Alpha Magnetic Spectrometer during the first 8.5 years onboard the International Space Station will be prese nted.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15758/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15758/ END:VEVENT BEGIN:VEVENT SUMMARY:On the interpretation of the latest AMS-02 cosmic ray electron spe ctrum DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15755@indico.ific.uv.es DESCRIPTION:Speakers: Fiorenza Donato (Torino University & INFN)\nThe late st AMS-02 data on cosmic ray electrons show a break in the energy spectrum around 40~GeV\, with a change in the slope of about 0.1. We perform a com bined fit to the newest AMS-02 positron and electron flux data above 10 Ge V using a model where sources include production of pairs from pulsar wi nd nebulae (PWNe)\, electrons from supernova remnants (SNRs) and both spec ies from spallation of hadronic cosmic rays with interstellar medium atoms .\nWe demonstrate that the change of slope in the AMS-02 electron data is well explained by the interplay between the flux contributions from SNRs a nd from PWNe. In fact\, the relative contribution to the data of these two populations changes by a factor of about 13 from 10 to 1000~GeV. The PWN contribution has a significance of at least $4\\sigma$\, depending on the model used for the propagation\, interstellar radiation field and energy l osses. \nThe effect of the energy losses alone\, when the inverse Compton scattering is properly computed within a fully numerical treatment of the Klein-Nishina cross section\, cannot explain the break in the $e^-$ flux d ata\, as recently proposed in the literature.\n\nhttps://indico.ific.uv.es /event/6178/contributions/15755/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15755/ END:VEVENT BEGIN:VEVENT SUMMARY:New Properties of Secondary Cosmic Rays observed by the Alpha Magn etic Spectrometer on the International Space Station DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15754@indico.ific.uv.es DESCRIPTION:Speakers: Yao Chen (Shandong Institute of Advanced Technology (SDIAT))\nPrecise knowledge of the rigidity dependence of secondary cosmic ray fluxes and of secondary-to-primary flux ratios is essential in the un derstanding of cosmic ray propagation. We report the properties of light s econdary cosmic-ray lithium\, beryllium \, boron nuclei\, and heavy secon dary cosmic ray fluorine nuclei in the rigidity R range 2 GV to 3 TV obser ved by the Alpha Magnetic Spectrometer experiment on the International Sp ace Station. The secondary-to-primary ratios fluorine-to-silicon and boron -to-oxygen (or boron-to-carbon) will be discussed\, showing that the propa gation properties of heavy cosmic rays\, from fluorine to silicon\, are di fferent from those of light cosmic rays\, from helium to oxygen. The prop erties of cosmic-ray sodium and aluminum nuclei\, which are partly seconda ry and partly primary\, will also be presented.\n\nhttps://indico.ific.uv. es/event/6178/contributions/15754/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15754/ END:VEVENT BEGIN:VEVENT SUMMARY:Update on the characterisation of the pGCT\, a 4m-prototype telesc ope built as part of the Cherenkov Telescope Array project DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15752@indico.ific.uv.es DESCRIPTION:Speakers: Emma Rébert (Observatoire de Paris GEPI)\nThe Gamma -ray Cherenkov Telescope prototype (pGCT) is a prototype of an Imaging Atm ospheric Cherenkov Telescope\, developed as Small-Sized Telescope (SST) of 4m during the preparation of the Cherenkov Telescope Array (CTA). Based o n a Schwarzschild-Couder dual-mirror optical design providing an optimised Point Spread Function (PSF) on a wide field\, it had its first Cherenkov light on the Meudon site of the Observatoire de Paris in 2015. Since the d ecision of CTA to harmonize its future SSTs\, the pGCT instrument and the experience gained with its development are now used by the Observatoire de Paris team to provide a test bench for Cherenkov astronomy and a pedagogi cal tool for educational purposes in Meudon. This paper briefly describes the design of the pGCT and presents the lastest advances in the optics of the prototype and its characterisation\, directly related to the implement ation of new high-quality metallic mirrors carried out since 2020.\n\nhttp s://indico.ific.uv.es/event/6178/contributions/15752/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15752/ END:VEVENT BEGIN:VEVENT SUMMARY:The High-Energy Particle Detector capabilities in the measurement of proton and electron fluxes along the China Seismo-Electromagnetic Satel lite orbits DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15751@indico.ific.uv.es DESCRIPTION:Speakers: Alessandro Sotgiu (INFN - section of Rome "Tor Verga ta")\nCSES-01 (China Seismo-Electromagnetic Satellite) is a multi-instrume ntal space mission developed by CNSA (Chinese National Space Administratio n) and ASI (Italian Space Agency) to investigate the near-Earth electromag netic\, plasma\, and particle environment\, focusing on the perturbations induced by natural sources and anthropocentric emitters. The Italian High- Energy Particle Detector (HEPD-01) onboard CSES-01\, made of two planes of silicon tracker and a calorimeter of plastic scintillators and LYSO inorg anic crystals\, provides precise measurements for electrons of 3-100 MeV\, protons of 30-200 MeV\, and light nuclei. The good capabilities in the de tection of particles\, combined with a very large detector acceptance and with the CSES-01 polar orbit\, make HEPD-01 well suited for many different purposes. These include measurements of the primary cosmic ray spectra\, the trapped proton spectra inside the South Atlantic Anomaly\, and the re- entrant albedo all-electrons fluxes. In this work\, we present the data-an alysis techniques and the different approaches used to provide measurement s of the different particle populations detected along the CSES-01 orbits. Some of the recent HEPD-01 results are presented and compared with models \, as the NASA AP9\, which provides predictions of high-energy proton spec tra in the radiation belts\, or the HelMod model\, used to simulate the so lar modulation effects of cosmic rays in the heliosphere.\n\nhttps://indic o.ific.uv.es/event/6178/contributions/15751/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15751/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Light Nuclei Isotopes Measured by the Alpha Magnetic Sp ectrometer on the ISS DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15749@indico.ific.uv.es DESCRIPTION:Speakers: Jiahui Wei (Université de Genève)\nPrecise knowled ge of the spectra of secondary cosmic-ray isotopes provides a powerful too l to constrain cosmic-ray propagation models. In particular\, $^3$He isoto pes in cosmic rays are produced by interactions of primary $^4$He with the interstellar medium\; similarly\, lithium and beryllium are mainly produc ed by the fragmentation of heavier primary cosmic-ray nuclei. Among light isotopes\, the radioactive $^{10}$Be\, which has half-life comparable to t he cosmic-ray residence time in the Galaxy\, provides crucial complementar y information. We present precision measurements of the fluxes of helium i sotopes\, $^3$He and $^4$He\, lithium isotopes\, $^6$Li and $^7$Li\, and b eryllium isotopes\, $^7$Be\, $^9$Be and $^{10}$Be\, as well as the time de pendence of the $^3$He/$^4$He flux ratio\, based on data collected by AMS on the International Space Station.\n\nhttps://indico.ific.uv.es/event/617 8/contributions/15749/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15749/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraining positron emission from pulsar populations with AMS-02 data DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15745@indico.ific.uv.es DESCRIPTION:Speakers: Luca Orusa (Turin U. and INFN)\nThe cosmic-ray flux of positrons ($e^+$) is measured with high precision by the space-borne pa rticle spectrometer AMS-02. The hypothesis that pulsar wind nebulae (PWNe) can significantly contribute to the excess of the $e^+$ cosmic-ray flux h as been consolidated after the observation of a $\\gamma$-ray emission at TeV energies of a few degree size around Geminga and Monogem PWNe. \nIn th is work we simulate Galactic pulsars populations adopting different distri butions for their position in the Galaxy as well as their intrinsic physic al properties\, in order to overcome the incompleteness of the ATNF catalo gue. We fit the $e^+$ AMS-02 data together with a secondary component due to collisions of primary cosmic rays with the interstellar medium. We find that several mock galaxies have a pulsar population able to explain the o bserved $e^+$ flux\, characterized by few\, bright sources. We determine t he physical parameters of the sources dominating the $e^+$ flux\, and asse ss the impact of different assumptions on radial distributions\, spin-down properties\, propagation scenarios and $e^+$ emission time.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15745/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15745/ END:VEVENT BEGIN:VEVENT SUMMARY:Using PIC and PIC-MHD to model the interaction between an electron -positron beam and a thermal plasma DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15744@indico.ific.uv.es DESCRIPTION:Speakers: Allard Jan van Marle (LUPM)\nThe origin of the gamma -ray halo around pulsars is associated with the reduced diffusivity of ene rgetic particles responsible for gamma-ray emission with respect to the me an-free path they adopt in the interstellar medium. A possible explanation for this behaviour is that the energetic particles released from the puls arwind termination shock themselves trigger the turbulence necessary to ex plain this reduced diffusivity (Evoli et al 2018). \nIn order to test the ability of the e-e beam to trigger an efficient streaming instability we a re in the process of conducting a series of benchmarking simulations using both PIC and PIC-MHD techniques to follow the evolution of both the elect ron-positron beam and the thermal background plasma and determine whether the beam can trigger the necessary instabilities. \nWe find that the passa ge of the electron-positron beam through the thermal plasma triggers strea ming instabilities that lead to local amplification of the magnetic field. \n\nhttps://indico.ific.uv.es/event/6178/contributions/15744/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15744/ END:VEVENT BEGIN:VEVENT SUMMARY:Status and prospects of the CRAFFT project for the next generation UHECR observation DTSTART;VALUE=DATE-TIME:20210902T152500Z DTEND;VALUE=DATE-TIME:20210902T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15736@indico.ific.uv.es DESCRIPTION:Speakers: Daisuke Ikeda (Kanagawa University)\nRecent observat ions by TA and Auger have advanced our understanding of ultra-high energy cosmic rays\, but their origin is still unclear. As a future approach\, it will be effective to obtain the directional energy spectra and compositio nal distributions by observing even larger statistics\, and there are acti ve discussions on future large-scale experiments. In order to realize such a huge observation area\, the Cosmic Ray Air Fluorescence Fresnel lens Te lescope (CRAFFT) project has started to develop a cost-effective fluoresce nce telescope with Fresnel lenses. We have succeeded in observing cosmic r ay induced air showers by simultaneous observations with TA using prototyp e telescope\, and the cost has reached 1/10 of the existing fluorescence t elescopes. The progress of the development of autonomous observation syste m and improved telescope\, the performance of event reconstruction\, the c onfiguration and analysis results of the test observation\, and future pro spects will be discussed.\n\nhttps://indico.ific.uv.es/event/6178/contribu tions/15736/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15736/ END:VEVENT BEGIN:VEVENT SUMMARY:CTA prospects for annihilating dark matter from observations of ne arby spiral galaxies DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15771@indico.ific.uv.es DESCRIPTION:Speakers: Miltiadis Michailidis (Univ Tübingen (IAAT))\nTBC\n \nhttps://indico.ific.uv.es/event/6178/contributions/15771/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15771/ END:VEVENT BEGIN:VEVENT SUMMARY:Intergalactic electromagnetic cascade echo from GRB 190114C DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15770@indico.ific.uv.es DESCRIPTION:Speakers: Timur Dzhatdoev (Moscow State University)\nPrimary v ery high energy (VHE\, E>100 GeV) gamma-rays from distant (redshift z>0.1) extragalactic gamma-ray sources are partially absorbed on extragalactic b ackground light (EBL) photons by means of the pair production process \\ga mma\\gamma\\rightarrow e^{+}e^{-} with the subsequent formation of interga lactic electromagnetic cascades through inverse Compton scattering of seco ndary electrons (mostly on cosmic microwave background (CMB) photons). The se electrons get deflected in the extragalactic magnetic field (EGMF)\; th erefore\, the parameters of the observable gamma-ray flux are sensitive to the EGMF strength and structure. The weakest EGMF (magnetic field strengt h B\n\nhttps://indico.ific.uv.es/event/6178/contributions/15770/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15770/ END:VEVENT BEGIN:VEVENT SUMMARY:Observable spectral and angular distributions of gamma-rays from e xtragalactic ultrahigh energy cosmic ray accelerators: application to extr eme TeV blazars DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15769@indico.ific.uv.es DESCRIPTION:Speakers: Timur Dzhatdoev (Moscow State University)\nThe origi n of gamma-ray radiation of extreme TeV blazars (ETBs) — active galactic nuclei with unusually hard observable spectra in the TeV energy region — is still poorly understood. This is especially unfortunate since ETB s tudies are important in extragalactic background light measurements\, and extremely important in extragalactic magnetic field measurements and axion -like particle searches. Besides very hard gamma-ray spectra\, ETBs are us ually characterized by relatively weak (~dozens of percent) and slow (typi cal timescale of ~months-years) variability of the gamma-ray flux. These u nusual properties of ETBs could in principle be explained if the observabl e gamma-rays were formed not inside these sources\, but rather in the inte rgalactic medium as a result of the development of electromagnetic cascade s. A scenario assuming the primary ultrahigh energy (E>1 EeV) protons — the so-called intergalactic hadronic cascade scenario (IHCM) — enjoyed e specially high popularity during the last decade. In the present work we c alculate the observable spectrum and angular distribution of observable ga mma-rays from extreme TeV blazars in the framework of the IHCM scenario\, for the first time taking into account the effect of primary proton deflec tion in filaments and galaxy clusters of a realistic extragalactic magneti c field. We show that the observable point-like spectrum (i.e. the spectru m inside the point spread function of a typical imaging atmospheric Cheren kov telescope) at multi-TeV energies is significantly softer than the one averaged over all values of the observable angle. The width of the observa ble angular distribution at E>10 GeV is greater than or comparable to the extent of the point spread function of operating and next-generation gamma -ray telescopes. These results imply that electromagnetic cascades from pr imary ultrahigh energy protons do not enhance the effective transparency o f the Universe in the very high energy range significantly. The reported s tudy was funded by RFBR\, Russia\, project number 20-32-70169.\n\nhttps:// indico.ific.uv.es/event/6178/contributions/15769/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15769/ END:VEVENT BEGIN:VEVENT SUMMARY:The Search for Ultra-High Energy Neutrinos through Highly Inclined Air Showers in the Pierre Auger Observatory DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15764@indico.ific.uv.es DESCRIPTION:Speakers: Gonzalo Parente (Universidade de Santiago de Compost ela)\nThe Surface Detector of the Pierre Auger Observatory\, an array of 1 600 water-\nCherenkov stations in a triangular grid with 1500 m separation between\nstations\, has the capability to detect neutrinos with energy ab ove 10^17 eV. The\nidentification through the special characteristics of h ighly inclined showers is\nefficiently performed for neutrinos of all flav ours interacting deep in the\natmosphere at large zenith angles as well as for Earth skimming τ neutrinos.\nIn this talk I review the status of the neutrino search at the Observatory using\nabout 15 years of data. Restric tive upper bounds on the neutrino flux from\ndiffuse sources and from poin t-like steady sources were stablished placing\nstrong constraints on sever al models of neutrino production at EeV energies\nand on the properties of the sources of ultra-high-energy cosmic rays.\nUnrivaled sensitivity in s earches for transient sources has been also achieved.\n\nhttps://indico.if ic.uv.es/event/6178/contributions/15764/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15764/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for High-Energy Neutrinos from Ultra-Luminous Infrared G alaxies with IceCube DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15763@indico.ific.uv.es DESCRIPTION:Speakers: Pablo Correa (Vrije Universiteit Brussel)\nThis work presents an IceCube search for high-energy neutrinos from Ultra-Luminous Infrared Galaxies (ULIRGs). ULIRGs are the most luminous infrared objects on the sky\, with infrared luminosities exceeding $10^{12}$ solar luminosi ties. They are mainly powered by starbursts that exhibit star-formation ra tes larger than 100 solar masses per year. In addition\, an active galacti c nucleus (AGN) can also contribute significantly to the ULIRG luminosity output. The acceleration of hadrons\, and consequently the production of n eutrinos\, can occur both in starburst and AGN environments. As such\, ULI RGs form a source population that could be responsible for a significant f raction of the diffuse neutrino flux observed by IceCube. In this study we perform a stacking analysis on a representative sample of 75 ULIRGs with redshift $z \\leq 0.13$ using 7.5 years of IceCube data. We find no eviden ce for astrophysical neutrinos correlated with our selection of ULIRGs. We therefore compute upper limits on the contribution of the ULIRG source po pulation to the diffuse neutrino observations\, and also use these limits to constrain model predictions.\n\nhttps://indico.ific.uv.es/event/6178/co ntributions/15763/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15763/ END:VEVENT BEGIN:VEVENT SUMMARY:Searches for sub-PeV photons in coincidence with neutrinos DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15760@indico.ific.uv.es DESCRIPTION:Speakers: Viktor Romanenko (The Institute for Nuclear Research of the Russian Academy of Sciences)\nThe mechanisms of origin of ultrahig h-energy gamma radiation are poorly studied. One way to find out is to sea rch for temporal and directional coincidences of high-energy galactic neut rinos with photons of similar energies. The results of such a search could provide indications of the hadronic origin of this radiation. In this pap er\, we report on the search for photons with energies above 300 TeV in co incidence with high-energy neutrinos. The searches of ultrahigh-energy gam mas were carried out at the Carpet-2 EAS array\, using three years of data taking.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15760/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15760/ END:VEVENT BEGIN:VEVENT SUMMARY:Unveiling the complex correlation patterns and emission mechanisms in Mrk 421 DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15753@indico.ific.uv.es DESCRIPTION:Speakers: Axel Arbet-Engels (ETH Zürich & Max Planck Institut e for Physics\, Münich)\nThe blazar Mrk421 (redshift z=0.031) is one of t he brightest and closest BL Lac type objects\, making it an ideal target t o probe blazar jet physics. We present a detailed characterisation and the oretical interpretation of the broadband emission of Mrk 421\, with a focu s on the multi-band flux correlations. The extensive multi-wavelength obse rvation campaign was organised in 2017\, during which the correlation patt erns show some disparity and complex behaviours. Observations from several instruments are used to achieve an optimal temporal coverage from radio t o TeV energies. In particular\, four multi-hour NuSTAR observations organi sed simultaneously with MAGIC allow to obtain a precise measurement of the falling segments of the two spectral bumps. A detailed investigation of t he very-high-energy (VHE\; >100 GeV) versus X-ray flux correlation is perf ormed\, by binning the data into several sub-energy bands. A positively co rrelated variability is observed\, but the correlation characteristics cha nge substantially across the various bands probed. Furthermore\, during th e simultaneous MAGIC and NuSTAR observations a clear change of the Compton dominance is detected without a simultaneous change in the synchrotron re gime\, indicating an "orphan gamma-ray activity". We also investigate an i ntriguing bright flare at VHE without a substantial flux increase in the X -rays. Within a leptonic scenario\, this behaviour is best explained by th e appearance of a second population of highly-energetic electrons spanning a narrow range of energies. Finally\, our multi-wavelength correlation st udy also reveals an anti-correlation between the UV/optical and X-ray band s at a significance level above 3 sigma. This behaviour suggests changes i n the acceleration and cooling efficiencies of the electrons.\n\nhttps://i ndico.ific.uv.es/event/6178/contributions/15753/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15753/ END:VEVENT BEGIN:VEVENT SUMMARY:Unveiling the origin of steep decay in 𝛾-ray bursts DTSTART;VALUE=DATE-TIME:20210901T154000Z DTEND;VALUE=DATE-TIME:20210901T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15743@indico.ific.uv.es DESCRIPTION:Speakers: Samuele Ronchini (Gran Sasso Science Institute)\nγ- ray bursts (GRBs) are transient cataclysmic events\, whose role became cen tral in the new multi-messenger era. In the present work I propose a novel investigation of the GRB emission mechanism\, via time-resolved spectral analysis of the X-ray tails of bright GRB pulses observed with the XRT ins trument onboard the Neil Gehrels Swift Observatory\, discovering a unique relation between the spectral index and the flux. The investigation of the spectral evolution during the GRB tail is an ideal diagnostic to understa nd the connection between the emission processes\, the cooling processes a nd the outflow environment. I thoroughly discuss possible interpretations in relation to current available models and I show the incompatibility of our results with the standard high latitude emission scenario. Our results for the first time strongly suggest evidence of adiabatic cooling of the emitting particles\, shedding light on fundamental physics of relativistic outflows in GRBs. Finally I discuss the crucial role of future wide-field X-ray telescopes\, such as the mission concept Theseus\, for the characte risation of the GRB tail emission\, highlighting also its importance in th e multi-messenger context.\n\nhttps://indico.ific.uv.es/event/6178/contrib utions/15743/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15743/ END:VEVENT BEGIN:VEVENT SUMMARY:Multimessenger Astronomy of Transient Point Sources at the Pierre Auger Observatory DTSTART;VALUE=DATE-TIME:20210901T152500Z DTEND;VALUE=DATE-TIME:20210901T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15738@indico.ific.uv.es DESCRIPTION:Speakers: Philip Ruehl (University of Siegen)\nOne of the key challenges in astroparticle physics is the identification of the sources o f cosmic rays at the highest energies (above 1 EeV). In this context\, the search for neutral messenger particles in the ultra-high-energy (UHE) reg ime is of high interest. The sources of the gravitational waves (GWs) that can be observed with the current generation of GW detectors provide extre me astrophysical environments that are most likely to be unique in the uni verse. Another extraordinary source candidate is the anomalous blazar TXS 0506+056 which has been found to be coincident with two periods of enhance d high-energy neutrino flux in 2014/15 and 2017 as reported by the IceCube Collaboration. Due to their distance and transient nature\, the capabilit ies of these sources to produce UHE radiation can only be studied through neutral messengers like photons and neutrinos.\nThe Pierre Auger Observato ry near Malargüe\, Argentina\, is the largest air-shower experiment for t he detection of UHE cosmic rays. With its surface detector\, consisting of a grid of 1660 water Cherenkov detectors covering an area of 3000 km²\, it has a unique exposure to UHE photons and neutrinos and has published fi rst constraints on these particles from GW sources and TXS 0506+056.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15738/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15738/ END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray image reconstruction of the Andromeda galaxy DTSTART;VALUE=DATE-TIME:20210901T151000Z DTEND;VALUE=DATE-TIME:20210901T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15733@indico.ific.uv.es DESCRIPTION:Speakers: Celine Armand (Astronomy department\, University of Geneva)\nAndromeda galaxy (M31) represents our nearest large neighbor spir al galaxy with a distance of 785 kpc. Its close proximity allows us to opt ically resolve its stellar disk and bulge as two separate components. Alth ough M31 spans 3.2º x 1º on the sky in optical light\, the determination of its extension in γ rays remains controversial. We analyze about 12 ye ars of Fermi-LAT data using the code skyFACT which combines template fitti ng and image reconstruction. In this work\, we robustly characterize its s pectral and morphological properties against systematic uncertainties rela ted to the modeling of the Galactic diffuse emission. We present for the f irst time a proper comparison of non-nested models describing M31 morpholo gy and show the reconstruction of its γ-ray image in a template-independe nt way in order to identify its components.\n\nhttps://indico.ific.uv.es/e vent/6178/contributions/15733/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15733/ END:VEVENT BEGIN:VEVENT SUMMARY:The impact of IMBHs on properties of binary black holes originatin g from Globular Clusters DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15517@indico.ific.uv.es DESCRIPTION:Speakers: Dorota Gondek-Rosinska (University of Warsaw)\nStell ar mass binary black holes are the most important sources of gravitational waves for current LIGO-Virgo-Kagra detectors. We analyze about a thousan d globular cluster (GC) models simulated using the MOCCA Monte Carlo code for star cluster evolution to study black hole - black hole interactions i n these dense stellar systems that can lead to gravitational wave emission . We extracted information for all coalescing binary black holes (BBHs) th at merge via gravitational radiation from these GC models and for those BH s that collide due to 2-body\, 3-body and 4-body\ndynamical interactions. By obtaining results from a substantial number of realistic star clusters evolution model\, that cover different initial parameters (masses\, metall icities\, densities etc) we have an extremely large statistical sample of two black holes which merge or collide within a Hubble time. The existence of Intermediate Mass Black Hole\, with masses 100-1000 solar masses\, str ongly infuences the results. We study also properties of BBHs escaping fr om globular clusters. Some of them contain IMBH. We discuss the importance of BBH originating from GC for gravitational waves observations.\n\nhttps ://indico.ific.uv.es/event/6178/contributions/15517/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15517/ END:VEVENT BEGIN:VEVENT SUMMARY:Characterizing the observation bias in gravitational-wave detectio ns and finding structured population properties DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15514@indico.ific.uv.es DESCRIPTION:Speakers: Doğa Veske ()\nThe observed distributions of the so urce properties from gravitational-wave detections are biased due to the s election effects and detection criteria in the detections\, analogous to t he Malmquist bias. In this work\, this observation bias is investigated th rough its fundamental statistical and physical origins. A semi-analytical formulation for its estimation for a network of detectors is derived which is more efficient and precise than the standard method of numerical simul ations\, with only a fraction of the computational cost. Then\, the estima ted bias is used for model-independent inferences on the binary black hole population. These inferences show additional structures\, specifically tw o potential mass gaps in the joint mass distribution\, which were not foun d via modelled inferences.\n\nhttps://indico.ific.uv.es/event/6178/contrib utions/15514/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15514/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for Black Hole Merger Families DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15513@indico.ific.uv.es DESCRIPTION:Speakers: Doğa Veske (Columbia U.)\nThe origin\, environment\ , and evolution of stellar-mass black hole binaries are still a mystery. O ne of the proposed binary formation mechanisms is manifest in dynamical in teractions between multiple black holes. A resulting framework of these dy namical interactions is the so-called hierarchical triple merger scenario\ , which happens when three black holes become gravitationally bound\, caus ing two successive black hole mergers to occur. In such successive mergers \, the black holes involved are directly related to each other\, and hence this channel can be directly tested from the properties of the detected b inary black hole mergers. Here we present a search for hierarchical triple mergers among events within the GWTC-1 and GWTC-2 catalogs of LIGO/Virgo\ , the eccentric localization of GW190521 and those found by the IAS-Prince ton group. We perform our analysis for different upper bounds on the mass distribution of first generation BHs. Our results demonstrate the importan ce of the mass distributions' properties for constraining the hierarchical merger scenario. We present the individually significant merger pairs. Th e search yields interesting candidate families and hints of its future imp act.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15513/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15513/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing the Ultralight Boson with the Ringdown Phase of Black Hole Mergers DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15510@indico.ific.uv.es DESCRIPTION:Speakers: Joseph Gais ()\nUltralight bosons are an encouraging class of dark matter candidate particles\, which may form long-lived boso nic clouds surrounding rotating black holes via superradiance. We compute the shifts in the gravitational quasinormal-mode frequencies of supermassi ve black holes due to the presence of such a bosonic cloud. We then use th e modified ringdown waveform of a supermassive black hole from a surroundi ng bosonic cloud as a novel probe of the existence of a potential ultralig ht boson of mass $ \\in [10^{-16}\, 10^{-18} ] \\rm eV$. Because the ringd own signal of a binary merger is significantly shorter than the inspiral\, our ringdown test of the ultralight boson can probe masses on timescales relatively shorter than inspiral-based\, stochastic\, or population-based search methods.\n\nhttps://indico.ific.uv.es/event/6178/contributions/1551 0/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15510/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching gravitational wave echoes in the post-merger phase after a binary black hole coalescences. DTSTART;VALUE=DATE-TIME:20210901T154000Z DTEND;VALUE=DATE-TIME:20210901T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15505@indico.ific.uv.es DESCRIPTION:Speakers: Andrea Miani (Virgo\, cWB Trento-Padova group)\nCurr ent gravitational wave (GW) surveys of binary black hole (BBH) mergers pro vide unprecedented probes of the dynamics in extreme gravitational fields and relativistic velocities.\nIt has been proposed that such compact objec ts may display exotic characteristics and could produce repeated GW pulses of widely uncertain morphology (echoes) in the post-merger phase. A detec tion of echoes would be a smoking gun on the existence of exotic compact o bjects (ECOs) and would shed light on their nature and their constituents. \nWe will present a method to search for echoes that is agnostic to the pr operties of the GW pulses and it is based on a targeted version of coheren tWaveBurst (cWB)\, the unmodelled GW transient search algorithm\, develope d in the LIGO Scientific Collaboration (LSC) and Virgo Collaboration and w idely used on LIGO-Virgo-KAGRA data.\nWe will discuss the results of this search on LIGO-Virgo open data and provide new upper limits in terms of th e detectable energy of echo-like signals. We will present some constraints that these observations set on the parameters space of ECOs' models.\n\nh ttps://indico.ific.uv.es/event/6178/contributions/15505/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15505/ END:VEVENT BEGIN:VEVENT SUMMARY:The search of higher multipole radiation in gravitational waves fr om compact binary coalescences by a minimally-modelled pipeline DTSTART;VALUE=DATE-TIME:20210901T152500Z DTEND;VALUE=DATE-TIME:20210901T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15501@indico.ific.uv.es DESCRIPTION:Speakers: Odysse Halim (INFN Trieste)\nThe coherent WaveBurst (cWB) pipeline implements a minimally-modelled search to find a coherent r esponse in the network of gravitational wave detectors of the LIGO-Virgo C ollaboration in the time-frequency domain. Here we describe an extension o f the cWB analysis to detect spectral features beyond the main quadrupolar emission of gravitational waves during the inspiral phase of compact bina ry coalescences. The search is performed by defining specific regions in t he time-frequency map to extract the energy of harmonics of main quadrupol e mode in the inspiral phase. The shapes of these regions are fixed by a m ild optimization of their Receiver Operating Characteristic curves. This m ethod has already been used in the GW190814 discovery paper (ref. ApJ). He re we describe in full detail the procedure to detect the (3\, 3) multipol e in GW190814 within the cWB framework\, as well as additional searches fo r other subdominant modes. We also apply this method on another event that displays possible higher multipoles\, GW190412.\n\nKeywords: gravitationa l waves\, analysis\, multipoles\, compact binary coalescences\n\nhttps://i ndico.ific.uv.es/event/6178/contributions/15501/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15501/ END:VEVENT BEGIN:VEVENT SUMMARY:Towards a gravitational-wave catalogue of boson-star mergers DTSTART;VALUE=DATE-TIME:20210901T151000Z DTEND;VALUE=DATE-TIME:20210901T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15498@indico.ific.uv.es DESCRIPTION:Speakers: Juan Calderon Bustillo (Galician Institute of High E nergy Physics (IGFAE))\nAdvanced LIGO and Virgo have delivered a conclusiv e gravitational-wave signal consistent with compact binary mergers in the intermediate-mass black-hole range and as well as several lower significan ce triggers. These signals have challenged in several ways our vanilla an alysis methods\, all done within the “canonical” paradigm of quasi-cir cular black hole mergers. First\, under such assumption\, GW190521 points to the existence of a black-hole in the PISN gap. Second\, analyses perfor med on the lower significance trigger S200114f with different waveform fam ilies report inconsistent results. The barely observable pre-merger emissi on of these signals\, however\, allows for the consideration of alternativ e scenarios both within and beyond the black-hole merger one. In this talk \, we will present an analysis of GW190521 and S200114f within the paradig m of the merger of horizonless compact objects known as boson (Proca)-star s\, providing estimates of the mass of the underlying ultralight bosons. T his could be the first step towards the construction of an eventual catalo gue of mergers of compact exotic objects.\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15498/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15498/ END:VEVENT BEGIN:VEVENT SUMMARY:Preparing for the future gravitational wave burst searches with ma chine learning techniques DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15511@indico.ific.uv.es DESCRIPTION:Speakers: Sophie Bini (Univ. Trento)\nGeneric searches for gra vitational wave bursts are a powerful discovery tool and in the near futur e they are expected to unveil new phenomena. The coherentWaveBurst (cWB) p ipeline is a state-of-the-art burst search pipeline\, and it has been used to analyze the data from the latest observing runs of the LIGO/Virgo dete ctors.\nIn preparation for the next observing run\, which will include KAG RA detector\, we are investigating several improvements involving also the application of cutting edge machine learning techniques. A decision tree algorithm will address the post production analysis of the candidate event s\, upgrading the selection criteria and ranking procedures applied so far . Moreover\, an autoencoder neural network will pinpoint morphologies asso ciated to well known noise transients\, mitigating their impact.\nWe show that both these procedures are robust and do not limit the general charact er of the search. We present preliminary results on public LIGO-Virgo data for widely different burst morphologies\, ranging from extreme ad-hoc sig nals to more astrophysically inspired gravitational-wave transients.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15511/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15511/ END:VEVENT BEGIN:VEVENT SUMMARY:Looking for Core-Collapse Supernovae with Gravitational Waves and Low-energy Neutrinos DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15503@indico.ific.uv.es DESCRIPTION:Speakers: Giulia Pagliaroli (INFN)\nCore-collapse supernovae a re fascinating astrophysical objects for multimessenger studies. Gravitati onal waves (GWs) are expected to play a role in the supernova explosion me chanism\, however their complex modelling makes the detection very challen ging. Low-energy neutrinos will be emitted enormously during the core-coll apse explosion and can help for the gravitational wave counterpart search. In this work we develop a multi-messengers strategy to search for such as trophysical objects by exploiting a global network of both low-energy neut rino and gravitational wave detectors. We also improve the detection poten tial of the neutrino sub-network by exploiting the temporal behaviour of a neutrino burst from a core-collapse supernova. We show that with the pro posed approach neutrino detectors can gain at least 10% of detection effic iency at the distance where their efficiency drops. Then\, we combine the information provided by GW and neutrino in a multi-messenger strategy. I n particular\, we obtain an increase of the probability to detect the GW s ignal from a CCSN at 60 kpc from zero when using only GW analysis to ∼33 % with our combined GW-ν approach.\n\nhttps://indico.ific.uv.es/event/617 8/contributions/15503/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15503/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for long-duration transient gravitational waves from glitch ing pulsars during LIGO-Virgo third observing run DTSTART;VALUE=DATE-TIME:20210902T154000Z DTEND;VALUE=DATE-TIME:20210902T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15502@indico.ific.uv.es DESCRIPTION:Speakers: Luana Modafferi (Universitat de les Illes Balears)\n Pulsars are spinning neutron stars which emit an electromagnetic beam. We expect pulsars to slowly decrease their rotational frequency. However\, su dden increases of the rotational frequency have been observed from differe nt pulsars. These events are called “glitches”\, and they are followed by a relaxation phase with timescales from days to months. Gravitational waves (GWs) emission may follow these peculiar events. We give an overview of an analysis of GW data from the Advanced LIGO and Virgo third observin g run (O3) searching for transient GW signals lasting hours to months afte r glitches in known pulsars during the 2019-2020 run period. The search me thod consists of placing a template grid in frequency-spindown space with fixed grid spacings. Then\, for each point we compute the transient F-stat istic which is maximized over a set of transient parameters like the durat ion and start time of the potential signals. A threshold on the detection statistic is then set\, and we search for peaks over the parameter space f or each candidate.\n\nhttps://indico.ific.uv.es/event/6178/contributions/1 5502/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15502/ END:VEVENT BEGIN:VEVENT SUMMARY:All-sky search in early O3 LIGO data for continuous gravitational- wave signals from unknown neutron stars in binary systems DTSTART;VALUE=DATE-TIME:20210902T152500Z DTEND;VALUE=DATE-TIME:20210902T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15499@indico.ific.uv.es DESCRIPTION:Speakers: Rodrigo Tenorio (Universitat de les Illes Balears)\n Rapidly spinning neutron stars are promising sources of persistent gravita tional waves. Detecting such a signal would allow probing of the physical properties of matter under extreme conditions. A significant fraction of t he known pulsar population belongs to binary systems. Searching for unknow n neutron stars in binary systems requires specialized algorithms to addre ss unknown orbital frequency modulations. We present a search for continuo us gravitational waves emitted by neutron stars in binary systems in early data from the third observing run of the Advanced LIGO and Advanced Virgo detectors using the semicoherent\, GPU-accelerated\, BinarySkyHough pipel ine. The search analyzes the most sensitive frequency band of the LIGO det ectors\, 50 - 300 Hz. Binary orbital parameters are split into four region s\, comprising orbital periods of 3 - 45 days and projected semimajor axes of 2 - 40 light-seconds. No detections are reported. We estimate the sens itivity of the search using simulated continuous wave signals\, achieving the most sensitive results to date across the analyzed parameter space.\n\ nhttps://indico.ific.uv.es/event/6178/contributions/15499/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15499/ END:VEVENT BEGIN:VEVENT SUMMARY:FCF formulation of Einstein equations: local uniqueness and numeri cal accuracy and stability DTSTART;VALUE=DATE-TIME:20210902T151000Z DTEND;VALUE=DATE-TIME:20210902T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15496@indico.ific.uv.es DESCRIPTION:Speakers: Samuel Santos-Pérez (Universitat de València)\nWe present Einstein equations in the so-called Fully Constrained Formulation (FCF). This formulation has two different sectors: the elliptic sector for med by the Hamiltonian and Momentum constraints together with the equation s derived from the gauge choice\, and the hyperbolic sector which encodes the evolution of the rest of degrees of freedom of the spacetime metric in cluding the gravitational waves. We present a modification of both sectors that keeps local uniqueness properties but has a better behaviour regardi ng the relativistic expansion of the equations. We also comment on numeric al properties of this reformulation and some potential applications.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15496/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15496/ END:VEVENT BEGIN:VEVENT SUMMARY:Primordial non-Gaussianity from the angular clustering: prospects for DES DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15692@indico.ific.uv.es DESCRIPTION:Speakers: Walter Riquelme (IFT UAM-CSIC)\nPrimordial non-Gauss ianity (PNG) is claimed to be a smoking gun to differentiate between the v ast collection of inflationary models. The current constraints on PNG\, pa rametrized by $f_{NL}$\, are obtained from the CMB\, which has reached the cosmic variance limit. A promising way to look for PNG is using the Large Scale Structures (LSS) of the universe\, with the potential of breaking t he $\\sigma(f_{NL})\\sim1$ barrier.\nIn this talk\, I will present an anal ysis of the methods for looking at Primordial non-Gaussianity in the Large Scale Structure of the Universe\, with the main focus on the Dark Energy Survey (DES).\nWe use the Angular Correlation Function (ACF) and show how it is modified by Primordial Non-Gaussianity via a scale-dependent bias (D alal et al. 2008). One of the main focus of the work is on the integral co nstraint (IC) condition\, which is found to be key to obtain unbiased PNG constraints. The IC corrects for the fact that the mean density of the Uni verse is measured from the observed galaxies.\nThe methods are analyzed an d optimized for two kinds of simulations: COLA mocks that follow the DES a ngular and redshift distribution and N-Body simulations with non-Gaussian initial conditions. With the aforementioned simulations\, we focus on opti mizing the methods to constraint $f_{NL}$ to obtain precise and unbiased r esults\, preparing the ground for the DES Y3 data. We highlight the potent ial that DES and future photometric surveys could have in constraining PNG .\n\nhttps://indico.ific.uv.es/event/6178/contributions/15692/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15692/ END:VEVENT BEGIN:VEVENT SUMMARY:Solid matter with zero shear modulus in flat universe DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15691@indico.ific.uv.es DESCRIPTION:Speakers: Peter Mészáros (Department of Theoretical Physics\ , Comenius University in Bratislava\, Slovakia)\nFor a perfect fluid\, the quantity defined through mixed components of the stress-energy tensor $\\ widetilde{w}=(T_{i}^{\\phantom{i}i}/3)/(-T_{0}^{\\phantom{0}0})$ is indepe ndent on the choice of coordinates only for two values of the pressure to energy density ratio $w=p/\\rho$: for radiation with $w=1/3$\, and for dar k energy with $w=-1$. With other choices of $w$\, the quantity $\\widetild e{w}$ is coordinate dependent\, and $\\widetilde{w}=w$ only in the local r est frame of the fluid. We show that the same is true also for solid matte r with shear stress Lamé coefficient set to zero in a flat Friedmann-Lema itre-Robertson-Walker universe with perturbed metric as well as stress-ene rgy tensor. We call the two different solids with coordinate independent $ \\widetilde{w}$ radiation-like solid and dark energy-like solid\, and we r estrict ourselves to these two special cases. By analysing second order pe rturbations we discover two one parametric sets of such solid matter model s containing special cases of radiation and dark energy as perfect fluids. We also study equations for perturbations up to the second order for both sets of models.\n\nhttps://indico.ific.uv.es/event/6178/contributions/156 91/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15691/ END:VEVENT BEGIN:VEVENT SUMMARY:Aspects of High Scale Leptogenesis with Low-Energy Leptonic CP Vio lation DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15684@indico.ific.uv.es DESCRIPTION:Speakers: Alessandro Granelli (SISSA)\nUsing the density matri x equations (DME) for high scale leptogenesis based on the type I seesaw m echanism\, in which the CP violation (CPV) is provided by the low-energy D irac or/and Majorana phases of the neutrino mixing (PMNS) matrix\, we inve stigate the 1-to-2 and the 2-to-3 flavour regime transitions\, where the 1 \, 2 and 3 leptogenesis flavour regimes in the generation of the baryon as ymmetry of the Universe $\\eta_B$ are described by the Boltzmann equations . Concentrating on the 1-to-2 flavour transition we determine the general conditions under which $\\eta_B$ goes through zero and changes sign in the transition. Analysing in detail the behaviour of $\\eta_B$ in the transit ion in the case of two heavy Majorana neutrinos $N_{1\,2}$ with hierarchic al masses\, $M_1 \\ll M_2$\, we find\, in particular\, that i) the Boltzma nn equations in many cases fail to describe correctly the generation of $ \\eta_B$ in the 1\, 2 and 3 flavour regimes\, ii) the 2-flavour regime can persist above (below) $\\sim 10^{12}$ GeV ($\\sim 10^9$ GeV)\, iii) the f lavour effects in leptogenesis persist beyond the typically considered max imal for these effects leptogenesis scale of $10^{12}$ GeV. We further det ermine the minimal scale $M_{1\\text{min}}$ at which we can have successfu l leptogenesis when the CPV is provided only by the Dirac or Majorana phas es of the PMNS matrix as well as the ranges of scales and values of the ph ases for having successful leptogenesis. We show\, in particular\, that wh en the CPV is due to the Dirac phase $\\delta$\, there is a direct relatio n between the sign of $\\sin \\delta$ and the sign of $\\eta_B$ in the reg ions of viable leptogenesis in the case of normal hierarchical light neutr ino mass spectrum\; for the inverted hierarchical spectrum the same result holds for $M_1 \n\nhttps://indico.ific.uv.es/event/6178/contributions/156 84/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15684/ END:VEVENT BEGIN:VEVENT SUMMARY:Recovering BAO in a SKA intensity mapping survey DTSTART;VALUE=DATE-TIME:20210901T154000Z DTEND;VALUE=DATE-TIME:20210901T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15673@indico.ific.uv.es DESCRIPTION:Speakers: Bernhard Vos Ginés (Universidad Autónoma de Madrid )\nThe radio-observatory Square Kilometre Array (SKA) will have great pote ntial to map the large-scale structure of the Universe. HI Intensity Mappi ng is one of the main planned surveys\, that will map neutral hydrogen (HI ) using large angular pixels\, but which will be able to reconstruct the t hree dimensional LSS of the Universe at very large scales (0 \n\nhttps://i ndico.ific.uv.es/event/6178/contributions/15673/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15673/ END:VEVENT BEGIN:VEVENT SUMMARY:Turnaround physics beyond spherical symmetry DTSTART;VALUE=DATE-TIME:20210901T152500Z DTEND;VALUE=DATE-TIME:20210901T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15671@indico.ific.uv.es DESCRIPTION:Speakers: Valerio Faraoni (Bishop's University)\nThe concept o f turnaround radius in an accelerating universe is generalized to arbitrar ily large deviations from spherical symmetry\, as needed for astronomical observations. As an application\, the turnaround surface is characterized when deviations from spherical symmetry are small and is extended to scala r-tensor gravity. An independent approach for small non-sphericities using the Hawking quasilocal energy produces the same result.\n[Based on A Gius ti & V. Faraoni 2021\, Phys. Rev. D 103\, 044049 (arXiv:1911.05130)\; 2019 \, Phys. Dark Universe 26\, 100353 (arXiv:1905.04263)]\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15671/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15671/ END:VEVENT BEGIN:VEVENT SUMMARY:Screening vs. gevolution: in chase of a perfect cosmological simul ation code DTSTART;VALUE=DATE-TIME:20210901T151000Z DTEND;VALUE=DATE-TIME:20210901T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15670@indico.ific.uv.es DESCRIPTION:Speakers: Maxim Eingorn (North Carolina Central University)\nW e compare two competing relativistic approaches to the N-body simulation o f the Universe large-scale structure. To this end\, employing the correspo nding alternative computer codes ("gevolution" and "screening")\, we condu ct a series of cosmological simulations in boxes of different sizes and ca lculate the power spectra of the scalar perturbation Φ\, the frame-draggi ng vector potential **B** and the difference between scalar modes χ=Φ− Ψ. We demonstrate that the corresponding power spectra are in very good a greement between the compared schemes. For example\, the relative differen ce of the power spectra for Φ is 0.04% maximum. Since the perturbed Einst ein equations have much simpler form in the "screening" approach\, the sim ulation with this code consumes less computational time\, saving almost 40 % of CPU hours.\n\nhttps://indico.ific.uv.es/event/6178/contributions/1567 0/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15670/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutron-antineutron oscillations as a probe of baryogenesis DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15690@indico.ific.uv.es DESCRIPTION:Speakers: Chandan Hati (Technische Universität München)\nAn observation of Neutron-antineutron ($n-\\bar{n}$) oscillations\, would dir ectly imply physics beyond the Standard Model violating baryon number by t wo units $|\\Delta B| = 2$ and hence might provide a close link to the mec hanism behind the observed baryon asymmetry of the Universe. In this talk\ , I will discuss the consequences of such a discovery in the near future\, e.g. at the Deep Underground Neutrino Experiment or the European Spallati on Source\, for baryogenesis mechanisms. I will discuss both an effective field theory approach and a more concrete simplified model approach with a source of CP violation and different hierarchies between the scales of ne w physics. I will also highlight the complementarity of $n-\\bar{n}$~oscil lation searches with other experimental constraints from dinucleon decay\, LHC\, and meson oscillations and discuss how an observation of $n-\\bar{n }$~oscillation can rule out many potential baryogenesis scenarios and favo ur only a select few providing an exciting possibility to understand our m atter dominated Universe at laboratory.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15690/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15690/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino decay in precision cosmology DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15686@indico.ific.uv.es DESCRIPTION:Speakers: Joe Zhiyu Chen (The University of New South Wales)\n Neutrino decay interaction with scalar majorons naturally arises from Stan dard Model extensions to model neutrino mass generation. The interaction i f present during the CMB epoch has the potential to disrupt neutrino free streaming and hence the CMB anisotropy spectra. This has been previously s tudied as a cosmological constraint on neutrino lifetime. In this work\, w e model the decay interaction with the full collisional Boltzmann hierarch y. The result shows the lifetime constraint from neutrino decay can be rel axed by several orders of magnitude.\n\nhttps://indico.ific.uv.es/event/61 78/contributions/15686/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15686/ END:VEVENT BEGIN:VEVENT SUMMARY:BBN and CMB combined and separate constraints on new physics: meas uring Neff and probing its evolution DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15685@indico.ific.uv.es DESCRIPTION:Speakers: Tsung-Han Yeh (University of Illinois Urbana-Champai gn)\nBig Bang nucleosynthesis (BBN) and the cosmic microwave background (C MB) both probe the physics of the early universe. BBN accounts for the cos mic origin of the lightest chemical elements\, such as helium-4 and deuter ium. Having precisely measured nuclear data and the neutron lifetime as in puts\, BBN abundance predictions depend on two cosmological parameters: th e cosmic baryon-to-photon ratio $\\eta = \\rm n_{b}/n_{\\gamma}$ (equivale nt to the baryon density $\\Omega_{\\rm b}h^{2}$) and the effective number of standard neutrino species $\\rm N_{\\rm eff}$. BBN analysis has long u sed observed primordial abundances from astronomical observations to infer $\\eta$ and $\\rm N_{\\rm eff}$. Crucially\, both parameters are also mea sured independently from the CMB. Thus\, the concordance between BBN and C MB determinations of these two parameters not only provides a critical tes t to the hot Big Bang model but also can reveal new physics. \n\nThe joint BBN+CMB constraint on $\\rm N_{eff}$ is one of the key concerns in the qu est for physics beyond the Standard Model (BSM). Any deviation in $\\rm N_ {\\rm eff}$ from the Standard Model prediction would point to nonstandard cosmology and likely new physics\, as a complementary cosmological approac h to terrestrial particle experiments. Moreover\, the BBN+CMB constraining power on new physics improves whenever new observations with unprecedente d high precision are available. Latest developments of relevant BBN+CMB an alyses will be discussed. Furthermore\, we can search for any changes in $ \\eta$ and/or $\\rm N_{\\rm eff}$ between BBN and the CMB. This is a new p robe: only recently BBN and the CMB independently reach levels of precisio n that can meaningfully reveal such changes. We will present likelihoods o f ($\\Delta \\eta$\, $\\Delta \\rm N_{\\rm eff}$) that constrain a broad v ariety of BSM models\, including extra entropy and/or radiation injection between BBN and the CMB.\n\nhttps://indico.ific.uv.es/event/6178/contribut ions/15685/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15685/ END:VEVENT BEGIN:VEVENT SUMMARY:Massive sterile neutrinos in the Early Universe: from thermal deco upling to cosmological constraints DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15680@indico.ific.uv.es DESCRIPTION:Speakers: Leonardo Mastrototaro (Università degli Studi di Sa lerno - INFN\, Sezione di Napoli\, Gruppo collegato di Salerno)\nWe consid er heavy sterile neutrinos $\\nu_s$ with mass in the range $10~\\mathrm{Me V}≤m_s≤m_π∼135~\\mathrm{MeV}$\, which are thermally produced in the Early Universe\, in collisional processes involving active neutrinos\, an d freezing out after the QCD phase transition. Notably\, if these neutrino s decay after the active neutrino decoupling\, they generate extra neutrin o radiation and contribute to entropy production: they alter the value of the effective number of neutrino species $N_{\\mathrm{eff}}$ and $^4\\mat hrm{He}$ production. We provide a detailed account of the numerical soluti on of the exact relevant Boltzmann equations. Finally\, we also identify t he parameter space allowed by current Planck satellite data and forecast t he parameter space probed by future Stage-4 ground-based CMB observations\ , expected to match or surpass BBN sensitivity\, improving the existing co nstraints on the sterile neutrino parameter space in both cases.\n\nhttps: //indico.ific.uv.es/event/6178/contributions/15680/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15680/ END:VEVENT BEGIN:VEVENT SUMMARY:Intimate relationship between sterile neutrino Dark Matter and ext ra radiation in the early Universe DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15679@indico.ific.uv.es DESCRIPTION:Speakers: Manibrata Sen (UC\, Berkeley)\nkeV-scale gauge-singl et fermions\, allowed to mix with the active neutrinos\, are elegant dark matter (DM) candidates. They are produced in the early universe via the Do delson-Widrow mechanism and can be detected as they decay very slowly\, em itting X-rays. In the absence of new physics\, this hypothesis is virtuall y ruled out by astrophysical observations. In this talk\, I will demonstra te that new interactions among the active neutrinos allow these sterile ne utrinos to make up all the DM while safely evading all current experimenta l bounds. Neutrino interactions mediated by a sub-MeV scalar can also lead a lower bound on the amount of extra radiation in the early Universe. Suc h models can\, therefore\, receive strong constraints from next generation cosmology experiments\, like CMB-S4\n\nhttps://indico.ific.uv.es/event/61 78/contributions/15679/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15679/ END:VEVENT BEGIN:VEVENT SUMMARY:Precision calculation of neutrino evolution in the early Universe DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15669@indico.ific.uv.es DESCRIPTION:Speakers: Julien Froustey (Institut d'Astrophysique de Paris)\ nIn the primordial Universe\, neutrino decoupling occurs only slightly bef ore electron-positron annihilations. This leads notably to an increased ne utrino energy density compared to the standard instantaneous decoupling ap proximation\, parametrized by the effective number of neutrino species $N_ \\mathrm{eff}$. A precise calculation of neutrino evolution is needed to a ssess its consequences on BBN\, structure formation or on the CMB\, and re quires to take into account multiple effects such as neutrino oscillations \, which represents a genuine numerical challenge.\n\nRecently\, several i mprovements have been made towards such a precision calculation\, leading to the new reference value $N_\\mathrm{eff}=3.0440$. We have managed to ge t a deeper understanding of the role of flavour oscillations\, which has l ed to a new approximation of neutrino evolution\, which exploits the large difference between the oscillation time scale and the kinetic evolution t ime scale. This novel approach can be generalized to study for instance th e evolution of neutrino asymmetries in the early universe\, allowing to pe rform a proper 3-neutrino calculation using the full collision term.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15669/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15669/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmological radiation density with non-standard neutrino-electron interactions DTSTART;VALUE=DATE-TIME:20210831T152500Z DTEND;VALUE=DATE-TIME:20210831T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15667@indico.ific.uv.es DESCRIPTION:Speakers: Pablo Martínez-Miravé (IFIC (CSIC-Univ Valencia))\ nNeutrino non-standard interactions (NSI) are known to modify the picture of neutrino decoupling from the cosmic plasma. These NSI alter flavour osc illations through matter effects and the annihilation and scattering betwe en neutrinos and electrons and positrons in the thermal plasma. In view of the forthcoming cosmological observations\, we perform a precision study of the impact of non-universal and flavour-changing NSI on the effective n umber of neutrinos\, $N_{\\rm eff}$. We present the variation of $N_{\\rm eff}$ arising from the different NSI parameters and discuss the existing d egeneracies among them\, from cosmology alone and in relation to the curre nt bounds from terrestrial experiments. We find that future cosmological d ata would provide competitive and complementary constraints for some of th e couplings and their combinations.\n\nhttps://indico.ific.uv.es/event/617 8/contributions/15667/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15667/ END:VEVENT BEGIN:VEVENT SUMMARY:Massive Neutrino Self-interactions and The Hubble Tension DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15666@indico.ific.uv.es DESCRIPTION:Speakers: Shouvik Roy Choudhury (Indian Institute of Technolog y Bombay)\nBased on: JCAP 03 (2021) 084 (arXiv: 2012.07519)\nWe have updat ed the constraints on flavour universal neutrino self-interactions mediate d by a heavy scalar\, in the effective 4-fermion interaction limit. We use the relaxation time approximation to modify the collisional neutrino Bolt zmann equations\, which is known to be very accurate for this particular s cenario. Based on the latest CMB data from the Planck 2018 data release as well as auxiliary data we confirm the presence of a region in parameter s pace with relatively strong self-interactions which provides a better than naively expected fit. However\, we also find that the most recent data\, in particular high-$\\ell$ polarisation data from the Planck 2018 release\ , disfavours this solution even though it cannot yet be excluded. Our anal ysis takes into account finite neutrino masses (parameterised in terms of $\\sum m_{\\nu}$) and allows for a varying neutrino energy density (parame terised in terms of $N_{\\rm eff}$)\, and we find that in all cases the ne utrino mass bound inferred from cosmological data is robust against the pr esence of neutrino self-interactions. Finally\, we also find that the stro ng neutrino self-interactions do not lead to a high value of $H_0$ being p referred\, i.e. this model is not a viable solution to the current $H_0$ d iscrepancy.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15666/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15666/ END:VEVENT BEGIN:VEVENT SUMMARY:Gerda: Final Results and Physics Beyond Neutrinoless Double-Beta D ecay DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15728@indico.ific.uv.es DESCRIPTION:Speakers: Patrick Krause (Technical University of Munich\, IN FN Roma Tre)\nThe Gerda experiment searched for the lepton number violatin g neutrinoless double-beta (0νββ) decay of 76Ge. Observation of this de cay would provide answers to fundamental problems in particle physics and cosmology\, including the origin of neutrino masses and baryon asymmetry i n the universe. The Gerda experiment achieved the most stringent lower lim it on the half-life of the 0νββ-decay of 1.8 · 10^26 yr at 90% C.L. (w hich coincides with the sensitivity) by operating high-purity germanium (H PGe) detectors enriched in 76Ge submerged in liquid argon (LAr). The colla boration could achieve this breakthrough by reducing the background event rate to 5.2 · 10^−4 counts/(keV kg yr) at the end-point energy. This un precedented background index could be achieved by developing unique techno logies like utilizing the scintillation light of the LAr to reject efficie ntly background events that deposit energy simultaneously in the HPGe dete ctors and in LAr\, and the pulse shape discrimination which exploits speci fic event topologies of backgrounds and signal candidates. Due to the ultr a-low background approach the Gerda data is also suited for other rare eve nt searches beyond the 0νββ decay like the search for super-WIMPs. This talk will present an overview of the Gerda experiment\, its final results and prospects for other physics in the Gerda data.\n\nhttps://indico.ific .uv.es/event/6178/contributions/15728/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15728/ END:VEVENT BEGIN:VEVENT SUMMARY:KamLAND-Zen 800 Status and Progress with the Artificial Intelligen ce Powered Analysis DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15726@indico.ific.uv.es DESCRIPTION:Speakers: Aobo Li (UNC Chapel Hill)\nThe discovery of neutrino less double beta decay (0νββ) would shed light on the persistent puzzle surrounding the origin of neutrino mass and help explain the matter-domin ated universe. KamLAND-Zen is one of the leading experiments searching for 0νββ. The first phase of the experiment\, called KamLAND-Zen 400\, set a world-leading limit on 0νββ lifetime. After the conclusion of KamLAN D-Zen 400\, a brand new mini-balloon with a larger volume and cleaner surf ace were instrumented to contain 745 kg of Xe136. Since Jan. 2019\, KamLAN D-Zen 800 has started data-taking and aims to improve on the previous 0ν ββ result. A detailed study of the backgrounds in this new data will be presented along with a state-of-the-art approach for classifying backgroun ds using a new algorithm called KamNet. The rejection power of KamNet does not rely on coincidence tagging and scales with hardware updates. With th e help of KamNet\, the 0νββ sensitivity of KamLAND-Zen 800 is significa ntly enhanced to a new summit.\n\nhttps://indico.ific.uv.es/event/6178/con tributions/15726/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15726/ END:VEVENT BEGIN:VEVENT SUMMARY:New Results from the CUPID-Mo demonstrator on the 100Mo 0νββ de cay half-life DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15722@indico.ific.uv.es DESCRIPTION:Speakers: Bradford Welliver (LBNL)\nCUPID-Mo served as a succe ssful demonstrator experiment for CUPID (CUORE Upgrade with Particle ID)\, the planned next-generation upgrade of the first ton scale cryogenic calo rimetric $0\\nu\\beta\\beta$ decay experiment\, CUORE (Cryogenic Undergrou nd Observatory for Rare Events). CUPID-Mo was operated at Laboratoire Sout errain de Modane in France as an array of 20 enriched Li$_{2}$$^{100}$MoO$ _{4}$ (LMO) cylindrical scintillating crystals ($\\sim$200g each) each fea turing a Ge light detector (LD) all at $\\sim$20 mK. The LMOs and LDs were instrumented with NTD thermistors allowing for the collection of both hea t and scintillation light. This dual mode of energy collection allows for $\\alpha$ events to be distinguished from $\\beta$/$\\gamma$ events\, sign ificantly reducing the background from degraded $\\alpha$s in the heat cha nnel. CUPID-Mo has a demonstrated energy resolution of $\\sim$7 keV (FWHM) at 2615 keV\, complete $\\alpha$/$(\\beta$/$\\gamma)$ discrimination and very low radioactive contamination. Here we report the results of an analy sis of the full CUPID-Mo exposure\, detailing improved analysis techniques and present an updated limit on the $0\\nu\\beta\\beta$ decay half-life f or $^{100}$Mo. We also will describe the status of other ongoing analysis efforts underway with the CUPID-Mo dataset.\n\nhttps://indico.ific.uv.es/e vent/6178/contributions/15722/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15722/ END:VEVENT BEGIN:VEVENT SUMMARY:The neutrinoless double beta decay CROSS experiment: demonstrator with surface sensitive bolometers DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15717@indico.ific.uv.es DESCRIPTION:Speakers: Anastasiia Zolotarova (CNRS/IJCLab)\nNowadays\, doub le beta decay searches are an important point of interest in neutrino phys ics: the observation of neutrinoless double beta (0$\\nu$2$\\beta$) decay will give essential information on neutrino masses and nature as well as o n lepton number violation. The technological challenge for highly sensitiv e 0$\\nu$2$\\beta$ experiments includes the minimization of the background index in the region of interest. The key feature of CROSS (Cryogenic Rare -event Observatory with Surface Sensitivity) is the active surface backgro und rejection using bolometric detectors coated with thin metallic films. Such a film on the detector surface affects the conversion of the energy d eposited by the particle interaction. The phonon reabsorbtion in the film leads to a modification of the pulse shape for close-to-film events. With single-channel separation of surface $\\alpha$ and $\\beta$ particles\, th e CROSS technology can be used for next-generation bolometric experiments\ , reaching a background index in the region of interest of $\\sim$10$^{-5} $ counts/(keV$\\times$kg$\\times$y).\n\nSeveral series of reduced-scale pr ototypes with coated Li$_2$MoO$_4$ and TeO$_2$ crystals (isotopes of inter est for 0$\\nu$2$\\beta$ are $^{100}$Mo and $^{130}$Te) were studied in an aboveground cryostat at IJCLab\, Orsay.\nSuccessful observation of surfac e alpha and beta separation with Pd-Al grids was performed\, and first ful l-size (45x45x45 mm\, $\\sim$280 g) prototypes based on a Li$_2$$^{100}$Mo O$_4$ crystal for the CROSS demonstrator were assembled.\n\nThe surface-ev ent identification can be combined with alpha particle rejection achievabl e in scintillating bolometers\, providing a powerful redundancy for backgr ound mitigation. In this framework\, the underground cryogenic facility of CROSS (Canfranc Underground laboratory) hosted several arrays of Li$_2$$^ {100}$MoO$_4$ scintillating bolometers (in collaboration with CUPID experi ment) to perform studies of detectors performance and reproducibility. Sev eral options for light collection optimization were investigated\, with li ght yields ranging from $\\sim$0.2 to $\\sim$0.6 keV/MeV. These results ar e used for the optimization of the detector modules both for the CUPID exp eriment and the CROSS demonstrator\, which will consist of an array of abo ut 60 crystals of Li$_2$MoO$_4$ containing 6.6 kg of $^{100}$Mo featuring both light-yield and pulse-shape discrimination capabilities. The 2 year s ensitivity of the CROSS demonstrator is 2$\\times$10$^{25}$ years\, corres ponding to effective neutrino mass bounds of 86 - 149 meV.\n\nhttps://indi co.ific.uv.es/event/6178/contributions/15717/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15717/ END:VEVENT BEGIN:VEVENT SUMMARY:BINGO: Bi-Isotope 0ν2β Next Generation Observatory DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15716@indico.ific.uv.es DESCRIPTION:Speakers: Claudia Nones (IRFU/DPhP)\nNeutrinoless double-beta decay (0ν2β) is a hypothetical rare nuclear transition. Its observation would provide an important insight about the nature of neutrinos (Dirac or Majorana particle) demonstrating that the lepton number is not conserved. BINGO aims to set the technological and conceptual grounds for future bol ometric 0ν2β experiments. It is based on a dual heat-light readout\, i.e . a main absorber embedding the double-beta decay isotope faced by a light detector. Dual heat-light readout helps to reject the α background compo nent\, thanks to the lower light output of α’s compared to β/γ’s. B INGO will study two of the most promising isotopes: 100Mo embedded in Li2M oO4 and 130Te embedded in TeO2. BINGO’s proposed technology aims at red ucing dramatically the background in the region of interest\, thus boostin g the discovery sensitivity of 0νββ. This can be achieved by fulfilling the following goals: (i) increasing the light detector sensitivity thanks to Neganov-Luke amplification\; (ii) having a revolutionary detector asse mbly that will reduce the total surface radioactivity contribution\; (iii) using an active shield\, based on ZnWO4 or BGO scintillators with bolomet ric readout\, to suppress the external gamma background. The proposed solu tions will have a high impact on next-generation bolometric tonne-scale ex periments.\nIn this contribution we present the first results on the revol utionary assembly and on the bolometric veto.\n\nhttps://indico.ific.uv.es /event/6178/contributions/15716/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15716/ END:VEVENT BEGIN:VEVENT SUMMARY:Barium Tagging for the NEXT Neutrinoless Double Beta Decay Program DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15698@indico.ific.uv.es DESCRIPTION:Speakers: Ben Jones (UTA)\nThe NEXT collaboration is pursuing a phased program to search for neutrinoless double beta decay (0nubb) usin g high pressure xenon gas time projection chambers. The power of electrol uminescent xenon gas TPCs for 0nubb derives from their excellent energy re solution (\n\nhttps://indico.ific.uv.es/event/6178/contributions/15698/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15698/ END:VEVENT BEGIN:VEVENT SUMMARY:Latest results of the R2D2 project towards a possible future neutr ino double beta decay experiment DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15694@indico.ific.uv.es DESCRIPTION:Speakers: Ioannis Katsioulas (University of Birmingham)\nThe s earch for neutrinoless double beta decay could cast light on one critical piece missing in our knowledge i.e. the nature of the neutrino mass. Its o bservation is indeed the most sensitive experimental way to prove that neu trino is a Majorana particle. The observation of such a potentially rare p rocess demands a detector with an excellent energy resolution\, an extreme ly low radioactivity and a large mass of emitter isotope. Nowadays many te chniques are pursued but none of them meets all the requirements at the sa me time. The goal of R2D2 is to prove that a spherical high pressure TPC c ould meet all the requirements and provide an ideal detector for the 0νβ β decay search. The prototype has demonstrated an excellent resolution wi th Argon and the preliminary results with Xenon are already very promising . In the proposed talk the R2D2 results obtained with the first prototype will be discussed as well as the project roadmap and future developments.\ n\nhttps://indico.ific.uv.es/event/6178/contributions/15694/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15694/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of the 136Xe two-neutrino double beta decay half-life with NEXT-White DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15584@indico.ific.uv.es DESCRIPTION:Speakers: Alberto Usón (IFIC (CSIC-Univ Valencia))\nThe NEXT (Neutrino Experiment with a Xenon TPC) collaboration searches for the neut rino-less double beta decay (ββ0ν) of 136Xe at the Laboratorio Subterr áneo de Canfranc (LSC) (Huesca\, Spain). The observation of such a lepton -number-violation process would prove the Majorana nature of neutrinos\, p roviding also information on the neutrino mass scale. A first large-scale prototype of a high-pressure Xenon gas electroluminescent TPC\, NEXT-White \, is being operated at the LSC since 2016. This 5-kg radiopure detector h as already proven an outstanding performance of the NEXT technology in ter ms of the energy resolution (\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15584/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15584/ END:VEVENT BEGIN:VEVENT SUMMARY:nEXO: Search for Neutrino-less Double Beta Decay at the Tonne Scal e DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15490@indico.ific.uv.es DESCRIPTION:Speakers: Ako Jamil (Yale University)\nnEXO is a 5 tonne monol ithic liquid xenon (LXe) time projection chamber (TPC) planned to search f or the neutrinoless double beta decay of $^{136}$Xe with an estimated half -life sensitivity of $> 10^{28}$ years at 90% C.L.. Advancements were made in terms of detector design\, signal modelling and data analysis to suppo rt a refined estimate of the sensitivity and discovery potential of the nE XO experiment. In particular\, we updated the detector geometry in line wi th most recent advancements in our engineering design\, we implemented a m ore realistic and data-driven modelling of the light and charge channel si gnals and developed a Deep Neutral Network based analysis to discriminate between signal and background. This talk will cover the simulation\, recon struction and the physics reach of nEXO.\n\nhttps://indico.ific.uv.es/even t/6178/contributions/15490/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15490/ END:VEVENT BEGIN:VEVENT SUMMARY:Prospects of neutrinoless double beta decay search with PandaX-4T and beyond DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15489@indico.ific.uv.es DESCRIPTION:Speakers: Ke Han (Shanghai Jiao Tong University)\nLarge liquid xenon Time Projection Chambers (TPC) with multi-ton of active mass\, such as PandaX-4T\, have hundreds of kilogram of Xe-136 and can be used to se arch for neutrinoless double beta decay (NLDBD). PandaX-4T is taking commi ssioning data as for now at China JinPing Underground Laboratory (CJPL). We will present the detector performance at high energy and the physics po tential to search for NLDBD. Next generation of xenon TPC with even large r target may reach the inverted mass hierarchy of effective Majorana neutr ino mass.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15489/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15489/ END:VEVENT BEGIN:VEVENT SUMMARY:The ultimate limit on 82Se neutrinoless double-beta decay search w ith CUPID-0 DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15485@indico.ific.uv.es DESCRIPTION:Speakers: Lorenzo Pagnanini (INFN - LNGS & GSSI)\nCUPID-0 is t he first pilot experiment of CUPID\, a next-generation project to search f or neutrinoless double beta decay (0νDBD) with scintillating bolometers.\ n\nThe detector\, consisting of 24 enriched and 2 natural ZnSe crystals\, has been taking data at Laboratori Nazionali del Gran Sasso from March 201 7 to December 2018 (Phase I) and from May 2019 to February 2020 (Phase II) \, for a total exposure of 16.59 kg yr of ZnSe. \nIn this contribution\, w e present the new combined results of Phase-I and Phase II in the search f or Se-82 0νDBD\, both to the ground state and to the excited states of Kr -82.\nThe successful operation of the CUPID-0 detector demonstrates that s cintillating calorimeters allow us to reach the lowest background for calo rimetric experiments: (3.5+1.0−0.9)×10−3 counts/(keV kg yr).\nWe re ach a 90% credible interval median sensitivity of $0.7~\\times~10^{25}$ yr and set the most stringent limit on the half-life of Se-82 0vDBD\, $T_{1/ 2}^{0\\nu} > 4.7~\\times~10^{24}$ yr (90% credible interval)\, correspo nding to $m_{\\beta\\beta} \n\nhttps://indico.ific.uv.es/event/6178/contri butions/15485/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15485/ END:VEVENT BEGIN:VEVENT SUMMARY:The MAJORANA DEMONSTRATOR's Search for Neutrinoless Double-Beta De cay DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15483@indico.ific.uv.es DESCRIPTION:Speakers: Julieta Gruszko (Univ North Carolina)\nThe MAJORANA DEMONSTRATOR has recently completed data-taking for its search for neutrin oless double-beta decay ($0\\nu\\beta\\beta$) in $^{76}$Ge. \nIf observed\ , this beyond the standard model process that would prove the neutrino is a Majorana fermion and provide a path to leptogenesis in the early univers e.\nThe experiment has completed operation of a modular array of 44 kg of high purity germanium detectors\, in the p-type point contact (PPC)\, inve rted-coaxial point-contact (ICPC)\, and broad energy germanium (BEGe) geom etries.\n30 kg of PPC and 6 kg of ICPC detectors belonging to the LEGEND e xperiment were enriched to 88% in $^{76}$Ge.\nAfter removing the enriched detectors in March of 2021 for future operation in LEGEND-200\, the experi ment is continuing to operate 23 BEGe detectors with natural isotopic abun dance.\nTo minimize backgrounds\, the DEMONSTRATOR is constructed from low -background materials and housed inside a compact shield consisting of lea d and copper at the Sanford Underground Research Facility (SURF) in Lead\, SD.\nEach of the detector geometries enable the use of pulse shape discri mination techniques that can reject multi-site and surface backgrounds.\nF urthermore\, the experiment has achieved a leading energy resolution of 0. 12% FWHM at 2039 keV.\nThis talk will provide an update on recent improvem ents to the MAJORANA analysis and future plans for the experiment.\n\nThis material is based upon work supported by the U.S. Department of Energy\, Office of Science\, Office of Nuclear Physics\, the Particle Astrophysics and Nuclear Physics Programs of the National Science Foundation\, and the Sanford Underground Research Facility.\n\nhttps://indico.ific.uv.es/event/ 6178/contributions/15483/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15483/ END:VEVENT BEGIN:VEVENT SUMMARY:SNO+ DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15482@indico.ific.uv.es DESCRIPTION:Speakers: Mark Chen (Queen's University)\nSNO+ is a multi-purp ose neutrino experiment located at SNOLAB. Now filled with liquid scintill ator after a challenging campaign of operations during the pandemic\, SNO+ is studying backgrounds in the detector and embarking on a neutrino physi cs program including reactor\, geo and solar neutrinos. The ultimate goal of SNO+ is to deploy roughly 4 tonnes of tellurium (0.5%) in the scintilla tor to conduct a neutrinoless double beta decay search. This talk will pre sent the prospects and a preliminary look at data from SNO+.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15482/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15482/ END:VEVENT BEGIN:VEVENT SUMMARY:CUPID: a next generation bolometric neutrinoless double beta decay experiment DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15480@indico.ific.uv.es DESCRIPTION:Speakers: Jonathan L. Ouellet (MIT)\nCUPID is a next-generatio n tonne-scale bolometric neutrinoless double beta decay experiment to prob e the Majorana nature of neutrinos and discover Lepton Number Violation if the effective neutrino mass is greater than 10 meV. CUPID will be built o n experience\, expertise and lessons learned in CUORE\, and will be instal led in the current CUORE infrastructure in the Gran Sasso underground labo ratory. The CUPID detector technology\, successfully tested in the CUPID-M o experiment\, is\nbased on scintillating bolometers of Li2MoO4 enriched i n the isotope of interest 100Mo. In order to achieve its ambitious science goals\, CUPID aims to reduce the backgrounds in the region of interest by a factor 100 with respect to CUORE. This performance will be achieved by introducing the high efficiently alpha/beta discrimination demonstrated by the\nCUPID-0 and CUPID-Mo experiments\, and using a high transition energ y double beta decay nucleus such as 100Mo to minimize the impact of the ga mma background. CUPID will consist of about 1500 hybrid heat-light detecto rs for a total isotope mass of 250 kg. The CUPID scientific reach is suppo rted by a detailed and safe background model that uses CUORE\, CUPID-Mo an d CUPID-0 results. The required performance in terms of energy resolution\ , alpha rejection factor and crystal purity have already been demonstrated and will be presented.\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15480/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15480/ END:VEVENT BEGIN:VEVENT SUMMARY:Light only Liquid Xenon (LoLX) experiment DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15479@indico.ific.uv.es DESCRIPTION:Speakers: Liang Xie (TRIUMF)\nThe Light only Liquid Xenon (LoL X) experiment was designed to study light production in liquid xenon durin g the first nanosecond and gain experience with the operation of a large n umber of closely spaced Silicon Photomultipliers (SiPMs) in liquid xenon. The LoLX detector is a 3D printed octagonal chamber housing 96 Hamamatsu V UV4 SiPMs\, 16 on top and bottom and 8 on each side of the octagon. A β-s ource Sr-90 is inserted in the middle of the chamber. Most (88) SiPMs are covered by long pass filters preventing transmission of light below 225nm\ , and are to be used for isolating the Cerenkov light. 4 SiPMs are uncover ed and 4 are covered by a band pass filter centered at the xenon scintilla tion wavelength. Results will be presented including a measure of the beta decays with the combined scintillation and Cerenkov channels. The focus o f the current phase of the experiment is to demonstrate spectral separatio n of Cerenkov and scintillation which is a prerequisite for studying scint illation during the first ns. LoLX will be upgraded in 2021 to achieve abo ut 100ps timing resolution as opposed to about 1ns currently achieved. Eve ntually digital SiPMs will be used in an attempt to reach 10ps single phot on timing resolution. The LoLX results will also include a study of SiPM e xternal cross-talk\, where photons produced by a charge avalanche in a SiP M trigger an avalanche in another. The unique shape of the chamber offers opportunity to study external crosstalk at varying angles and distances. N ot only will LoLX results help predict the performances of the nEXO experi ment but also determine if early light measurement carry valuable informat ion for better timing and possibly energy resolutions\, to improve particl e identification.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15 479/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15479/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of AMoRE DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15478@indico.ific.uv.es DESCRIPTION:Speakers: Yoomin Oh (Center for Underground Physics\, Institut e for Basic Science)\nAMoRE is a search for neutrinoless double beta decay using Mo-100 enriched crystal scintillators at an ultra-low temperature. We have understood the major background sources and how they can be reduce d from a pilot stage run in the Yangyang underground laboratory. AMoRE-I i s currently running with twelve $^{48\\textrm{depl}}$Ca$^{100}$MoO$_{4}$ a nd five Li$_{2}^{100}$MoO$_{4}$ crystals with a total mass of enriched $^{ 100}$Mo 2.8 kg. The detector design for the main stage of the experiment\, AMoRE-II\, has been finalized and the detector is under construction in Y emiLab\, a new underground laboratory located in an iron mine with an aver age depth 2500 meter of water equivalent. The status of AMoRE-I and the pr eparations for AMoRE-II will be presented.\n\nhttps://indico.ific.uv.es/ev ent/6178/contributions/15478/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15478/ END:VEVENT BEGIN:VEVENT SUMMARY:The LEGEND program - search for neutrinoless double beta decay in Ge-76 DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15475@indico.ific.uv.es DESCRIPTION:Speakers: Ralph Massarczyk (Los Alamos National Laboratory)\nT he Large Enriched Germanium Experiment for Neutrinoless $\\beta\\beta$ Dec ay (LEGEND) is a phased experimental effort to search for neutrinoless dou ble-beta decay in $^{76}$Ge. The first phase uses existing resources build ing off the experiences of the Majorana and GERDA experiments\, as well as new techniques like larger inverted coaxial detectors and an improved Arg on detector system. It consists of 200 kg of $^{76}$Ge enriched germanium\ , and assembly and testing of components has begun. The collaboration is p lanning to start commissioning in the second half of this year. I will giv e an overview on the status of the effort and also on its proposed success or\, LEGEND-1000. My presentation will also cover LEGENDs physics reach\, its design\, its ongoing R\\&D\, and further efforts that are necessary to deploy an experiment with an half-life discovery potential of beyond 10$^ {28}$ years half-life for neutrinoless double beta decay. \n\n*This work i s supported by the U.S. DOE\, and the NSF\, the LANL\, ORNL and LBNL LDRD programs\; the European ERC and Horizon programs\; the German DFG\, BMBF\, and MPG\; the Italian INFN\; the Polish NCN and MNiSW\; the Czech MEYS\; the Slovak SRDA\; the Swiss SNF\; the UK STFC\; the Russian RFBR\; the Can adian NSERC and CFI\; the LNGS and SURF facilities.\nLA-UR-21-26052\n\nhtt ps://indico.ific.uv.es/event/6178/contributions/15475/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15475/ END:VEVENT BEGIN:VEVENT SUMMARY:CDEX-300ν: neutrinoless double beta decay experiment based on 76G e DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15473@indico.ific.uv.es DESCRIPTION:Speakers: Qian Yue ()\nNeutrinoless double beta decay has been a key topic that could help scientists to understand the properties of th e neutrino including whether the neutrino is its own antiparticle\, lepton number violation and so on. The China Dark Matter Experiment (CDEX) aims at direct searches of light Weakly Interacting Massive Particles (WIMPs) a nd neutrinoless double beta decay experiment at the China Jinping Undergro und Laboratory (CJPL) based on germanium detector array. From 2021 on\, CD EX collaboration is pushing forward to setup a CDEX-300ν experiment based on 76Ge-enriched germanium array detector system to search neutrinoless d ouble beta decays of 76Ge isotope. CDEX-300ν detector system will include s a 76Ge-enriched germanium array detector system with total mass of 300 k g and the germanium detectors are immersed into a liquid argon cooling and active shielding system with volume of ~8 m³. The liquid argon tank is l ocated into a liquid nitrogen tank with a volume of 1725 m³ for cooling d own and further decreasing the ambient radioactive backgrounds. More detai ls of CDEX-300ν will be introduced in this talk.\n\nhttps://indico.ific.u v.es/event/6178/contributions/15473/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15473/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of 48Ca double beta decay search in CANDLES DTSTART;VALUE=DATE-TIME:20210831T162500Z DTEND;VALUE=DATE-TIME:20210831T164000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15472@indico.ific.uv.es DESCRIPTION:Speakers: Yuto Minami (RCNP\, Osaka Univ.)\nThe origin of neut rino masses is one of the unsolved puzzles in particle physics. One possib ility is that neutrinos have Majorana masses.We can test the Majorana natu re of neutrinos by searching for neutrinoless double-beta decay ($0\\nu\\b eta\\beta$) events.CANDLE is a project which targets $0\\nu\\beta\\beta$ e vents from ${}^{48}$Ca using its high Q$_{\\beta\\beta}$-value of $4.27\\\ ,$MeV. We developed a CANDLES-III system with 96 $\\mathrm{CaF}_2$ scintil lation crystals with natural Ca isotope\, which corresponds to $350\\\,$g of ${}^{48}$Ca.The key to search for $0\\nu\\beta\\beta$ with the CANDLES- III is to identify and remove the $\\beta$ decay background events from im purities in $\\mathrm{CaF}_2$ crystals. Especially\, $\\beta$ decay events from ${}^{208}$Tl with Q$_{\\beta}$-value of $5.0\\\,$MeV are dominant ba ckground events.\nIn the proposed talk\, an improved sensitivity by a new ${}^{208}$Tl background removal method and the latest results of the searc h for $0\\nu\\beta\\beta$ will be discussed.\n\nhttps://indico.ific.uv.es/ event/6178/contributions/15472/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15472/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for double beta decay of 106Cd with TGV-2 spectrometer DTSTART;VALUE=DATE-TIME:20210831T161000Z DTEND;VALUE=DATE-TIME:20210831T162500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15471@indico.ific.uv.es DESCRIPTION:Speakers: Nikolay Rukhadze (Joint Institute for Nuclear Resear ch)\nSearch for double beta decay processes (EC/EC\, β+/EC\, β+β+) of 1 06Cd was performed at the Modane underground laboratory (LSM\, France\, 48 00 m w.e.) using the low-background multi–detector spectrometer TGV-2 an d enriched 106Cd. The detector part of the TGV-2 is composed of 32 HPGe p lanar type detectors with the sensitive volume of 2040 mm2 x 6 mm each. Th e total sensitive volume of the detectors is about 400 cm3. TGV-2 detector s are arranged in 16 sandwich-like pairs of face-to-face detectors with 16 thin double beta emitters placed between them. The total mass of 16 inves tigated 106Cd foils (with an enrichment of 99.57% of 106Cd) have a total m ass of ~23.2 g. The distance between the detectors and the emitters is 20 cm)\, a steel airtight box against radon\, a lead shielding (> 10 cm)\, a nd a neutron shielding made from borated polyethylene (16 cm).The TGV-2 sp ectrometer provides a high possibility of detection of double beta process es in 106Cd. Experiment started in February 2014. The preliminary results of data accumulated during 42500h will be presented with sensitivity level of T1/2 ~1×10^21 y at 90% C.L.\n\nhttps://indico.ific.uv.es/event/6178/c ontributions/15471/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15471/ END:VEVENT BEGIN:VEVENT SUMMARY:Exposure-background duality in the searches of neutrinoless double beta decay DTSTART;VALUE=DATE-TIME:20210831T152500Z DTEND;VALUE=DATE-TIME:20210831T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15465@indico.ific.uv.es DESCRIPTION:Speakers: Manoj Kumar Singh (Institute of Physics\, Academia S inica)\nNeutrinoless double-$\\beta$ decay (0$\\nu\\beta\\beta$) is an exp erimentally sensitive avenue to probe the nature (Majorana versus Dirac) a nd exact mass of neutrinos. This work [1] quantitatively explores the inte rplay between exposure and background levels in 0$\\nu\\beta\\beta$ experi ments at their design stage. In particular\, background reduction will be playing increasingly important and investment-effective roles in future 0$ \\nu\\beta\\beta$ experiments. Although the primary goal of current runnin g and projected experiments is to probe the inverted mass hierarchy\, curr ent neutrino oscillation experiments reveal a preference for non-degenerat e (ND) normal mass hierarchy (NH). Therefore the strategy of scaling the s ummit of 0$\\nu\\beta\\beta$ should also take this genuine possibility int o account. Present work would explore the role of background suppression i n alleviating the necessity of large exposure for future 0$\\nu\\beta\\bet a$ experiments with sensitivity goals of approaching and covering ND-NH. I n particular\, the roles of energy resolution in suppressing the irreducib le background of 2$\\nu\\beta\\beta$ will be discussed.\n\n[1] M.K.Singh e t al.\, Phys. Rev. D 101\, 013006 (2020).\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15465/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15465/ END:VEVENT BEGIN:VEVENT SUMMARY:Latest results from the CUORE experiment DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15456@indico.ific.uv.es DESCRIPTION:Speakers: Matteo Biassoni (INFN Milano Bicocca)\nThe Cryogenic Underground Observatory for Rare Events (CUORE) is the first bolometric e xperiment searching for 0νββ decay that has been able to reach the one- tonne mass scale. The detector\, located at the LNGS in Italy\, consists o f an array of 988 TeO2 crystals arranged in a compact cylindrical structur e of 19 towers. CUORE began its first physics data run in 2017 at a base t emperature of about 10 mK and in April 2021 released its 3rd result of the search for 0νββ\, corresponding to a tonne-year of TeO2 exposure. Thi s is the largest amount of data ever acquired with a solid state detector and the most sensitive measurement of 0νββ decay in 130Te ever conducte d\, with a median exclusion sensitivity of 2.8×10^25 yr. We find no evide nce of 0νββ decay and set a lower bound of 2.2 ×10^25 yr at a 90% cred ibility interval on the 130Te half-life for this process. In this talk\, w e present the current status of CUORE search for 0νββ with the updated statistics of one tonne-yr. We finally give an update of the CUORE backgro und model and the measurement of the 130Te 2νββ decay half-life\, study performed using an exposure of 300.7 kg⋅yr.\n\nhttps://indico.ific.uv.e s/event/6178/contributions/15456/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15456/ END:VEVENT BEGIN:VEVENT SUMMARY:CUTE : A Cryogenic Underground Test Facility at SNOLAB DTSTART;VALUE=DATE-TIME:20210831T120000Z DTEND;VALUE=DATE-TIME:20210831T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15938@indico.ific.uv.es DESCRIPTION:Speakers: Andrew Kubik (SNOLAB)\nOperational since 2019\, the Cryogenic Underground TEst (CUTE) facility is located 2 km underground in the SNOLAB laboratory near Sudbury Ontario\, Canada. Although designed wit h the focus of performance testing cryogenic (~ 10 mK) detectors for the S uper Cryogenic Dark Matter Search (SuperCDMS)\, CUTE also makes available a well shielded and vibrationally isolated underground platform for other cryogenic detectors or projects which may benefit from such a low backgrou nd underground facility. The main features and performance of the CUTE fa cility will be discussed\, as well as some examples of devices and detecto rs which have been or are planned to be tested at CUTE.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15938/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15938/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of the neutron flux at the Canfranc Underground Labora tory with HENSA DTSTART;VALUE=DATE-TIME:20210831T114500Z DTEND;VALUE=DATE-TIME:20210831T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15937@indico.ific.uv.es DESCRIPTION:Speakers: Sonja Orrigo (IFIC (CSIC-Univ Valencia))\nS.E.A. Orr igo\, J.L. Tain\, J. Agramunt\, A. Algora\, E. Nacher\, A. Tolosa\n*Instit uto de Física Corpuscular (IFIC)\, CSIC-Univ. Valencia\, Spain*\n\nA. Ta rifeño-Saldivia\, F. Calviño\, N. Mont\, A. De Blas\, R. García\, G. Co rtés \n*Institute of Energy Technologies (INTE)\, Technical University of Catalonia (UPC)\, Barcelona\, Spain*\n\nL.M. Fraile\, A. Domínguez Bugar ín\n*Grupo de Física Nuclear & IPARCOS\, Universidad Complutense de Madr id (UCM)\, Madrid\, Spain*\n\nD. Bemmerer\, M. Grieger\n*Helmholtz-Zentrum Dresden-Rossendorf (HZDR)\, 01328 Dresden\, Germany*\n\nI. Dillmann\n*TRI UMF\, 4004 Wesbrook Mall\, Vancouver\, British Columbia V6T 2A3\, Canada*\ n\nNeutrons constitute a main limitation for experiments dealing with rare event searches underground. Even if neutrons produced by cosmic-ray muons are largely suppressed in underground laboratories\, radiogenic neutrons are still produced in the rocks by (alpha\,n) reactions and spontaneous fi ssion. They have a large penetrability and can induce background signals i n the detectors [1\,2] affecting nuclear astrophysics\, neutrino and dark matter experiments.\n\nTherefore it is of paramount importance to measure and fully characterize the neutron flux at the experimental location. Sinc e the neutron background in underground laboratories is low\, measurements have a low rate and last for months\, demanding detectors with high effic iency for neutrons\, high background discrimination capability and long-te rm stability. These requirements are fulfilled by 3He proportional counter s [2-6]. The new High Efficiency Neutron-Spectrometry Array (HENSA)\, base d on the Bonner spheres principle [3]\, is composed of ten long proportion al counters filled with 3He gas embedded in high-density polyethylene mode rators with different thickness\, achieving sensitivity to neutron energie s ranging from thermal to 10 GeV.\n\nIn October 2019 we started a long-ter m measurement of the neutron flux with HENSA in the Hall A of the Canfranc Underground Laboratory (LSC). The aim is to measure the neutron flux and characterize the energy spectrum precisely as well as to study the long-te rm evolution of the neutron rate looking for possible seasonal variations. These goals are of relevance for a number of experiments at LSC investiga ting fundamental questions of modern physics [7\,8]. The Hall A measuremen t campaign extended up to March 2021\, demonstrating an excellent stabilit y of the HENSA setup. Results from the campaign in Hall A will be presente d for the first time at the TAUP conference.\n\n[1] E. Aprile et al.\, J. Phys. G 40\, 115201 (2013)\n[2] J.L. Tain et al.\, J. Phys. Conf. Series 6 65\, 012031 (2016)\n[3] D.J. Thomas and A.V. Alevra\, Nucl. Instr. Meth. A 476\, 12 (2002)\n[4] D. Jordan et al.\, Astrop. Phys. 42\, 1 (2013)\n[5] D. Jordan et al.\, Astrop. Phys. 118\, 102372 (2020) \n[6] M. Grieger et a l.\, Phys. Rev. D 101\, 123027 (2020)\n[7] A. Ianni\, J. Phys. Conf. Serie s 718\, 042030 (2016)\n[8] LSC Annual Report (2018)\n\nhttps://indico.ific .uv.es/event/6178/contributions/15937/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15937/ END:VEVENT BEGIN:VEVENT SUMMARY:The Boulby Underground Screening (BUGS) Facility DTSTART;VALUE=DATE-TIME:20210831T113000Z DTEND;VALUE=DATE-TIME:20210831T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15929@indico.ific.uv.es DESCRIPTION:Speakers: Paul Scovell (STFC - Boulby Underground Laboratory)\ nThe Boulby Underground Screening (BUGS) facility has been in operation si nce 2014. Initially comprising 2 low background germanium detectors\, this has expanded to include now 6 low and ultra-low background germanium dete ctors\, two XIA Ultralo-1800 detectors and will soon include a low backgro und radon emanation assay facility. With these facilities underground and with plans for cleanliness R&D facilities on the surface we are aiming to position BUGS as a facility that offers everything needed for material cha racterisation in current and next generation low-background particle physi cs experiments. This talk will introduce the facility and discuss the curr ent status and plans for the future.\n\nhttps://indico.ific.uv.es/event/61 78/contributions/15929/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15929/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for Dark Matter with the PICO-500 Experiment DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15914@indico.ific.uv.es DESCRIPTION:Speakers: Guillaume Giroux (Queen's University)\nThe PICO coll aboration searches for WIMPs using large superheated liquid detectors\, or bubble chambers. Recent results from the complete exposure of the PICO-60 C$_3$F$_8$ detector at SNOLAB set the world’s most stringent limits on WIMP-proton spin-dependent interactions. I will present the current status of the construction and physics potential of the next generation\, tonne- scale experiment at SNOLAB: PICO-500.\n\nhttps://indico.ific.uv.es/event/6 178/contributions/15914/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15914/ END:VEVENT BEGIN:VEVENT SUMMARY:Investigating WIMPs with XENONnT DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15899@indico.ific.uv.es DESCRIPTION:Speakers: Jacques Pienaar (University of Chicago)\nThe multi-t onne XENONnT detector is the next step in the evolution of the XENON proje ct. The experiment\, aimed at direct detection of WIMPs\, utilizes 5.9t of instrumented liquid xenon. Dedicated screening results of all detector ma terials were used to project the expected overall background in the detect or\, while improvements in suppressing intrinsic backgrounds from electron ic recoil sources will allow XENONnT to reduce this background to an expec ted level 1/6th that of its predecessor within a 4t fiducial volume. The a ddition of a neutron veto around the XENONnT cryostat allows for significa nt suppression of the overall neutron background as well. XENONnT is aimed at achieving a 20 t.y exposure over its lifetime. In this talk I will pre sent the sensitivity to spin-dependent and -independent WIMP nucleon inter actions. In the case of spin-independent interactions\, the sensitivity wi ll reach a cross-section of $1.4\\times10^{-48}\\\,\\mathrm{cm}^2$ for a 5 0\\\,GeV/c$^2$ mass WIMP at 90% confidence level\, more than one order of magnitude beyond the current best limits.\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15899/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15899/ END:VEVENT BEGIN:VEVENT SUMMARY:Acoustic response of nuclear recoils in bubble chambers DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15898@indico.ific.uv.es DESCRIPTION:Speakers: Benjamin Broerman (Queen's University)\nThe bubble c hambers of the PICO collaboration use the acoustic signal generated from n ucleations to classify nuclear recoil events from alpha decays in the bulk fluid. The success of these detectors in probing the potential WIMP-proto n cross section comes in part from the low energy threshold that can be ac hieved. This nucleation threshold\, based on the Seitz model\, is dependen t on fluid type\, pressure\, and temperature. At higher thresholds bubble nucleation does occur but with a significant loss in the measurable acoust ic signal. To investigate this\, the acoustic response of bulk nuclear rec oil events was measured as a function of pressure and temperature and foun d to depend exponentially on both parameters. Understanding the form of th e acoustic response can be used to predict potential operating conditions for specific thresholds in future larger-scale superheated liquid detector s. Details of the measurement in a small-scale test setup and a comparison to existing data will be presented.\n\nhttps://indico.ific.uv.es/event/61 78/contributions/15898/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15898/ END:VEVENT BEGIN:VEVENT SUMMARY:A look at the PandaX-4T commissioning data DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15897@indico.ific.uv.es DESCRIPTION:Speakers: Yi Tao (Shanghai Jiao Tong University)\nAfter PandaX -II experiment\, we started to build PandaX-4T detector with 4 ton liquid xenon in the sensitive volume at China Jinping Underground laboratory. PandaX-4T experiment has completed detector construction\, and detector c ommissioning has begun since the end of the year 2020. Through the commi ssioning\, we are optimizing the detector operation conditions\, testing various calibration sources including the newly installed DD neutron sou rce\, developing detector response model and signal reconstruction algori thm. In this talk\, I will give an overview of the commissioning data an d detector performance.\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15897/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15897/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent progress of PandaX-4T experiment DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15894@indico.ific.uv.es DESCRIPTION:Speakers: Qing Lin (University of Science and Technology of Ch ina)\nPandaX-4T is a tonne-scale dark matter direct searching experiment\ , utilizing 4 tonne liquid xenon as target material in sensitive volume.   The experiment is located at China Jinping Underground Laboratory\, with overburden of 2400 meter water equivalent. Recently\, the PandaX-4T experiment has finished assembling on site\, and started commissioning o f the sub-systems. In this talk\, I will talk about the status and perform ances of major sub-systems of PandaX-4T as well as the ongoing commission ing runs.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15894/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15894/ END:VEVENT BEGIN:VEVENT SUMMARY:DEAP-3600 constraints on dark matter effective interactions and ha lo substructures DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15874@indico.ific.uv.es DESCRIPTION:Speakers: Ariel Zuñiga Reyes (Universidad Nacional Autónoma de México (UNAM))\nThe WIMP search in 231 live-days of data collected by the DEAP-3600 experiment showed no event candidates\, resulting in a world -leading upper limit on the spin-independent dark matter-nucleon cross-sec tion for an argon target. The present study reanalyzed that null result wi thin a Non-Relativistic Effective Field Theory (NREFT) framework\, and fur ther examined the impact of potential dark matter halo substructures motiv ated by the observations of stellar distributions from the Gaia satellite and other astronomical surveys. Constraints were set on the coupling stren gth of the effective operators O1\, O3\, O5\, O8\, and O11\, considering i soscalar\, isovector\, and xenonphobic scenarios\, as well as on the NREFT -derived specific interactions: millicharge\, magnetic dipole\, electric d ipole\, and anapole. The effects of halo substructures on each of the oper ators was explored as well\, showing that the O5 and O8 operators are part icularly sensitive to the velocity distribution\, even for heavy WIMPs.\n\ nhttps://indico.ific.uv.es/event/6178/contributions/15874/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15874/ END:VEVENT BEGIN:VEVENT SUMMARY:Detection Of Heavy Dark Matter Particles In DEAP-3600 DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15872@indico.ific.uv.es DESCRIPTION:Speakers: Michela Lai (University of Cagliari)\nDEAP-3600\, ho sted at SNOLAB\, has been designed for the search of WIMPs\, Weakly Intera cting Massive Particles\; its target of 3.3 t of liquid argon makes it the largest direct detection experiment. In addition to its sensitivity to WI MPs\, DEAP-3600 is sensitive to super-massive dark matter candidates with masses up to the Planck scale. For particles with masses above 10^{16} GeV and cross-sections with argon above 10^{-24} cm^2\, these dark matter par ticles are expected to reach an underground experiment and give a detectab le signal in liquid argon. Due to the large cross-section\, the expected s ignal in DEAP-3600 is a collinear sequence of nuclear recoils in the same acquisition window\, giving a very distinguishable and unique signature\; hence\, we refer to them as Multi-Scattering Heavy Dark Matter Particles. \nIn this talk\, the search for this candidate in three years of data-taki ng is presented\, starting from the expected signal compared to the expect ed background\, and Monte Carlo model developed\; then\, the results of th e unblinding procedure will be presented.\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15872/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15872/ END:VEVENT BEGIN:VEVENT SUMMARY:DarkSide-20k and the Future Liquid Argon Dark Matter Program DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15822@indico.ific.uv.es DESCRIPTION:Speakers: Emilija Pantic (UC Davis)\nDarkSide run since mid-20 15 a 50-kg-active-mass dual-phase Liquid Argon Time Projection Chamber (TP C)\, filled with low radioactivity argon from an underground source and pr oduced world-class results for both the low mass (M_WIMP100 GeV/c^2) direc t detection search for dark matter.\nThe next stage of the DarkSide progra m will be a new generation experiment involving a global collaboration fro m all the current Argon based experiments. DarkSide-20k is designed as a 2 0-tonne fiducial mass dual-phase Liquid Argon TPC with SiPM based cryogeni c photosensors and is expected to be free of any instrumental background f or exposure of >100 tonne x year. Like its predecessor\, DarkSide-20k will be housed at the INFN Gran Sasso (LNGS) underground laboratory\, and it i s expected to attain a WIMP-nucleon cross-section exclusion sensitivity of 7.4 x 10^{-48} cm^2 for a WIMP mass of 1 TeV/c^2 in a 200 t yr run. DarkS ide-20k will be installed inside a membrane cryostat containing more than 700 t of liquid Argon and be surrounded by an active neutron veto based on a Gd-loaded acrylic shell. The talk will give the latest updates of the o ngoing R&D and prototype tests validating the initial design.\nA subsequen t objective\, towards the end of the next decade\, will be the constructio n of the ultimate detector\, ARGO\, with a 300 t fiducial mass to push the sensitivity to the neutrino floor region for high mass WIMPs.\n\nhttps:// indico.ific.uv.es/event/6178/contributions/15822/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15822/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of the underground argon radiopurity for Dark Matter d irect searches DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15820@indico.ific.uv.es DESCRIPTION:Speakers: Vicente Pesudo (CIEMAT and LSC)\nA major worldwide e ffort is underway to procure the radiopure argon needed for DarkSide-20k ( DS-20k)\, the first large scale detector of the new Global Argon Dark Matt er Collaboration. The Urania project will extract and purify underground a rgon (UAr) from CO2 wells in the USA at a production rate of about 300 kg/ day. Additional chemical purification of the UAr will be required prior to its use in the DS-20k LAr-TPC. The Aria project will purify UAr using a c ryogenic distillation column (Seruci-I)\, located in Sardinia (Italy). Ass essing the UAr purity in terms of Ar-39 is crucial for the physics program of the DarkSide-20k experiment. DArT is a small (1 litre) radiopure chamb er that will measure the Ar-39 depletion factor in the UAr. The detector w ill be immersed in the active liquid Ar volume of ArDM (LSC\, Spain)\, whi ch will act as a veto for gammas from the detector materials and the surro unding rock. In this talk\, I will review the status and prospects of the UAr projects for DarkSide-20k.\n\nhttps://indico.ific.uv.es/event/6178/con tributions/15820/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15820/ END:VEVENT BEGIN:VEVENT SUMMARY:Physics Reach of the LUX-ZEPLIN Experiment DTSTART;VALUE=DATE-TIME:20210830T154000Z DTEND;VALUE=DATE-TIME:20210830T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15798@indico.ific.uv.es DESCRIPTION:Speakers: Amy Cottle (University of Oxford)\nLUX-ZEPLIN (LZ) i s a direct dark matter detection experiment currently being commissioned a t the 4850’ level of the Sanford Underground Research Facility in Lead\, South Dakota. The detector comprises a position sensitive xenon time proj ection chamber surrounded by an instrumented xenon “skin” and liquid s cintillator active vetoes. An active mass of 7 tonnes of xenon is used\, f rom which a fiducial region of mass 5.6 tonnes is formed that has minimal gamma-ray and neutron activity. The radiopure environment has been further ensured through an extensive material screening and selection campaign\, together with in-house xenon purification. These background mitigation str ategies underpin LZ’s unprecedented projected sensitivity to WIMPs\, dow n to a spin-independent cross section of 1.4 x 10^-48 cm^2 for a 40 GeV/c^ 2 mass in 1000 live days. This talk will provide an overview of the scienc e reach of the LZ experiment\, not just for WIMPs but also for other new p hysics.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15798/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15798/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of the LUX-ZEPLIN (LZ) experiment DTSTART;VALUE=DATE-TIME:20210830T152500Z DTEND;VALUE=DATE-TIME:20210830T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15794@indico.ific.uv.es DESCRIPTION:Speakers: David Woodward (Penn State University)\nLUX-ZEPLIN ( LZ) is a dark matter direct detection experiment currently being commissio ned at the Sanford Underground Research Facility (SURF) in Lead\, South Da kota. The experiment utilizes a two-phase time projection chamber (TPC) to look for dark matter interactions. The active region of the detector cons ists of 7 tonnes of liquid xenon with a 5.6 tonne fiducial volume\, and is expected to significantly improve our experimental sensitivity to dark ma tter beyond existing limits set by previous experiments. In this talk\, I will give an overview of the LZ project and describe the current status of the experiment\, which is expected to start taking science data this year .\n\nhttps://indico.ific.uv.es/event/6178/contributions/15794/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15794/ END:VEVENT BEGIN:VEVENT SUMMARY:DARWIN - a future dark matter and neutrino physics observatory DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15790@indico.ific.uv.es DESCRIPTION:Speakers: Teresa Marrodán Undagoitia (Max-Planck-Institut fü r Kernphysik\, Heidelberg\, Germany)\nDARWIN is a planned 50 ton liquid xe non time-projection-chamber with the primary goal of searching directly fo r dark matter. It aims to measure nuclear recoils induced by Weakly Intera cting Massive Particles (WIMPs) down to WIMP-nucleon cross sections of 1e- 48 cm2 at which neutrinos become an irreducible background.\n\nThanks to i ts low energy threshold at a few keV\, its ultra-low expected background l evels\, and unprecedented large target mass\, further physics measurements become feasible. Those include the observation of pp-solar neutrinos\, co herent neutrino-nucleus interactions\, eventually supernova neutrinos\, th e search for axions or for rare processes like the neutrinoless double-bet a decay of 136Xe. The talk will summarise the physics goals of DARWIN whic h are driving its design. In addition\, an overview of the baseline detect or setup and on-going R&D activities will be given.\n\nhttps://indico.ific .uv.es/event/6178/contributions/15790/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15790/ END:VEVENT BEGIN:VEVENT SUMMARY:The MAGIC view of the very-high gamma-ray sky DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15748@indico.ific.uv.es DESCRIPTION:Speakers: Ruben Lopez-Coto (INFN-Padova)\nMAGIC is a system of two 17 meter Imaging Air Cherenkov Telescopes\, located at the Observator io Roque de los Muchachos at an altitude of 2200 meters on the Canary isla nd of La Palma. It detects gamma rays in the very high energy regime betwe en a few tens of GeV and tens of TeV. In this presentation\, I will show t he latest highlights achieved by the powerful low energy threshold of the instrument\, like the measurement of the spectrum of the Geminga pulsar do wn to a few tens of GeV. I will also show the latest results on multiwavel ength and multimessenger astronomy\, in which MAGIC has played a leading r ole\, putting special emphasis on the flaring blazar TXS 0506+056 coincide nt with high-energy neutrino IceCube-170922A and the very recent VHE gamma -ray measurement of the GRB 190114C.\n\nhttps://indico.ific.uv.es/event/61 78/contributions/15748/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15748/ END:VEVENT BEGIN:VEVENT SUMMARY:High-energy neutrinos from Supernovae: Prospects for Identificatio n in Current and Future Neutrino Telescopes DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15768@indico.ific.uv.es DESCRIPTION:Speakers: Ali Kheirandish (Pennsylvania State University)\nNeu trino emission from supernova has played a transformative role in the deve lopment of neutrino physics and our understanding of how the star works. I nteraction of accelerated cosmic rays in the supernova ejecta and the circ umstellar material will produce high-energy neutrinos. Current and future cubic kilometer neutrino telescopes can identify high-energy neutrinos fro m a supernova in the neighborhood of the Milky Way. Observation of high-en ergy neutrinos along with the MeV neutrinos from supernovae will provide u nprecedented opportunities to understand unanswered questions in cosmic ra y physics and neutrino physics. In this talk\, we present the prospects fo r observation of high-energy neutrino bursts from in local galaxies by cur rent and future neutrino telescopes and demonstrate how additions of new n eutrino telescopes will extend the edge for identification of high-energy neutrinos from supernovae.\n\nhttps://indico.ific.uv.es/event/6178/contrib utions/15768/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15768/ END:VEVENT BEGIN:VEVENT SUMMARY:A Numerical Study of Oscillations of Highly Magnetized Non-rotatin g Axisymmetric Neutron Stars DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15766@indico.ific.uv.es DESCRIPTION:Speakers: Man Yin Leung (Department of Physics\, The Chinese U niversity of Hong Kong)\nHighly magnetized neutron stars with magnetic fie lds of $10^{15-16}$ G are promising candidates to be the observed soft gam ma repeaters and X-ray pulsars. On the other hand\, oscillations of pertur bed neutron stars are closely related to the composition\, structure\, and equation of state of the star. Thus far\, the numerical study of oscillat ions of magnetized neutron stars has not yet realized the observed order o f field magnitude. Here\, we present a breakthrough by using a multigrid-b ased general relativistic code\, `Gmunu`\, to dynamically simulate the osc illations of highly magnetized non-rotating axisymmetric neutron stars wit h field strengths of $10^{15-17}$ G under non-linear perturbations. We ext ract the eigenfrequencies and eigenfunctions of the excited oscillation mo des and preliminary results show that the eigenfrequencies decrease with t he magnetic to binding energy ratio of the neutron star\, implying a suppr ession of perturbative oscillations in a more magnetized neutron star.\n\n https://indico.ific.uv.es/event/6178/contributions/15766/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15766/ END:VEVENT BEGIN:VEVENT SUMMARY:Detecting and characterising pulsar halos with the Cherenkov Teles cope Array DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15757@indico.ific.uv.es DESCRIPTION:Speakers: Veronika Vodeb (UNG)\nThe recently identified TeV so urce class of pulsar halos may be numerous and bright enough to constitute a large fraction of the sources that will be observed with the Cherenkov Telescope Array (CTA)\, especially in the context of the Galactic Plane Su rvey (GPS)\, one of the Key Science Projects of CTA. In this study\, we ex amine the prospects offered by CTA for the detection and characterization of such objects. CTA will cover energies from 20 GeV to 300 TeV\, in betwe en those already probed by the Fermi-LAT and the High Altitude Water Chere nkov (HAWC) Observatory\, and will also have a better angular resolution t han both\, allowing us to explore the radial profile of the halos. From si mple models for individual pulsar halos and their population in the Milky Way\, we examine under which conditions such sources can be identified in the GPS observations\, possibly supplemented by additional dedicated expos ure. In the framework of a full spatial-spectral likelihood analysis\, we derive the sensitivity of CTA by considering both\, general extended emiss ion\, and the specific physical pulsar halo model.\n\nhttps://indico.ific. uv.es/event/6178/contributions/15757/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15757/ END:VEVENT BEGIN:VEVENT SUMMARY:Dissecting the inner Galaxy with gamma-ray pixel count statistics DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15747@indico.ific.uv.es DESCRIPTION:Speakers: Silvia Manconi (TTK\, RWTH Aachen)\nThe nature of th e GeV gamma-ray Galactic center excess (GCE) in the data of Fermi-LAT is s till under investigation. Different techniques\, such as template fitting and photon-count statistical methods\, have been applied in the past few y ears in order to disentangle between a GCE coming from sub-threshold point sources or rather from diffuse emissions\, such as the dark matter annihi lation in the Galactic halo.\nA major limit to all these studies is the mo deling of the Galactic diffuse foreground\, and the impact of residual mis -modeled emission on the results' robustness.\nIn Ref.[1]\, we combine for the first time adaptive template fitting and pixel count statistical meth ods in order to assess the role of sub-threshold point sources to the GCE\ , while minimizing the mis-modelling of diffuse emission components.\nWe r econstruct the flux distribution of point sources in the inner Galaxy well below the Fermi-LAT detection threshold\, and measure their radial and lo ngitudinal profiles. We find that point sources and diffuse emission from the Galactic bulge each contributes about 10% of the total emission therei n\, disclosing a sub-threshold point-source contribution to the GCE.\n\n[1 ] arXiv:2102.12497\n\nhttps://indico.ific.uv.es/event/6178/contributions/1 5747/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15747/ END:VEVENT BEGIN:VEVENT SUMMARY:Supernova bounds on axion-like particles coupled with nucleons and electrons DTSTART;VALUE=DATE-TIME:20210830T154000Z DTEND;VALUE=DATE-TIME:20210830T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15742@indico.ific.uv.es DESCRIPTION:Speakers: Giuseppe Lucente (Università di Bari & INFN Sez. Ba ri)\nWe investigate the potential of core-collapse supernovae (SNe) to co nstrain axion-like particles (ALPs) coupled to nucleons and electrons. A LPs coupled to nucleons can be efficiently produced in the SN core via nuc leon-nucleon bremsstrahlung and\, for a wide range of parameters\, leave t he SN unhindered producing a large ALP flux. For masses exceeding 1 MeV\, these ALPs would decay into electron-positron pairs\, generating a positro n flux. In the case of Galactic SNe\, the annihilation of the created posi trons with the electrons present in the Galaxy would contribute to the 511 keV annihilation line. Using the SPI (SPectrometer on INTEGRAL) observati on of this X-ray line\, allows to exclude a wide range of the axion-electr on coupling $10^{-19} \n\nhttps://indico.ific.uv.es/event/6178/contributio ns/15742/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15742/ END:VEVENT BEGIN:VEVENT SUMMARY:Can unresolved PWNe weaken the evidence of CR spectral hardening i n the inner Galaxy? DTSTART;VALUE=DATE-TIME:20210830T152500Z DTEND;VALUE=DATE-TIME:20210830T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15740@indico.ific.uv.es DESCRIPTION:Speakers: Vittoria Vecchiotti (GSSI)\nThe large-scale diffuse $\\gamma-$ray flux observed by Fermi-LAT in the 1-100 GeV energy range is parameterized as a power law with spectral index $\\Gamma$ that depends on the distance from the Galactic center.\nThis feature\, if attributed to t he diffuse emission produced by cosmic rays (CR) interactions with the int erstellar gas\, can be interpreted as the evidence of a progressive CR spe ctral hardening towards the Galactic center\, challenging the standard cos mic rays diffusion paradigm.\nWe report on the implications of TeV Pulsar Wind Nebulae observed by the HESS Galactic Plane Survey in the 1-100 TeV e nergy range for the interpretation of Fermi-LAT data.\nWe show that the co nsistency among HGPS and Fermi-LAT (3FGL) catalogue requires that Galactic sources\, observed by both experiments\, have a spectral break at $\\sim 0.1-1.0$ TeV and an harder emission spectrum in the GeV domain.\nSuch spec tral shape is well compatible with the expected gamma-ray emission in youn g PWNe due to Inverse Compton scattering of high-energy electrons on backg round radiation fields.\nWe argue that a fraction of this population canno t be resolved by Fermi-LAT in the GeV domain providing a relevant contribu tion to the large-scale diffuse emission\, viz. the $30\\%$ of the total d iffuse $\\gamma$-ray emission in the inner Galaxy.\nThe inclusion of this additional component in fitting Fermi-LAT data strongly affects the spectr al index for the truly diffuse emission\, that can be increased by an amou nt $\\Delta \\Gamma=0.17$\, weakening the evidence of a progressive harden ing of the cosmic-ray proton spectrum in the inner Galaxy.\n\nhttps://indi co.ific.uv.es/event/6178/contributions/15740/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15740/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrinos from galactic sources DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15729@indico.ific.uv.es DESCRIPTION:Speakers: Viviana Niro (Laboratoire APC)\nThe HAWC telescopes has recently revealed new spectra for gamma-ray sources in the Galactic pl ane. In this talk I will review the possibility of detecting these sources at KM3 detectors. I will consider\, with particular emphasis\, the 2HWC J 1825-134 source. Amongst the HAWC sources\, it is indeed the most luminous in the multi-TeV domain and therefore is one of the first that should be searched for with a neutrino telescope in the northern hemisphere. I will show the prospects to detect this source at the KM3NeT detector and commen t on the possibilities for others neutrino telescopes. \nI will consider\, moreover\, the gamma-ray sources eHWC J1907+063\, eHWC J2019+368 and 2HWC J1857+027. For these sources\, I will show the prediction for neutrinos a t the IceCube detector\, presenting the calculation of the statistical sig nificance\, considering 10 and 20 years of running time\, and I will comme nt on the current results reported by the collaboration.\n\nhttps://indico .ific.uv.es/event/6178/contributions/15729/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15729/ END:VEVENT BEGIN:VEVENT SUMMARY:Deep Science at Boulby Underground Laboratory DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15942@indico.ific.uv.es DESCRIPTION:Speakers: Sean Paling (STFC Boulby Underground Laboratory)\nAn update of facilities and science in the UK's deep underground science fac ility. For more than three decades astro-particle physicists have been ope rating experiments to search for Dark Matter 1100m below ground in a purpo se-built low-background facility at Boulby mine in the North East of Engla nd. Dark Matter studies continue at Boulby. The facility currently support s various smaller Dark Matter R&D studies and operates the BUGS facility - a growing suite of high sensitivity Germanium detectors and surface alpha measurement systems needed to undertake ever-more sensitive material scre ening measurements for rare-event studies. In the meantime the range of sc ience projects exploiting the special properties of deep underground envir onment at Boulby has grown\, with projects current and/or planned in the a reas of astroparticle and low background science\, Earth and environmental science\, biology/astrobiology and planetary exploration technology devel opment. For the future Boulby is planning to expand to host future major r are-event and wider multidisciplinary science studies. This talk will give an overview of the Boulby Underground Laboratory\, the science currently supported and plans for science at Boulby in the future.\n\nhttps://indico .ific.uv.es/event/6178/contributions/15942/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15942/ END:VEVENT BEGIN:VEVENT SUMMARY:LABChico: a shallow underground laboratory in Mexico DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15940@indico.ific.uv.es DESCRIPTION:Speakers: Eric Vazquez-Jauregui (Instituto de Física\, UNAM)\ nLABChico will be an underground laboratory in Mineral del Chico\, Comarca Minera\, Hidalgo UNESCO Global Geopark\, in Mexico inside a decommissione d mine with an approximate rock overburden of 100 meters. This laboratory currently under development and with construction planned by the end of 20 21\, will be primarily focusing on research in low background gamma assay for neutrino and dark matter experiments\, detector prototypes\, and appli cations related to environmental radioactivity by measuring the presence o f radionuclides in food\, soil\, and water. The facility will initially ho st two HPGe detectors for gamma assays and plastic scintillator counters f or muon flux measurements used for educational purposes. LABChico is suppo rted by the National Autonomous University of Mexico (UNAM)\, the governme nt of Hidalgo and the Comarca Minera\, Hidalgo UNESCO Global Geopark in Me xico\, and the Global Challenges Research Fund in the UK. In this talk\, I will present the current status of the facility\, measurements of gamma b ackgrounds at the location of the laboratory\, and the results of the gamm a and alpha screening program.\n\nhttps://indico.ific.uv.es/event/6178/con tributions/15940/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15940/ END:VEVENT BEGIN:VEVENT SUMMARY:The ANDES Deep Underground initiative and underground mine sites i n Argentina DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15939@indico.ific.uv.es DESCRIPTION:Speakers: Xavier Bertou (CNEA/CONICET)\nANDES is an internatio nal effort to build a world class deep underground laboratory at the borde r between Argentina and Chile in the planned Agua Negra tunnel. With 1750 m of overburden\, horizontal access\, and 70 000 m3 of volume\, it should offer an attractive option in the southern hemisphere to the underground s cience community. As the construction of the tunnel and laboratory is plan ned to take 10 years\, efforts are also currently focused on providing to the regional community alternative shallow sites to start developing proto type for future underground science detectors.\nI will discuss the status of ANDES and the prospects for 2 mine sites in Argentina\, the Sierra Gran de mine which was used in the 1990s for a dark matter experiment\, and the mina Casposo\, in the vicinity of the location planned for ANDES.\n\nhttp s://indico.ific.uv.es/event/6178/contributions/15939/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15939/ END:VEVENT BEGIN:VEVENT SUMMARY:The Sar-Grav Laboratory DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15936@indico.ific.uv.es DESCRIPTION:Speakers: Davide Rozza (INFN-LNS & University of Sassari)\nLoc ated in Sardinia close to Lula\, the region of the Sos Enattos mine is und erstudies to host the third generation of gravitational wave interferomete r: Einstein Telescope (ET). The Sar-Grav laboratory\, a seed of ET\, will host underground experiments\, cryogenic payloads\, low frequency and cryo genic sensor development that need low seismic and anthropogenic noise. In deed\, the Sos Enattos mine already hosts seismometer and magnetometer net s\, located both on the surface and underground\, that prove the quietness of the site. On the surface area\, the Sar-Grav laboratory is characteriz ed by a hangar of 900 square meters equipped with rooms for the experiment s\, an optical laboratory\, and a control room. An area of 250 square mete rs and small experimental areas are planned to be located underground wher e stations at different depths already host the sensors net.\n\nhttps://in dico.ific.uv.es/event/6178/contributions/15936/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15936/ END:VEVENT BEGIN:VEVENT SUMMARY:Callio Lab – the deep underground research centre in Finland\, E urope DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15935@indico.ific.uv.es DESCRIPTION:Speakers: Jari Joutsenvaara (Kerttu Saalasti Institute\, Unive rsity of Oulu)\nLocated just below the Polar circle\, Callio Lab is one of the northernmost underground laboratories in Europe [1\,2]. The undergrou nd research centre has developed from underground physics (formerly known as the Centre for Underground Physics in Pyhäsalmi\, CUPP [3]). Over the years\, its strategy has been shifted to a multi-and transdisciplinary res earch centre\, now known as Callio Lab.\nThe Callio Lab is physically loca ted at the 1.44 km deep Pyhäsalmi mine\, Pyhäjärvi\, Finland. The mine has produced copper\, zinc and pyrite since its opening in 1962. The depo sit is geologically located within a 1.9 bn-year-old seafloor and belongs to the class of volcanic massive sulphide (VMS) deposits [4]. Seismically the bedrock is stable and tremors are mainly induced by the mining activit ies. The mine has a flat overburden\, and access to the mine is through an 11 km incline or the 1.4 km deep elevator shaft. The travel times are 30 minutes and 2.5 minutes\, respectively [5]. \nThe development of undergrou nd research facilities in the Pyhäsalmi mine started in the late 1990s at the margin of the then known ore resources. However\, with the discovery of a new deposit below the old one\, the life span of the underground mini ng was extended year by year. However\, it is expected that mining will ce ase at the later part of 2021. The eventual end of underground extraction will give more room and possibilities for science\, research and business. The latter is governed by the Callio – Mine for business [6]\, governed by the local town. The scientific activities of Callio Lab are coordinate d by the University of Oulu\, Finland.\nThroughout the years the various s cientific activities and research initiatives have been started at the Cal lio Lab. The characterisation of underground halls (i.e.\, Labs in the fac ility) has included the on-site natural background radiation measurements (gamma\, neutron\, radon) and sample analysis of the building materials us ed and samples of the surrounding bedrock [7–12]. The muon background me asurements were done in 2005 [13]. The rock overburden at a depth of 1390 has been measured to be 4000 m.w.e.\, and at Lab 2\, located at a depth of 1436m\, it is estimated around 4100 m.w.e [5].\nThe scientific activities at utilising the Callio lab research infrastructure range from mining and mining-related training to geothermal concept and technology testing\, un derground food production\, working environment research\, and particle ph ysics. The low-background facility\, using the low background HPGe detecto r from Baltic Scientific Instruments\, is located at Lab 5 at a depth of 1 410 m. [14]. The facility provides sample analysis services for the EUL pr oject laboratories [15]\, but other scientific institutions benefit from t he facility too.\nCallio Lab is part of the DULIA network\, a founding mem ber of the European Underground Laboratories association [15]\, a candidat e as a thematic core service for the European Plate Observation System\, E POS [16]\, member of Nordic and Finnish EPOS research infrastructures\, an d is a strategic research infrastructure of the University of Oulu. EPOS i s on the European and Finnish research infrastructure roadmaps.\n\nThis wo rk has been supported by grants by the Interreg Baltic Sea programme and N ordforsk. \n \nReferences\n1. Puputti J\, Joutsenvaara J\, Kotavaara O\, Niinikoski E-R. 2021 From Earth and beyond - Callio Lab underground centr e for Science and R\\&D. In EGU General Assembly Conference Abstracts\, pp . EGU21-14229.\n2. 2021 Callio Lab. See https://calliolab.com/facilities-2 /facilities/ (accessed on 20 April 2021).\n3. Enqvist T et al. 2005 Resear ch options in the pyhäsalmi underground facility. Nucl. Phys. B - Proc. S uppl. 143\, 561. (doi:10.1016/j.nuclphysbps.2005.01.226)\n4. Mäki T\, Kou sa J\, Luukas J. 2015 The Vihanti-Pyhäsalmi VMS Belt. In Mineral Deposits of Finland\, pp. 507–530. Elsevier Inc. (doi:10.1016/B978-0-12-410438-9 .00020-0)\n5. Joutsenvaara J (Jari). 2016 Deeper understanding at Lab 2:th e new experimental hall at Callio Lab underground centre for science and R & D in the Pyhäsalmi Mine\, Finland. University of Oulu. See http://urn. fi/URN:NBN:fi:oulu-201606042350.\n6. 2021 Callio - Mine for Business. See https://callio.info.\n7. Debicki Z\, Jedrzejczak K\, Kasztelan M\, Marszal W\, Orzechowski J\, Szabelski J\, Tokarski P. 2019 Measurements of therma l neutron flux in underground laboratories\, a standard proposal for the B SUIN project. In The multi-messenger astronomy: gamma-ray bursts\, search for electromagnetic counterparts to neutrino events and gravitational wave s\, pp. 48–54.\n8. Jedrzejczak K\, Kasztelan M\, Szabelski J\, Tokarski P\, Orzechowski J\, Marszał W\, Przybylak M. 2020 Characteristics of natu ral neutron radiation background performed within the BSUIN project. In EG U General Assembly Conference Abstracts\, p. 3353.\n9. Polaczek-Grelik K e t al. 2020 Natural background radiation at Lab 2 of Callio Lab\, Pyhäsalm i mine in Finland. Nucl. Instruments Methods Phys. Res. Sect. A Accel. Spe ctrometers\, Detect. Assoc. Equip. 969\, 164015. (doi:10.1016/j.nima.2020. 164015)\n10. Gostilo V\, Sokolov A\, Pohuliai S\, Joutsenvaara J. 2020 Cha racterisation of the natural gamma-ray background in the underground Calli o Lab facility. Appl. Radiat. Isot. 156\, 108987. (doi:10.1016/j.apradiso. 2019.108987)\n11. Abdurashitov J. N. GVNMVLSAAYVEPJKT. 2006 Measurement of Neutron Background at the Pyhasalmi mine for CUPP Project\, Finland. arXi v:nucl-ex \n12. Pohuliai S\, Sokolov A\, Gostilo V\, Joutsenvaara J\, Pupu tti J. 2020 Measurements of gamma-ray background radiation in Pyhäsalmi m ine. Appl. Radiat. Isot. 161. (doi:10.1016/j.apradiso.2020.109166)\n13. En qvist T et al. 2005 Measurements of muon flux in the Pyhäsalmi undergroun d laboratory. Nucl. Instruments Methods Phys. Res. Sect. A Accel. Spectrom eters\, Detect. Assoc. Equip. 554\, 286–290. (doi:10.1016/j.nima.2005.08 .065)\n14. Pohuliai S\, Sokolov A\, Gostilo V\, Joutsenvaara J\, Puputti J . 2020 Measurements of gamma-ray background radiation in Pyhäsalmi mine. Appl. Radiat. Isot. 161\, 109166. (doi:10.1016/j.apradiso.2020.109166)\n15 . Mischo H\, Fuławka K\, Joutsenvaara J. 2021 European Underground Labora tories Association EUL-An International Partner for Underground Research O pportunities. In EGU General Assembly Conference Abstracts\, pp. EGU21--77 30.\n16. Elger K\, Lauterjung J\, Ulbricht D\, Cocco M\, Atakan K\, Bailo D\, Glaves H\, Jeffrey K. 2016 Implementation of the European Plate Observ ing System (EPOS) Infrastructure.\n\nhttps://indico.ific.uv.es/event/6178/ contributions/15935/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15935/ END:VEVENT BEGIN:VEVENT SUMMARY:The Sanford Underground Research Facility DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15933@indico.ific.uv.es DESCRIPTION:Speakers: Jaret Heise (Sanford Underground Research Facility)\ nThe Sanford Underground Research Facility (SURF) has been operating since 2007 supporting underground research in rare-process physics\, as well as offering research opportunities in other disciplines. SURF laboratory fac ilities include a Surface Campus as well as campuses at the 4850-foot leve l (1500 m\, 4300 m.w.e.) that host a range of significant physics experime nts\, including the LUX-ZEPLIN (LZ) dark matter experiment and the MAJORAN A DEMONSTRATOR neutrinoless double-beta decay experiment. The CASPAR nucle ar astrophysics accelerator recently completed the first phase of operatio n. Furthermore\, the BHUC laboratory dedicated to critical material assays for current and future experiments has been operating since Fall 2015. Co nstruction is underway for the Long-Baseline Neutrino Facility (LBNF) that will host the international Deep Underground Neutrino Experiment (DUNE). SURF is a dedicated research facility with significant expansion capabilit y\, and applications from new experiments are welcome.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15933/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15933/ END:VEVENT BEGIN:VEVENT SUMMARY:The New Underground Facility (Yemilab) in Korea DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15930@indico.ific.uv.es DESCRIPTION:Speakers: Kang Soon Park (Institute for Basic Science (IBS))\n A new underground facility called Yemilab with a depth of 1\,000 m will be constructed for studies on neutrinos and dark matter search. The new unde rground facility is located within the site of an iron mine in Jeongseon-g un\, Gangwon-do\, South Korea. Since the mine has a vertical shaft with a diameter of 6 m and a length of 600 m\, the facility uses this shaft. The construction of the new underground facility consists of a cage for passen gers (man-cage) to enter the underground\, excavation of tunnels with a to tal area of 10\,000 m$^2$ including a dedicated area of 2\,600 m$^2$ for e xperiments\, and construction of electrical and mechanical facilities for operation. The construction is carried out in two phases. In the first pha se\, man-cage manufacture/installation and most of the tunnel excavation w ere carried out. In the second stage\, excavation of a large cylindrical p it with dimensions of 20 m (D) x 20 m (H) is being carried out together wi th the installation of a 2 MW power supply and construction of facilities for ventilation\, drainage\, and fire prevention. The first phase construc tion started in 2018 and was completed in August 2020. The second phase co nstruction started in May 2021 and is going to be completed in May 2022. T he Yemilab will be introduced in this presentation.\n\nhttps://indico.ific .uv.es/event/6178/contributions/15930/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15930/ END:VEVENT BEGIN:VEVENT SUMMARY:Low radioactivity and Multi- disciplinarily Underground Laboratory of Modane (LSM) DTSTART;VALUE=DATE-TIME:20210830T152500Z DTEND;VALUE=DATE-TIME:20210830T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15928@indico.ific.uv.es DESCRIPTION:Speakers: Ali Dastgheibi Fard (CNRS/LPSC_LSM)\nThe Modane Unde rground Laboratory (LSM) is located 1700 m (4800 m.w.e) below Fréjus pea k (Alpes chain) mountain in the middle of the Fréjus tunnel between Franc e/Italy. The LSM is a multi-disciplinary platform for the experiments requ iring low radioactivity environment. Several experiments in Particle and A stroparticle Physics\, low-level of High Purity of Germanium gamma ray spe ctrometry\, biology and home land security hosted in the LSM. It’s equip ped by Anti-Radon facility where all of the detectors are under Radon depl eted Air. We will present the LSM structure and briefly reviewed of all ex periments are installed in.\n\nhttps://indico.ific.uv.es/event/6178/contri butions/15928/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15928/ END:VEVENT BEGIN:VEVENT SUMMARY:Status and prospect of China Jinping Underground Laboratory DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15927@indico.ific.uv.es DESCRIPTION:Speakers: Hao Ma (Tsinghua University)\nChina Jinping undergro und laboratory (CJPL) is located in the Jinping Mountain\, Sichuan Provinc e\, southwest China\, with a rock overburden of about 2400m. The laborator y is operated by Tsinghua University and Yalong River Hydropower Developme nt Company\, LTD. The scientific project at CJPL is mainly focused on dark matter detection\, nuclear astrophysics and low background screening tech niques. Based on CJPL extension project (CJPL-II)\, the Deep Underground a nd ultra-low Radiation Background Facility for frontier physics experiment s (DURF) will start construction this September. This talk will give an ov erview of CJPL status and DURF project\, as well as main experiments and s cientific activities carried out at CJPL.\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15927/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15927/ END:VEVENT BEGIN:VEVENT SUMMARY:Estimations for the Newtonian noise of the future Einstein Telesco pe on the basis of data measured at Mátra Mountain Range in Hungary DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15515@indico.ific.uv.es DESCRIPTION:Speakers: Edit Fenyvesi (Wigner Research Centre for Physics)\n Seismic noise\, the related gravitational gradient noise (Newtonian noise) and the thermal noise of the suspension last stage and of the test masses determine the sensitivity of current gravitational-wave detectors at low frequencies. Seismic and Newtonian noises can be mitigated by installing t he detectors under the ground\, while the thermal noise can be reduced by cryogenically cooling down the test masses. One of the proposed subterrane an detectors\, the European Einstein Telescope (ET) is planned to be built 200 to 300 m below the surface. The noise budget of ET at low frequencies is expected to be dominated by seismic noise and Newtonian noise of seism ic and infrasonic origin. In order to get to know the long-term evolution of these types of noises\, the Mátra Gravitational and Geophysical Labora tory (MGGL) was built 88 m below the surface at the Hungarian Mátra Mount ain Range. Infrasound measurements and seismic noise measurements were sta rted in 2017. The seismic noise measurements are still going on. We invest igate the evolution of the Newtonian noise via applying the most recent mo delling methods presented in literature and using our measurement data as input. I give an overview of the measurements done at MGGL\, the modelling methods of Newtonian noise\, and the results of our investigations.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15515/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15515/ END:VEVENT BEGIN:VEVENT SUMMARY:Sub-threshold search for strongly lensed gravitational-wave events in the first half of LIGO-Virgo's third observing run DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15507@indico.ific.uv.es DESCRIPTION:Speakers: Chan Chun Lung (The Chinese University of Hong Kong) \nStrong gravitational lensing of gravitational waves can produce duplicat e signals separated in time with different amplitudes. We consider the cas e in which strong lensing produces identifiable gravitational wave events and weaker sub-threshold signals hidden in the noise background. We presen t a search method for the sub-threshold signals using targeted template ba nks targeting specific confirmed gravitational wave events. We apply the m ethod to all the gravitational-wave signals from compact binary coalescenc es detected by Advanced LIGO and Advanced Virgo during O3a\, the first hal f of their third observing run. Finally\, we present the top 8 possible le nsed candidates for O3a gravitational wave events that passed our nominal significance threshold of False Alarm Rate 1 in 16 years. Furthermore\, we discuss the likelihood that these candidates are strongly lensed.\n\nhttp s://indico.ific.uv.es/event/6178/contributions/15507/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15507/ END:VEVENT BEGIN:VEVENT SUMMARY:Beyond the detector horizon: forecasting gravitational-wave strong lensing DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15506@indico.ific.uv.es DESCRIPTION:Speakers: Renske Wierda (Utrecht University)\nGravitational wa ves could be gravitationally lensed just like light. Strong lensing makes gravitational waves appear as repeated events with different amplitudes wi thin our detectors. We will investigate recent forecasts for observed lens ed event rates\, including sub-threshold searches. We will also discuss a pressing issue related to the current lensed event searches: the rising pr obability of so-called search false alarms. We show how the inclusion of l ensing statistics can help remedy this problem.\n\nhttps://indico.ific.uv. es/event/6178/contributions/15506/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15506/ END:VEVENT BEGIN:VEVENT SUMMARY:Environmental noises in current and future gravitational-wave dete ctors. DTSTART;VALUE=DATE-TIME:20210831T154500Z DTEND;VALUE=DATE-TIME:20210831T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15495@indico.ific.uv.es DESCRIPTION:Speakers: Francesca Badaracco (UCLouvain)\nGravitational-wave detectors are very sensitive instruments that suffer from a huge number of noises. If we aim to observe gravitational waves with Earth-based detecto rs\, we need to take care of every source that can prevent the observation .\nSeismic noise poses a huge challenge to the sensitivity in the the low frequency band and it is tackled with suspensions and active controls. The low frequency band can also be threatened by the so-called Newtonian nois e\, generated by the fluctuations of the gravity field. If this has not be en a problem in the first generation gravitational-wave detectors\, it wil l be so in the next runs and especially in the third-generation detectors\ , like the Einstein Telescope. We need then to be prepared to suppress as much as possible these noises\, otherwise they might become the last wall for the sensitivity of our detectors. \nThis talk will explore environment al noises with a particular detail on Newtonian and seismic noise and the techniques that we can employ to reduce their effects.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15495/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15495/ END:VEVENT BEGIN:VEVENT SUMMARY:Bridging the microhertz gap with asteroids: opportunities and chal lenges for gravitational wave detection DTSTART;VALUE=DATE-TIME:20210831T154000Z DTEND;VALUE=DATE-TIME:20210831T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15497@indico.ific.uv.es DESCRIPTION:Speakers: Michael A. Fedderke (The Johns Hopkins University)\n The science case for a broad program of gravitational wave (GW) detection across all frequency bands is exceptionally strong. At present\, there is a dearth of coverage by existing and proposed searches in the GW frequency band lying between the peak sensitivities of PTAs and LISA\, roughly 0.1- 100 microhertz. In this talk\, I will outline a conceptual mission proposa l to access this band. I will demonstrate that a few carefully chosen aste roids which orbit in the inner Solar System can act as excellent naturally occurring gravitational test masses despite the environmental noise sourc es. As such\, a GW detector can be constructed by ranging between these as teroids using optical or radio links. At low frequencies\, I will discuss how gravity gradient noise arising from the combined motion of the other $ \\sim 10^6$ asteroids in the inner Solar System sharply cuts off the sensi tivity of this proposal. Sensitivity in the middle of this band is mostly limited by various solar perturbations to the asteroid test masses\, while the high-frequency sensitivity is limited by noise in the ranging link. T he projected strain-sensitivity curve that I will present indicates signif icant potential reach in this frequency band for a mission of this type.\n \nhttps://indico.ific.uv.es/event/6178/contributions/15497/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15497/ END:VEVENT BEGIN:VEVENT SUMMARY:CSIS: a Cryogenic Superconducting Inertial Sensor DTSTART;VALUE=DATE-TIME:20210831T152500Z DTEND;VALUE=DATE-TIME:20210831T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15494@indico.ific.uv.es DESCRIPTION:Speakers: Joris van Heijningen (UCLouvain)\nThe future of Grav itational Waves (GWs) is bright. LIGO and Virgo have detected more than 70 signals from black hole and/or neutron star mergers. All measured signals come in-band at around 30 Hz as suspension control noise\, fueled by many cross couplings between angular and translational degrees of freedom\, is dominant below 30 Hz. It is impossible to know\, but exciting to imagine what signals are lurking there once we can access this regime.\n\nEinstein Telescope (ET) will be an underground and cryogenic detector sensitive to GWs down to 2 Hz. New sensor development is underway for ET. We believe t he cryogenic environment can be used in combination with superconducting m aterials to open up pathways to low-loss actuators and sensor mechanics. \ n\nThe Cryogenic Superconducting Inertial Sensor (CSIS) revolutionizes the (cryogenic) inertial sensor field by obtaining a displacement sensitivity at 0.5 Hz of 3 orders of magnitude better than state-of-art. Not only wil l it help ET detect GWs from 2 Hz onwards\, CSIS will also be deployed on the Moon. The recently published Lunar GW Antenna (LGWA) concept uses an i nertial sensor to probe surface motion as a result of the GW excitation of the Moon's normal body modes (fundamental just below 1 mHz and many other modes and their harmonics at higher frequencies). In summary\, CSIS will be the world's most sensitive low-frequency inertial sensor and\, when dep loyed in ET and on the Moon\, will enable GW science from 1 mHz to 10 Hz.\ n\nhttps://indico.ific.uv.es/event/6178/contributions/15494/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15494/ END:VEVENT BEGIN:VEVENT SUMMARY:Lunar Gravitational-Wave Antenna DTSTART;VALUE=DATE-TIME:20210831T151000Z DTEND;VALUE=DATE-TIME:20210831T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15493@indico.ific.uv.es DESCRIPTION:Speakers: Jan Harms (Gran Sasso Science Institute)\nGravitatio nal waves excite quadrupolar vibrations of elastic bodies. Monitoring thes e vibrations was one of the first concepts proposed for the detection of g ravitational waves by Joseph Weber. At laboratory scale\, these experiment s became known as resonant-bar detectors\, which form an important part of the history of GW detection. Due to the dimensions of these bars\, the ta rgeted signal frequencies were in the kHz range. It was also Weber who sug gested to monitor vibrations of the Moon to search for gravitational waves in the mHz band. His Lunar Surface Gravimeter was deployed on the Moon in 1972 by the Apollo 17 crew. A design error made it impossible to carry ou t the intended search for GWs\, but the idea remains intriguing. We propos e a Lunar Gravitational-Wave Antenna (LGWA) based on Weber’s idea. The k ey component is a next-generation\, high-sensitivity seismometer to be dep loyed on the Moon. LGWA would have rich scientific synergies with other GW detectors like LISA and ET and also with EM observatories. At the same ti me\, it would serve as a high-precision geophysical station shedding light on the interior structure of the Moon\, the mechanisms of moonquakes\, an d the Moon's formation history. Furthermore\, its technology is of high re levance for ET\, and other future terrestrial GW detectors\, as part of a new generation of seismic isolation systems.\n\nhttps://indico.ific.uv.es/ event/6178/contributions/15493/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15493/ END:VEVENT BEGIN:VEVENT SUMMARY:The International Dark Matter Day in Argentina DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15784@indico.ific.uv.es DESCRIPTION:Speakers: Maria Belen Lovino (CAB/UNRN)\nThe International Dar k Matter Day is celebrated worldwide on October 31 every year since 2017. In Argentina\, it was organized for the first time in 2019 in an outreach effort coordinated by the ANDES deep underground laboratory. In 2019\, we started a call for art students to propose an audiovisual piece on Dark Ma tter\, asked about whether basic science was important for Argentina and c oordinated the projection of the full dome "Phantom of the Universe" video in 4 digital planetarium in Argentina. In 2020\, with no possibility of p ublic event due to the pandemic\, we repeated the audiovisual art call and organized a call for drawings and questions about Dark Matter for kids\, reaching kids from Brazil and Mexico in addition to Argentina\, among othe r activities.\n\nIn this presentation I will showcase some of the answers obtained to the calls and how these answers could be used to understand be tter how to communicate abstract topics such as Dark Matter to our society \, taking into account the preconceptions about the topic.\n\nhttps://indi co.ific.uv.es/event/6178/contributions/15784/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15784/ END:VEVENT BEGIN:VEVENT SUMMARY:Teaching physics to school students from an Einsteinian standpoint DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15783@indico.ific.uv.es DESCRIPTION:Speakers: Rahul Choudhary (The University of Western Australi a)\nIn my presentation\, I will discuss my study on middle school students ’ understanding of Einsteinian physics with an emphasis on quantum physi cs that demonstrates the possibility of teaching physics from an Einsteini an standpoint. Firstly\, I will show the age group dependence between stud ents of year 7—10 by measuring students’ knowledge\, and attitude towa rds physics. Secondly\, I will demonstrate the possibility of combining ph ysical models and analogies with digital learning resources for teaching E insteinian physics. Finally\, I will present a quantitative method for tea ching the fundamental concepts of matter-wave interference and diffraction using simple devices called phasor wheels at the middle school level.\n\n https://indico.ific.uv.es/event/6178/contributions/15783/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15783/ END:VEVENT BEGIN:VEVENT SUMMARY:Spreading the space-time news: outreach and communication activiti es from the EGO-Virgo Collaboration DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15782@indico.ific.uv.es DESCRIPTION:Speakers: Jerome Degallaix (LMA - IP2I)\nThe recent discoverie s of Gravitational Wave (GW) signals have attracted a lot of interest from the general public and scientific colleagues. It is crucial to properly c ommunicate the excitement of the emerging field of GW science to the socie ty and have the potential to engage and educate new generations of future scientists. \nThe EGO-Virgo Collaboration is active in many outreach and c ommunication fronts: from the fascinating complexity of the Advanced Virgo detector\, together with its partners Advanced LIGO and KAGRA\, to the ph ysics behind the recent detections from this worldwide network of GW detec tors. This talk will review the main outreach and communication activities carried out in this effort\, including some specifically developed to cop e for the pandemic: online and live remote visits and virtual tours to the EGO site\, webinars\, round table and online events\, social media\, coll aboration with artists\, sonifications\, outreach and educational material translated in several languages and the development of exhibits for gener al public events.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15 782/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15782/ END:VEVENT BEGIN:VEVENT SUMMARY:International masterclasses at IFIC: 17 years of particle physics for high school students DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15781@indico.ific.uv.es DESCRIPTION:Speakers: Alberto Aparici (IFIC (CSIC-Univ Valencia))\nThe Int ernational Masterclasses "Hands on Particle Physics" is an initiative spon sored by the International Particle Physics Outreach Group and hosted by C ERN\, Fermilab and multiple research centers around the world. It aims to make particle physics knowledge available to high school-grade students an d to create an environment where the students can feel how it is to work o n an international collaboration. A central activity during the masterclas ses is the rough analysis of real data from particle physics experiments b y the students\, usually by means of a simple software provided by the exp eriments. This allows several groups in different countries to carry out t he same analysis on similar dates\, and then the different groups can be g athered and their results can be compared and combined. The International Masterclasses have been running since the mid-2000s\, and the Instituto de Física Corpuscular (IFIC) has participated in most of the editions. This talk will provide a review of our experience and the feedback we have gat hered from students and teachers.\n\nhttps://indico.ific.uv.es/event/6178/ contributions/15781/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15781/ END:VEVENT BEGIN:VEVENT SUMMARY:Outreach and educational activities of the ALICE collaboration dur ing the COVID pandemic DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15780@indico.ific.uv.es DESCRIPTION:Speakers: Despina Hatzifotiadou (INFN Bologna)\nWith the onset of the COVID pandemic in 2020 all outreach and educational activities wit h in-person participation had to stop. The ALICE collaboration adapted to the new situation and continued reaching out to the public using the mult itude of online tools and platforms available. We will focus here on two o f our main outreach activities\, virtual visits and masterclasses.\n\nWith the cancellation of all in-person visits to the underground installations \, virtual visits became the only way to explore the experiment. ALICE ha d already been offering virtual visits for remote audiences with equipment installed in the ALICE Run Control Centre (ARC). We recently acquired ded icated mobile equipment for the virtual visits to the cavern and developed a scenario which includes both the cavern and the ARC as well as a Q&A se ssion. In this way\, visitors from many countries have the opportunity to interact with scientists and to see parts of the experiment that they woul d never be able to see during a real visit.\n\nALICE has been participatin g in the International Masterclasses (IMC) programme ever since measuremen ts based on LHC data were introduced in it. The packages used had been dev eloped by simplifying the ALICE event display and were based on ROOT. Wit h the spreading of the COVID pandemic the 2020 IMC programme was interrupt ed. In 2021\, with most activities taking place remotely\, it was obvious that web-based versions were needed. The implementation of such versions allowed us to hold remote masterclasses for high-school students\, thus e nsuring the continuity of this important outreach activity of our communit y. In addition we reached new countries and also involved high-school tea chers in this global effort.\n\nhttps://indico.ific.uv.es/event/6178/contr ibutions/15780/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15780/ END:VEVENT BEGIN:VEVENT SUMMARY:Undergroud muon flux measured by EEE students DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15779@indico.ific.uv.es DESCRIPTION:Speakers: Stefano Boi ()\nThe Extreme Energy Events experiment (EEE) is an extended array of about 60 cosmic ray detectors installed in several Italian High Schools and in a few research laboratories. The EEE e xperiment has two main targets: a scientific and a dissemination. An array of telescopes made of three MRPC detectors is used to detect cosmic rays and perform physics measurements\, such as studies on galactic cosmic rays variation\, anisotropies or long distance correlations. The dissemination goal is achived by allowing students to actively participate in collabora tion's activities\, building telescopes\, monitoring data acquisition\, pe rforming physics analysis under supervision of EEE researchers and present ing their results in monthly EEE collaboration meetings.\n\nFor field oper ations\, the EEE collaboration developed a portable scintillator-based det ector named Cosmic Box (CB). The CB allows students to perform cosmic ray counting measurements in various environments. CBs are made with two 15 x 15 x 1 cm scintillators read by two 3 x 3 cm$^2$ SIPMs operated in coincid ence. Three CBs were deployed in Nuraxi Figus and Seruci coal mine to perf orm an underground measurement of the cosmic muon flux attenuation. 83 day s were required to collect a total of 4260 events at the maximum depth of 512 m. High schools students from Sardinia and Lombardia were directly inv olved in all phases of the measurements. After a safety training\, student s helped in underground positioning of the detectors\, DAQ configuring and data collection. Data were recorded in a SD memory card and eventually tr anfered for the off-line analysis.\n\nAfter presenting the EEE project\, t he contribution will be focused on the experimental set up and the measure ment\, reporting some preliminary results.\n\nhttps://indico.ific.uv.es/ev ent/6178/contributions/15779/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15779/ END:VEVENT BEGIN:VEVENT SUMMARY:The Cosmic Ray Live Project @SNOLAB DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15778@indico.ific.uv.es DESCRIPTION:Speakers: Silvia Scorza (SNOLAB)\nThe Cosmic Ray Live project aims at building three muon detectors at SNOLAB. The detectors can measure muons in real time and show their trajectories. They would add significan t data to the existing array and promote the international relationships t hat make science possible. One of SNOLAB’s missions is to inspire the ne xt generation of innovators through strong educational outreach. This proj ect aims to develop a tangible way for students and visitors to the Scienc e North Museum to understand cosmic rays and why SNOLAB is located 2km und erground. Our international partner at Laboratori Nazionali del Gran Sasso (LNGS) has perfected the build requirements and the accompanying smartpho ne app\, which makes this science accessible to everyone in Canada. I will review them along with the current status of the project.\n\nhttps://indi co.ific.uv.es/event/6178/contributions/15778/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15778/ END:VEVENT BEGIN:VEVENT SUMMARY:Science Summaries: explaining LIGO-Virgo-KAGRA results to the glob al public DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15777@indico.ific.uv.es DESCRIPTION:Speakers: David Keitel (Universitat de les Illes Balears)\nLIG O\, Virgo and KAGRA form the second-generation global network of gravitati onal wave detectors. From the first detection of the GW150914 binary black hole merger to the latest results from the recent O3 observing run\, our observations are pushing frontiers in observational astrophysics. To conti nue inspiring the wider public with our findings\, one key communications activity of the LVK collaborations are "science summaries" for each of our papers. These texts provide a less technical introduction to the topics c overed in each paper and its key results\, aimed at both students and inte rested lay readers. They are published at www.ligo.org and promoted throug h social media channels of the three collaborations. Before the pandemic\, they also proved popular as printouts at science fairs\, and we all hope we can return to that mode of outreach soon. As a global collaboration\, o ver recent years we have also significantly stepped up our output of trans lations of these summaries\, drawing on member scientists from across the globe\, with materials published in a total of 23 different languages so f ar.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15777/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15777/ END:VEVENT BEGIN:VEVENT SUMMARY:Global Cosmic-Ray studies educational platform DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15776@indico.ific.uv.es DESCRIPTION:Speakers: Barbora Bruant Gulejova (IPPOG / University of Bern / CERN)\nThe International Particle Physics Group (IPPOG) is a global netw ork active in informal education and outreach in particle physics and rela ted research\, including cosmic-ray and astro-particle physics. Since many years\, IPPOG has been actively supporting the International Cosmic Day o rganized by DESY and the International Muon Week organized by Quarknet. In 2015 IPPOG started work on establishing a universal portal through which successful cosmic-ray study programmes can reach out to teachers and stude nts around the world. This common web platform is being developed by IPPOG in the frame of its new IPPOG web pages. It will contain all information for schools interested in taking part in cosmic-ray experiments and analys ing real data in classroom\; also instructions about how to build\, borrow \, or purchase cosmic-ray detectors. The platform will also facilitate col laboration and exchanges between the experiments' project managers and adv ertising of related events.\n\nhttps://indico.ific.uv.es/event/6178/contri butions/15776/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15776/ END:VEVENT BEGIN:VEVENT SUMMARY:The Outreach and Education program of the Darkside experiment DTSTART;VALUE=DATE-TIME:20210901T154500Z DTEND;VALUE=DATE-TIME:20210901T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15775@indico.ific.uv.es DESCRIPTION:Speakers: Bianca Bottino (Princeton University and INFN Genova )\nThe Darkside experiment aims at the direct detection of Dark Matter in the form of Weakly Interacting Massive Particles (WIMPs). It is a 20-tonne (fiducial) argon dual-phase Time-Projection Chamber (TPC) that exploits t he cryogenic SiPM technology to identify unambiguously the nuclear recoils induced by WIMPs. The experiment is being installed at the LNGS and will start operation around 2024.\n\nThe goal of the Outreach and Education pro gram of Darkside is to disseminate the experiment activity through promoti onal videos and events addressed to the general public and students. One o f our main activities is the DarkSide Masterclass\, in which high school s tudents become physicists for a day searching for WIMPs. After a few intro ductory lectures\, the students analyze real data from the precursor DarkS ide-50 experiment. Master degree students have access to a more complex ve rsion of this Masterclass. Six Masterclass events took place in the last t wo years\, with the participation reaching 400 students in one event. In t his talk\, we will present the detailed Outreach and Education program of Darkside Collaboration.\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15775/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15775/ END:VEVENT BEGIN:VEVENT SUMMARY:The International Particle Physics Outreach Group - Reaching Acros s the Globe with Science DTSTART;VALUE=DATE-TIME:20210901T154000Z DTEND;VALUE=DATE-TIME:20210901T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15774@indico.ific.uv.es DESCRIPTION:Speakers: Steven Goldfarb (University of Michigan)\nThe Intern ational Particle Physics Outreach Group (IPPOG) is a network of scientists \, science educators and communication specialists working across the glob e in informal science education and outreach for particle physics. The pri mary methodology adopted by IPPOG requires the direct involvement of scien tists active in current research with education and communication speciali sts\, in order to effectively develop and share best practices in outreach . IPPOG member activities include the International Particle Physics Maste rclass programme\, International Day of Women and Girls in Science\, World wide Data Day\, International Muon Week and International Cosmic Day organ isation\, and participation in activities ranging from public talks\, fest ivals\, exhibitions\, teacher training\, student competitions\, and open d ays at local institutions. These independent activities\, often carried ou t in a variety of languages to public with a variety of backgrounds\, all serve to gain the public trust and to improve worldwide understanding and support of science. We present our vision of IPPOG as a strategic pillar o f particle physics\, fundamental research and evidence-based decision-maki ng around the world.\n\nhttps://indico.ific.uv.es/event/6178/contributions /15774/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15774/ END:VEVENT BEGIN:VEVENT SUMMARY:Engaging the public with astrophysics virtual reality experiences DTSTART;VALUE=DATE-TIME:20210901T152500Z DTEND;VALUE=DATE-TIME:20210901T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15773@indico.ific.uv.es DESCRIPTION:Speakers: Magdalena Kersting (University of Oslo)\nVirtual rea lity (VR) technologies present exciting opportunities for astrophysics edu cation and outreach. VR turns abstract concepts into experienceable phenom ena and can increase interest and engagement with physics and astronomy. H owever\, we still lack knowledge about how to maximise the benefits of VR when we use these technologies in public outreach programs. In this talk\, we will present a case study of an astrophysics virtual reality experienc e at a science festival. To study the relationship between VR and visitor engagement\, we developed a framework that comprises four aspects of visit or activity: immersion\, facilitation\, collaboration\, and visualisation. This framework and our findings reveal important ways that VR supports vis itor engagement at a science festival. We will finish the talk by giving r ecommendations for engaging the public with astrophysics both with and wit hout VR.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15773/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15773/ END:VEVENT BEGIN:VEVENT SUMMARY:Involving the new generations in particle physics endeavours DTSTART;VALUE=DATE-TIME:20210901T151000Z DTEND;VALUE=DATE-TIME:20210901T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15772@indico.ific.uv.es DESCRIPTION:Speakers: Simone Donati (University of Pisa)\nSince 1984 the I talian groups of the Istituto Nazionale di Fisica Nucleare (INFN) and Ital ian Universities\, collaborating with the DOE laboratory of Fermilab (US) have been running a two-month summer training program for Italian universi ty students. While in the first year the program involved only four physic s students of the University of Pisa\, in the following years it was exten ded to engineering students. This extension was very successful and the en gineering students have been since then extremely well accepted by the Fer milab Technical\, Accelerator and Scientific Computing Division groups. Ov er the many years of its existence\, this program has proven to be the mos t effective way to engage new students in Fermilab endeavors. Many student s have extended their collaboration with Fermilab with their Master Thesis and PhD.\nSince 2004 the program has been supported in part by DOE in the frame of an exchange agreement with INFN. An additional agreement for sha ring support for engineers of the School of Advanced Studies of S.Anna (SS SA) of Pisa was established in 2007 between SSSA and Fermilab. In the fram e of this program four SSSA students are supported each year. Over its 35 years of history\, the program has grown in scope and size and has involve d more than 500 Italian students from more than 20 Italian Universities\, Since the program does not exclude appropriately selected non-italian stud ents\, a handful of students of European and non-European Universities wer e also accepted in the years. \nEach intern is supervised by a Fermilab Me ntor responsible for performing the training program. Training programs sp anned from Tevatron\, CMS\, Muon (g-2)\, Mu2e and SBN design and experimen tal data analysis\, development of particle detectors (silicon trackers\, calorimeters\, drift chambers\, neutrino and dark matter detectors)\, desi gn of electronic and accelerator components\, development of infrastructur es and software for tera-data handling\, research on superconductive eleme nts and on accelerating cavities\, theory of particle accelerators.\nSince 2010\, within an extended program supported by the Italian Space Agency a nd the Italian National Institute of Astrophysics\, a total of 30 students in physics\, astrophysics and engineering have been hosted for two months in summer at US space science Research Institutes and laboratories. \nIn 2015 the University of Pisa included these programs within its own educati onal programs. Accordingly\, Summer School students are enrolled at the Un iversity of Pisa for the duration of the internship and are identified and ensured as such. At the end of the internship the students are required t o write summary reports on their achievements. After positive evaluation b y a University Examining Board\, interns are acknowledged 6 ECTS credits f or their Diploma Supplement. \nInformation on student recruiting methods\, on training programs of recent years and on final student`s evaluation pr ocess at Fermilab and at the University of Pisa will be given in the prese ntation.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15772/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15772/ END:VEVENT BEGIN:VEVENT SUMMARY:Exploring the Sun's core with BabyIAXO DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15689@indico.ific.uv.es DESCRIPTION:Speakers: Javier Galan (Universidad de Zaragoza)\nAxions are a natural consequence of the Peccei-Quinn mechanism\, the most compelling s olution to the strong-CP problem. Similar axion-like particles (ALPs) also appear in a number of possible extensions of the Standard Model\, notably in string theories. Both axions and ALPs are very well motivated candidat es for Dark Matter\, and in addition\, they would be copiously produced at the sun’s core. A relevant effort during the last decade has been the C AST experiment at CERN\, the most sensitive axion helioscope to-date. The International Axion Observatory (IAXO) is a large-scale 4th generation hel ioscope. As its primary physics goal\, IAXO will look for solar axions or ALPs with a signal to background ratio of about 5 orders of magnitude high er than CAST.\n\nIn this talk I will briefly review astrophysical hints an d models that we will be able to explore while searching for solar axions within the context of the IAXO helioscope search program\, and in particul ar the physics under reach of BabyIAXO\, and intermediate helioscope stage towards the full IAXO.\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15689/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15689/ END:VEVENT BEGIN:VEVENT SUMMARY:A numerical approach to stochastic inflation and primordial black holes DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15675@indico.ific.uv.es DESCRIPTION:Speakers: Eemeli Tomberg (NICPB\, Tallinn)\nQuantum fluctuatio ns created during cosmic inflation act as seeds of all structure in the un iverse. The strongest fluctuations lead to the formation of primordial bla ck holes\, a dark matter candidate. I present a study where these fluctuat ions are analyzed numerically within the framework of stochastic inflation . This method allows us to probe nonperturbative effects and include backr eaction between the fluctuations and the local background. The results rev eal a non-Gaussian\, exponential tail in the probability distribution of t he fluctuations\, enhancing black hole production by a factor of $10^5$ co mpared to a Gaussian estimate in our CMB-compatible example scenario. The same method may be used to improve the primordial black hole predictions o f any inflationary model.\n\nhttps://indico.ific.uv.es/event/6178/contribu tions/15675/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15675/ END:VEVENT BEGIN:VEVENT SUMMARY:Resurrecting the Fraternal Twin WIMP Miracle DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15674@indico.ific.uv.es DESCRIPTION:Speakers: Jakub Scholtz (U degli studi di Torino)\nIn Twin Hig gs models which contain the minimal particle content required to address t he little hierarchy problem (i.e. fraternal models)\, the twin tau has bee n identified as a promising candidate for dark matter. In this class of sc enarios\, however\, the elastic scattering cross section of the twin tau w ith nuclei exceeds the bounds from XENON1T and other recent direct detecti on experiments. In this paper\, we propose a modification to the Fraternal Twin Higgs scenario that we call $\\mathbb{Z}_2$FTH\, incorporating visib le and twin hypercharged scalars (with $Y=2$) which break twin electromagn etism. This leads to new mass terms for the twin tau that are unrelated to its Yukawa coupling\, as well as additional annihilation channels via the massive twin photon. We show that these features make it possible for the right-handed twin tau to freeze out with an acceptable thermal relic abun dance while scattering with nuclei at a rate that is well below existing c onstraints. Nonetheless\, large portions of the currently viable parameter space in this model are within the reach of planned direct detection expe riments. The prospects for indirect detection using gamma rays and cosmic- ray antiprotons are also promising in this model. Furthermore\, if the twi n neutrino is light\, the predicted deviation of $\\Delta N_{\\mathrm{eff} }\\sim 0.1$ would be within reach of Stage 4 CMB experiments. Finally\, th e high luminosity LHC should be able to probe the entire parameter space o f the $\\mathbb{Z}_2$FTH model through charged scalar searches. We also di scuss how searches for long-lived particles are starting to constrain Frat ernal Twin Higgs models.\n\nhttps://indico.ific.uv.es/event/6178/contribut ions/15674/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15674/ END:VEVENT BEGIN:VEVENT SUMMARY:Thermal axions with multi-eV masses are possible in low-reheating scenarios DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15672@indico.ific.uv.es DESCRIPTION:Speakers: Pierluca Carenza (Bari University & INFN Bari)\nWe r evise cosmological mass bounds on hadronic axions in low-reheating cosmolo gical scenarios\, with a reheating temperature $T_{\\rm RH}\\le 100$ MeV\, in light of the latest cosmological observations. In this situation\, the neutrino decoupling would be unaffected\, while the thermal axion relic a bundance is suppressed. Moreover\, axions are colder in low-reheating temp erature scenarios\, so that bounds on their abundance are possibly loosen ed. As a consequence of these two facts\, cosmological mass limits on axi ons are relaxed. Using state-of-the-art cosmological data and characterizi ng axion-pion interactions at the leading order in chiral perturbation th eory\, we find in the standard case an axion mass bound $m_a \n\nhttps://i ndico.ific.uv.es/event/6178/contributions/15672/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15672/ END:VEVENT BEGIN:VEVENT SUMMARY:Maximally misaligned axions DTSTART;VALUE=DATE-TIME:20210830T154500Z DTEND;VALUE=DATE-TIME:20210830T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15668@indico.ific.uv.es DESCRIPTION:Speakers: Mario Reig (IFIC (CSIC-Univ Valencia))\nIn this talk I will discuss a simple model of maximal axion misalignment. Maximally-mi saligned axions with masses larger than 10^{-22} eV constitute an attracti ve DM candidate with interesting phenomenology. On the other hand\, maxima lly-misaligned axions with masses m=O(1-100)H_0 generically behave as dark energy with a decay constant that can take values well below the Planck s cale\, avoiding problems associated to super-Planckian scales.\n\nhttps:// indico.ific.uv.es/event/6178/contributions/15668/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15668/ END:VEVENT BEGIN:VEVENT SUMMARY:An update on the two singlet Dark Matter model DTSTART;VALUE=DATE-TIME:20210830T154000Z DTEND;VALUE=DATE-TIME:20210830T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15665@indico.ific.uv.es DESCRIPTION:Speakers: Tanushree Basak (Indus University)\nWe revisit the t wo real singlet extension of the Standard Model with a $Z_2\\times Z_2^\\p rime$ symmetry. One of the singlet scalars $S_2$\, by virtue of an unbroke n $Z_2^\\prime$ symmetry\, plays the role of a stable dark matter candidat e. The other scalar $S_1$\, with spontaneously broken $Z_2$-symmetry\, mix es with the SM Higgs boson and acts as the scalar mediator. We analyze the model by putting in the entire set of theoretical and recent experimental constraints. The latest bounds from direct detection Xenon1T experiment s everely restricts the allowed region of parameter space of couplings. To e nsure the dark matter satisfies the relic abundance criterion\, we rely on the Breit-Wigner enhanced annihilation cross-section. Further\, we study the viability of explaining the observed gamma-ray excess in the galactic center in this model with a dark matter of mass in the $\\sim 36-51$ GeV w indow and present our conclusions.\n\nhttps://indico.ific.uv.es/event/6178 /contributions/15665/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15665/ END:VEVENT BEGIN:VEVENT SUMMARY:Axion Production in Pulsar Magnetosphere Gaps DTSTART;VALUE=DATE-TIME:20210830T151000Z DTEND;VALUE=DATE-TIME:20210830T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15663@indico.ific.uv.es DESCRIPTION:Speakers: Anirudh Prabhu (Stanford University)\nPulsar magneto spheres admit non-stationary vacuum gaps that are characterized by non-van ishing $\\bf {E \\cdot B}$. The vacuum gaps play an important role in plas ma production and electromagnetic wave emission. We show that these gaps g enerate axions whose energy is set by the gap oscillation frequency. The d ensity of axions produced in a gap can be several orders of magnitude grea ter than the ambient dark matter density. In the strong pulsar magnetic fi eld\, a fraction of these axions may convert to photons\, giving rise to b roadband radio signals. We show that dedicated observations of nearby puls ars with radio telescopes (FAST) and interferometers (SKA) can probe axion -photon couplings that are a few orders of magnitude lower than current as trophysical bounds.\n\nhttps://indico.ific.uv.es/event/6178/contributions/ 15663/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15663/ END:VEVENT BEGIN:VEVENT SUMMARY:TA\, TALE and TAx4\, Latest Results DTSTART;VALUE=DATE-TIME:20210831T120000Z DTEND;VALUE=DATE-TIME:20210831T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15762@indico.ific.uv.es DESCRIPTION:Speakers: Douglas Bergman (University of Utah)\nThe Telescope Array (TA) is an ultra-high energy cosmic ray detector\, the largest in th e Northern Hemisphere\, sensitive to cosmic rays with energies from 1 PeV to above 100 EeV. The main detector is a hybrid detector consisting of an array of 507 surface detectors covering 700 km$^2$ overlooked by three flu orescence telescope detector stations. The energy range has been extended at the low end by the TA Low Energy (TALE) extension consisting of fluores cence detector stations with higher elevation viewing angle and an infill array of surface detectors. At the lowest energies\, around 1 PeV\, the TA LE fluorescence telescopes operate as imaging air Cherenkov telescopes and work in hybrid with the Non-Imaging Cherenkov (NICHE) array for hybrid Ch erenkov observation. TA is also being extended at the highest energies by increasing the covered area by a factor of four in the TAx4 project. In th is presentation\, we will present the latest results from TA including a m easurement of the spectrum and anisotropy studies\, nuclear composition re sults from TALE\, and the first results from TAx4.\n\nhttps://indico.ific. uv.es/event/6178/contributions/15762/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15762/ END:VEVENT BEGIN:VEVENT SUMMARY:Latest results form LHAASO Observatory DTSTART;VALUE=DATE-TIME:20210831T113000Z DTEND;VALUE=DATE-TIME:20210831T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15746@indico.ific.uv.es DESCRIPTION:Speakers: Domenico della Volpe (Université de Genève)\nThe r ecent release of a Nature paper on twelve Galactic sources\, and the detec tion of photons up to 1.4 PeV revealed the enormous physics potential of L HAASO.\nIn this contribution\, we will briefly illustrate the LHASSO Obser vatory and its potential and latest published results.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15746/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15746/ END:VEVENT BEGIN:VEVENT SUMMARY:Line of sight PeV-EeV neutrinos from gamma-ray blazars due to ultr ahigh-energy cosmic-ray propagation DTSTART;VALUE=DATE-TIME:20210831T114500Z DTEND;VALUE=DATE-TIME:20210831T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15730@indico.ific.uv.es DESCRIPTION:Speakers: Soebur Razzaque (University of Johannesburg Centre f or Astro-Particle Physics)\nBlazars are potential candidates of cosmic-ray acceleration up to ultrahigh energies (𝐸 > 1 EeV). For an efficient co smic-ray injection from blazars\, 𝑝𝛾 collisions with the extragalact ic background light (EBL) and cosmic microwave background (CMB) can produc e neutrino spectrum with peaks near PeV and EeV energies\, respectively. W e analyze the contribution of these neutrinos to the diffuse background me asured by the IceCube neutrino observatory. The fraction of neutrino lumin osity originating from individual redshift ranges is calculated using the distribution of BL Lacs and FSRQs provided in the Fermi-LAT 4LAC catalog. Furthermore\, we use a luminosity dependent density evolution to find the neutrino flux from unresolved blazars. The results obtained in our model i ndicate that as much as ≈10% of the flux upper bound at a few PeV energi es can arise from cosmic-ray interactions on EBL. The same interactions wi ll also produce secondary electrons and photons\, initiating electromagnet ic cascades. The resultant photon spectrum is limited by the isotropic dif fuse 𝛾-ray flux measured between 100 MeV and 820 GeV. The latter\, toge ther with the observed cosmic-ray flux at $𝐸>10^{16.5}$ eV\, can constr ain the baryonic loading factor depending on the maximum cosmic-ray accele ration energy.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15730 / LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15730/ END:VEVENT BEGIN:VEVENT SUMMARY:New Properties of Primary Cosmic Rays observed by the Alpha Magnet ic Spectrometer on the International Space Station DTSTART;VALUE=DATE-TIME:20210902T120000Z DTEND;VALUE=DATE-TIME:20210902T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15750@indico.ific.uv.es DESCRIPTION:Speakers: Mercedes Paniccia (University of Geneva (CH))\nWe re port the observation of new properties of primary cosmic-ray neon (Ne)\, m agnesium (Mg)\, silicon (Si) and iron (Fe) nuclei measured in the rigid ity range from 2 GV to 3 TV by the Alpha Magnetic Spectrometer on the Inte rnational Space Station. The properties of the light primary cosmic-ray he lium (He)\, carbon (C) and oxygen (O) nuclei will be also discussed\, show ing that Ne\, Mg\, Si and He\, C\, O form two different classes of primary cosmic rays\, and that unexpectedly Fe belongs to the class of light prim ary cosmic rays He\, C\, and O.\n\nhttps://indico.ific.uv.es/event/6178/co ntributions/15750/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15750/ END:VEVENT BEGIN:VEVENT SUMMARY:A novel multimessenger study of Starburst galaxies: implications f or neutrino astronomy DTSTART;VALUE=DATE-TIME:20210902T114500Z DTEND;VALUE=DATE-TIME:20210902T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15735@indico.ific.uv.es DESCRIPTION:Speakers: Antonio Ambrosone (University of Naples Federico II and Istituto Nazionale di Fisica Nucleare sezione Napoli)\nStarburst galax ies (SBGs) and more in general starforming galaxies represent a class of g alaxies with a high star formation rate (up to 100 Mo/year). Despite their low luminosity\, they can be considered as guaranteed “factories” of high energy neutrinos\, being “reservoirs” of accelerated cosmic rays and hosting a high density target gas in the central region. The estimatio n of their point-like and diffuse contributions to the neutrino astrophysi cal flux measured by IceCube can be crucial to describe the diffuse neutri no spectral features as well as the peculiar point-like excess like NGC106 8. To this aim we use the most update gamma-ray catalog of this class of o bjects to perform a multimessenger study and describe their gamma-ray emi ssion through a calorimetric scenario.\n\nFor the diffuse analysis we perf orm a blending of the measured spectral indexes and obtain a multi-compone nt description of extragalactic background light (EGB)\, high energy start ing events (HESE) and high-energy cascade IceCube data. Remarkably\, we fi nd that\, differently from recent prototype scenarios\, the spectral index blending allows starburst galaxies to account for up to 40% of the HESE events at 95.4% CL and favors a maximal energy of the accelerated cosmi c rays at teens of PeV.\n\nFor the point like analysis we apply the calori metric approach to the known SBGs within 100 Mpc\, considering\, were poss ible\, a source-by-source description of the star formation rate. These re sults are then compared with what IceCube and ANTARES have seen at TeV ene rgies as well as with what can be expected from the incoming KM3NeT.\n\nht tps://indico.ific.uv.es/event/6178/contributions/15735/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15735/ END:VEVENT BEGIN:VEVENT SUMMARY:LST-1\, the Large-Sized Telescope prototype of CTA: status and fir st observations. DTSTART;VALUE=DATE-TIME:20210902T113000Z DTEND;VALUE=DATE-TIME:20210902T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15732@indico.ific.uv.es DESCRIPTION:Speakers: Abelardo Moralejo Olaizola (Institut de Física d'Al tes Energies (IFAE-BIST)\, Barcelona)\nCTA (Cherenkov Telescope Array) is the next generation ground-based\nobservatory for gamma-ray astronomy at v ery-high energies. Once\ncompleted\, CTA will outperform present-day facil ities by an order of\nmagnitude in sensitivity\, and significantly enlarge the accessible energy \nrange and survey capabilities. Deployed in the CT A north site\, on the \nisland of La Palma (Spain)\, LST-1 is the prototyp e for the CTA Large-Sized \nTelescopes\, which will cover the lower end of the energy range of the array\, \ndown to 20 GeV. LST-1 started astronomi cal observations in late 2019\, and\nis currently completing its commissio ning phase. We will present the\nstatus of the instrument and an overview of the first physics results.\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15732/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15732/ END:VEVENT BEGIN:VEVENT SUMMARY:State-of-the art parameter estimation of gravitational wave events with the new phenomenological waveform models in frequency and time domai n DTSTART;VALUE=DATE-TIME:20210902T120000Z DTEND;VALUE=DATE-TIME:20210902T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15512@indico.ific.uv.es DESCRIPTION:Speakers: Maite Mateu-Lucena (University of the Balearic Islan ds)\nIn this talk we present in-depth state-of-the-art parameter estimatio n studies of several gravitational wave events with open LIGO-Virgo data. \nWe use the fourth generation of phenomenological waveform models\, the f requency domain IMRPhenomX and the time domain IMRPhenomT families which i nclude higher harmonics and precession\, and constitute the computationall y most efficient inspiral-merger-ringdown frequency and time domain wavefo rm models for binary black holes with are currently available in the LALSu ite software framework. We systematically compare the Bilby and LALInferen ce frameworks for parameter estimation\, and perform highly parallel simul ations in a traditional supercomputing environment. We discuss our automat isation of Bayesian inference runs\, and the use of a machine learning mod el in order to predict the duration of a PE run or its number of likelihoo d evaluations. Due to the computational efficiency of the waveform models we can perform systematic tests of different priors\, sampler settings\, w aveform models and inference codes. We discuss the computational cost\, an d the wall-clock time required to get fast parameter estimation results\, and aspects of the systematic uncertainties in the waveform models. Regard ing results\, special emphasis is put on the intermediate mass black hole GW190521 event\, which is astrophysically particularly interesting\, but also particularly challenging due to the shortness of the signal.\n\nhttps ://indico.ific.uv.es/event/6178/contributions/15512/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15512/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for unmodeled long duration gravitational waves for Advan ced LIGO and Advanced Virgo's third observing run DTSTART;VALUE=DATE-TIME:20210902T113000Z DTEND;VALUE=DATE-TIME:20210902T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15509@indico.ific.uv.es DESCRIPTION:Speakers: Claudia Lazzaro (Università degli Studi di Padova)\ nMany astrophysical phenomena are foreseen to emit GW transient signal wit h long duration (since few up to few hundreds seconds)\, such as fallback accretion\, accretion disk instabilities\, nonaxisymmetric deformations in magnetars. The theoretical predictions for those astrophysical processes cover a wide range of signal morphologies and in most cases are poorly kno wn. In such cases\, we need unmodeled search techniques.\nWe report on res ults of unmodeled long-duration transient searches in the third observing run of Advanced LIGO and Advanced Virgo. The search is performed using m inimal assumptions and covers the range of 2s-500s duration in the frequen cy band of 24Hz-2048Hz. We use three different algorithms to improve dete ction capability and coverage of search parameter space thanks to differe nt assumptions and data handling techniques.\n\nhttps://indico.ific.uv.es/ event/6178/contributions/15509/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15509/ END:VEVENT BEGIN:VEVENT SUMMARY:Gravitational-wave lensing with ground-based gravitational-wave de tectors DTSTART;VALUE=DATE-TIME:20210902T114500Z DTEND;VALUE=DATE-TIME:20210902T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15500@indico.ific.uv.es DESCRIPTION:Speakers: Otto Hannuksela ()\nGravitational waves\, like light \, could be gravitationally lensed by intervening matter. Recent studies s uggest that we might see gravitational-wave lensing within the coming year s as the current ground-based detectors are upgraded. However\, the method s to detect and employ gravitational-wave lensing are entirely different f rom light lensing. Indeed\, we detect waves instead of particles\, and the source population is one of merging black holes. For these reasons\, the field might also pave the way to new applications. Here I will discuss som e of our recent work in the field.\n\nhttps://indico.ific.uv.es/event/6178 /contributions/15500/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15500/ END:VEVENT BEGIN:VEVENT SUMMARY:Combined Dark Matter searches from dwarf spheroidal galaxies obser vations by Fermi-LAT\, HAWC\, H.E.S.S.\, MAGIC\, and VERITAS DTSTART;VALUE=DATE-TIME:20210902T114500Z DTEND;VALUE=DATE-TIME:20210902T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15902@indico.ific.uv.es DESCRIPTION:Speakers: Daniel Kerszberg (IFAE-BIST)\nDwarf spheroidal galax ies (dSphs) are ideal targets for Dark Matter (DM) indirect searches due t o their high DM content and their negligible expected astrophysical backgr ound. In this presentation\, we report on the combined analysis of the obs ervations of 20 dSphs by Fermi-LAT\, HAWC\, H.E.S.S.\, MAGIC\, and VERITAS collaborations in the search for DM\, focusing on the Weakly Interacting Massive Particles (WIMPs) scenario. The combined analysis allows us to max imize the sensitivity by combining individual data sets from all five expe riments for which the energy ranges of the search overlap. New constraints \, spanning a range of DM masses from 5 GeV to 100 TeV\, on the velocity-w eighted cross section for DM self annihilation will be presented.\n\nhttps ://indico.ific.uv.es/event/6178/contributions/15902/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15902/ END:VEVENT BEGIN:VEVENT SUMMARY:Results of axion searches at 34 μeV with RADES haloscope and pros pects for searches in BabyIaxo DTSTART;VALUE=DATE-TIME:20210902T120000Z DTEND;VALUE=DATE-TIME:20210902T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15877@indico.ific.uv.es DESCRIPTION:Speakers: Sergio Arguedas Cuendis ()\nThe Relic Axion Detector Exploratory Setup (RADES) detector employs rectangular cavities joined by irises to search for axion dark matter between 8 and 9 GHz present in the galactic halo using the haloscope technique. The first results for an axi on search in the mass range 34.6738 μeV \n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15877/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15877/ END:VEVENT BEGIN:VEVENT SUMMARY:Sensitivity of CTA to gamma-ray emission from the Perseus galaxy c luster DTSTART;VALUE=DATE-TIME:20210902T113000Z DTEND;VALUE=DATE-TIME:20210902T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15856@indico.ific.uv.es DESCRIPTION:Speakers: Judit Pérez-Romero (IFT UAM-CSIC)\nWe estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse gamma -ray emission from the Perseus galaxy cluster\, both from interactions of cosmic rays (CR) with the intra-cluster medium\, or as a product of annihi lation or decay of dark matter (DM) particles in case they are weakly inte ractive massive particles (WIMPs). The observation of Perseus constitutes one of the Key Science Projects proposed by the CTA Consortium for the fir st years of operation of the CTA Observatory. In this talk\, we will focus on the DM-induced component of the flux. Our DM modeling includes the sub structures we expect in the main halo of Perseus\, as predicted within the standard cosmological model hierarchical structure formation scenario\, w hich will boost the annihilation signal significantly. We compute the expe cted CTA sensitivity using a likelihood maximization analysis including th e most recent CTA instrument response functions. We also model the expecte d CR-induced gamma-ray flux in the cluster\, and both DM- and CR-related u ncertainties via nuisance parameters. We will show the sensitivity of CTA to discover\, at best\, diffuse gamma-rays in galaxy clusters for the firs t time. Even in absence of signal\, we show that CTA will allow us to prov ide stringent and competitive constraints on TeV DM\, that will rely on st ate-of-the-art modeling of the cluster's DM distribution. Finally\, we wil l discuss the optimal strategy for CTA observations of Perseus.\n\nhttps:/ /indico.ific.uv.es/event/6178/contributions/15856/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15856/ END:VEVENT BEGIN:VEVENT SUMMARY:New Results from a Three-Year Annual Modulation Search with COSINE -100 DTSTART;VALUE=DATE-TIME:20210831T120000Z DTEND;VALUE=DATE-TIME:20210831T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15895@indico.ific.uv.es DESCRIPTION:Speakers: William Thompson (Yale University)\nCOSINE-100 is a direct detection dark matter experiment that is testing DAMA/LIBRA's claim of dark matter discovery. Located in South Korea's Yangyang Underground L aboratory\, COSINE-100 comprises 106 kg of sodium iodide detectors surroun ded by a ~2000 L liquid scintillator veto. In this talk\, I will present n ew results from an annual modulation search using three years of data and the impact on DAMA/LIBRA's discovery claim. I will also discuss improvemen ts over our previous modulation analysis\, including lowering the analysis threshold to 1 keV and the development of a more robust time-dependent ba ckground model. In addition\, I will review ongoing R&D projects for\, and the physics reach of future phases of the experiment.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15895/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15895/ END:VEVENT BEGIN:VEVENT SUMMARY:Windchime: Gravitational Direct Detection of Dark Matter DTSTART;VALUE=DATE-TIME:20210831T114500Z DTEND;VALUE=DATE-TIME:20210831T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15832@indico.ific.uv.es DESCRIPTION:Speakers: Rafael Lang (Purdue University)\nRecent calculations have demonstrated that we may attempt the direct detection of dark matter in the laboratory through gravitational interaction alone. This is in par ticular relevant around the well-motivated Planck mass scale (10^19 GeV or 22 micro-gram). The Windchime collaboration is working towards a large ar ray of dedicated sensors\, based on MEMS accelerometers. Paired with quant um-enhanced readout including squeezed light sources and quantum back-acti on evasion\, such an experiment may ultimately realize this exciting sensi tivity. In the meantime\, searches for ultra-light (\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/15832/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15832/ END:VEVENT BEGIN:VEVENT SUMMARY:Annual modulation results from three-year exposure of ANAIS-112 DTSTART;VALUE=DATE-TIME:20210831T113000Z DTEND;VALUE=DATE-TIME:20210831T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15818@indico.ific.uv.es DESCRIPTION:Speakers: Maria Martinez (CAPA-UZ)\nANAIS-112 is a dark matter direct detection experiment that operates 112 kg of NaI(Tl) scintillators at the Canfranc Underground Laboratory (LSC\, Spain). Its main goal is to test in a model independent way one of the most puzzling results in the p resent particle physics scenario: the DAMA/LIBRA observation of an annual modulation in the detection rate compatible with that expected for dark ma tter. This signal is in strong tension with the negative results of other very sensitive experiments. However\, until recently a direct comparison using the same target material (NaI(Tl)) was lacking.\nANAIS-112 has been taking data since August 2017 in stable conditions with excellent performa nce. Results from the first three years are compatible with the absence of modulation and incompatible with the DAMA/LIBRA measured modulation at mo re than 2.5 sigma C.L. This result supports the projected goal of reaching a 3 sigma sensitivity to the DAMA/LIBRA result for the five-year operatio n scheduled.\nIn this talk we will describe the ANAIS-112 setup\, the expe riment performance and the data analysis. Then we will present the results of the three-year annual modulation search and discuss the physical impli cations and the experiment's prospects.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15818/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15818/ END:VEVENT BEGIN:VEVENT SUMMARY:TeV-scale Lepton Number Violation: Connecting Leptogenesis\, Neutr inoless Double Beta Decay\, and Colliders DTSTART;VALUE=DATE-TIME:20210827T120000Z DTEND;VALUE=DATE-TIME:20210827T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15688@indico.ific.uv.es DESCRIPTION:Speakers: Julia Harz (Technical University of Municht (TUM))\n In the context of TeV-scale lepton number violating (LNV) interactions\, w e illustrate the interplay between leptogenesis\, neutrinoless double beta (0νββ) decay\, and LNV searches at proton-proton colliders. Using a co ncrete model for illustration\, we identify the parameter space where stan dard thermal leptogenesis is rendered unviable due to washout processes an d show how 0νββ decay and pp-collisions provide complementary probes. W e find that the new particle spectrum can have a decisive impact on the re lative sensitivity of these two probes.\n\nhttps://indico.ific.uv.es/event /6178/contributions/15688/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15688/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmology meets functional QCD: First-order cosmic QCD transition induced by large lepton asymmetries DTSTART;VALUE=DATE-TIME:20210827T114500Z DTEND;VALUE=DATE-TIME:20210827T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15687@indico.ific.uv.es DESCRIPTION:Speakers: Isabel M. Oldengott (UC Louvain)\nThe lepton flavour asymmetries of the Universe are observationally almost unconstrained befo re the onset of neutrino oscillations. We calculate the cosmic trajectory during the cosmic QCD epoch in the presence of large lepton flavour asymme tries. By including QCD thermodynamic quantities derived from functional Q CD methods in our calculation our work reveals for the first time the poss ibility of a first-order cosmic QCD transition. We specify the required va lues of the lepton flavour asymmetries for which a rst-order transition oc curs for a number of different benchmark scenarios.\n\nhttps://indico.ific .uv.es/event/6178/contributions/15687/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15687/ END:VEVENT BEGIN:VEVENT SUMMARY:Testing fundamental cosmological assumptions with Euclid DTSTART;VALUE=DATE-TIME:20210827T113000Z DTEND;VALUE=DATE-TIME:20210827T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15683@indico.ific.uv.es DESCRIPTION:Speakers: Matteo Martinelli (IFT\, UAM/CSIC)\nThe forthcoming Euclid survey will be able to map the Large Scale Structure with unprecend ent precision\, with the aim of tightly constraining the standard cosmolog ical model and its most common extensions. The great sensitivity of Euclid can however also be exploited to test our most fundamental assumptions at the basis of the cosmological investigation.\nIn this talk I will present two recents results of the Euclid Collaboration\, where forecast Euclid p roducts are used alongside data from other surveys to constrain violation of the Distance Duality Relation and time evolution of the fine structure constant. I will show how Euclid will significantly contribute in constrai ning these effects\, both connected with the presence of new physics beyon d the standard cosmological model.\n\nhttps://indico.ific.uv.es/event/6178 /contributions/15683/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15683/ END:VEVENT BEGIN:VEVENT SUMMARY:The electronic recoil excess in XENON1T and the prospect to deciph er it with XENONnT DTSTART;VALUE=DATE-TIME:20210827T113000Z DTEND;VALUE=DATE-TIME:20210827T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15875@indico.ific.uv.es DESCRIPTION:Speakers: Jingqiang Ye (Columbia University)\nThe XENON1T dark matter experiment\, operated at the INFN Laboratori Nazionali del Gran Sa sso\, achieved the lowest electronic recoil background among all dark mat ter experiments\, which is $76 \\pm 2\\\,\\mathrm{events}/(\\mathrm{t}\\cd ot\\mathrm{y}\\cdot\\mathrm{keV})$ below 30 keV. An excess of electronic r ecoils was found below 7 keV and most prominent between 2 and 3 keV. The e xcess could be induced by solar axions\, solar neutrinos with an enhanced magnetic moment\, or a trace amount of tritium background which could not be confirmed nor rejected. Consistent results were obtained by using ioniz ation signals only\, an approach which is more sensitive at low energies. XENONnT\, the upgraded version of XENON1T\, features a factor of 3 larger active mass and a factor of 6 reduced background\, and thus will be more s ensitive to low-energy electronic recoils. In this talk\, I will review th e excess electronic recoils in XENON1T and present the prospect to deciphe r the origin of the excess with data from XENONnT.\n\nhttps://indico.ific. uv.es/event/6178/contributions/15875/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15875/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of the DEAP-3600 experiment DTSTART;VALUE=DATE-TIME:20210827T114500Z DTEND;VALUE=DATE-TIME:20210827T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15851@indico.ific.uv.es DESCRIPTION:Speakers: Marcin Kuźniak (AstroCeNT / CAMK PAN)\nDEAP-3600 is a single-phase liquid argon (LAr) dark matter detector operating 2 km und erground at SNOLAB in Sudbury\, Canada. The detector consists of 3.3 tonne s of LAr in a spherical acrylic vessel viewed by an array of 255 photomult iplier tubes. DEAP-3600 has been taking data stably since November 2016. D EAP-3600 is sensitive to nuclear recoils from dark matter particles\, whic h cause the emission of prompt scintillation light. While DEAP-3600 demons trated excellent performance and holds the leading WIMP exclusion among LA r detectors\, its sensitivity is limited by backgrounds induced by alpha a ctivity at the LAr inlet\, in a shadowed region of detector. The upcoming hardware upgrade of the detector aims at fixing that limitation and\, in c onsequence\, at reaching the full WIMP sensitivity. This talk presents the latest results from DEAP-3600\, the status of the ongoing physics analyse s\, as well as of the hardware upgrade. Plans for the following physics ru n will also be discussed.\n\nhttps://indico.ific.uv.es/event/6178/contribu tions/15851/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15851/ END:VEVENT BEGIN:VEVENT SUMMARY:Building\, calibrating and searching for WIMPs and reactor CEvNS w ith Scintillating Bubble Chambers DTSTART;VALUE=DATE-TIME:20210827T120000Z DTEND;VALUE=DATE-TIME:20210827T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15844@indico.ific.uv.es DESCRIPTION:Speakers: Rocco Coppejans (Northwestern University)\nThe Scint illating Bubble Chamber (SBC) Collaboration is rapidly developing liquid-n oble bubble chambers to detect sub-keV nuclear recoils. Demonstrations in liquid xenon at the few-gram scale have confirmed that this technique comb ines the event-by-event energy resolution of a liquid-noble scintillation detector with the world-leading electron-recoil discrimination capability of the bubble chamber\, and in fact maintains that discrimination capabili ty at much lower thresholds than traditional Freon-based bubble chambers. The promise of unambiguous identification of sub-keV nuclear recoils in a scalable detector makes this an ideal technology for both GeV-mass WIMP se arches and CEvNS detection at reactor sites. We will present calibration r esults from the xenon chamber\, progress in building SBC's first 10-kg liq uid argon bubble chamber at Fermilab\, WIMP sensitivity projections for a dark matter search at SNOLAB\, and CEvNS science and site selection studie s at reactors in Mexico.\n\nhttps://indico.ific.uv.es/event/6178/contribut ions/15844/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15844/ END:VEVENT BEGIN:VEVENT SUMMARY:Fast neutrino flavor conversion induced by the coherent backward s catterings in the core-collapse supernovae DTSTART;VALUE=DATE-TIME:20210831T120000Z DTEND;VALUE=DATE-TIME:20210831T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15600@indico.ific.uv.es DESCRIPTION:Speakers: Masamichi Zaizen (University of Tokyo)\nIn the envir onment with dense neutrino gases such as in core-collapse supernovae (CCSN e)\, the neutrino self-interactions are potentially dominant\, and collect ive flavor conversions occur near the core. In particular\, the crossings in the neutrino angular distribution can induce fast flavor conversion. Th e coherent scatterings off heavy nuclei in the preshock region of CCSNe ca n create tiny negative crossings in the backward direction and lead to fas t instability. We demonstrate the flavor evolution triggered by the fast i nstability and a cascade due to the nonlinear effects.\n\nhttps://indico.i fic.uv.es/event/6178/contributions/15600/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15600/ END:VEVENT BEGIN:VEVENT SUMMARY:IceCube constraints on Violation of Equivalence Principle DTSTART;VALUE=DATE-TIME:20210831T114500Z DTEND;VALUE=DATE-TIME:20210831T120000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15523@indico.ific.uv.es DESCRIPTION:Speakers: Damiano F.G. Fiorillo (University of Naples "Federic o II")\nAmong the information provided by high energy neutrinos\, a promis ing possibility is to analyze the effects of a Violation of Equivalence Pr inciple (VEP) on neutrino oscillations. We analyze the IceCube data on atm ospheric neutrino fluxes under the assumption of a VEP and obtain updated constraints on the parameter space with the benchmark choice that neutrino s with different masses couple with different strengths to the gravitation al field. In this case we find that the VEP parameters times the local gra vitational potential at Earth can be constrained at the level of $10^{-27} $. We show that the constraints from atmospheric neutrinos strongly depend on the assumption that the neutrino eigenstates interacting diagonally wi th the gravitational field coincide with the mass eigenstates\, which is n ot a priori justified: this is particularly clear in the case that the bas is of diagonal gravitational interaction coincide with the flavor basis\, which cannot be constrained by the observation of atmospheric neutrinos. F inally\, we quantitatively study the effect of a VEP on the flavor composi tion of the astrophysical neutrinos\, stressing again the interplay with t he basis in which the VEP is diagonal: we find that for some choices of su ch basis the flavor ratio measured by IceCube can significantly change.\n\ nhttps://indico.ific.uv.es/event/6178/contributions/15523/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15523/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing secret interactions of astrophysical neutrinos in the high -statistics era DTSTART;VALUE=DATE-TIME:20210831T113000Z DTEND;VALUE=DATE-TIME:20210831T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15635@indico.ific.uv.es DESCRIPTION:Speakers: Iván Esteban (CCAPP\, Ohio State University)\nDo ne utrinos have sizable self-interactions? This fundamental question\, whose answer directly affects future precise astrophysical and cosmological obse rvations\, is difficult to directly test in the laboratory. For the last y ears\, neutrino telescopes have been identified as unique tools to explore neutrino self-interactions. The actual discovery of astrophysical neutrin os and the advent of future neutrino telescopes\, together with a more pre cise understanding of neutrino masses from laboratory and cosmological pro bes\, calls for a robust theoretical description of the underlying particl e physics and its connections with other neutrino observables. In this wor k\, we set up such theoretical framework for present and future studies. W e quantify the relevance of previously ignored effects\, and we clarify th e interplay with other experimental probes of neutrino properties. These d irectly affect the interpretation of present data in terms of self-interac tions\, as well as the testability of current "hints" in future facilities . After applying our formalism\, we find that current IceCube data shows n o evidence of neutrino self-interactions\, and it is beginning to exclude self-interactions that have been argued to affect cosmological parameter e xtraction (most notably $H_0$). Furthermore\, our results show that the fu ture IceCube Gen2 observatory should be sensitive to many cosmologically r elevant neutrino self-interaction models.\n\nhttps://indico.ific.uv.es/eve nt/6178/contributions/15635/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15635/ END:VEVENT BEGIN:VEVENT SUMMARY:HOLMES: progresses towards a calorimetric neutrino mass measuremen t with eV scale mass sensitivity DTSTART;VALUE=DATE-TIME:20210827T120500Z DTEND;VALUE=DATE-TIME:20210827T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15715@indico.ific.uv.es DESCRIPTION:Speakers: Angelo Nucciotti (Dipartimento di Fisica\, Universit à di Milano-Bicocca\, Milano\, Italy)\nThe assessment of the absolute neu trino mass scale is still a crucial challenge in today’s particle physic s and cosmology. Beta or electron capture decay spectra end-point measure ments are currently the only experimental methods which can provide a mode l-independent measurement of the absolute neutrino mass scale. \nWhile KAT RIN is successfully pushing the mass sensitivity below 1 eV\, there is a s trong need for radically different direct experiments to confirm and stren gthen present and future KATRIN's results. $^{163}$Ho electron capture cal orimetric experiments are among the best candidates for this task. In cal orimetric measurements\, the energy released in the decay process is entir ely contained into the detector\, except for the fraction carried away by the neutrino: this provides an independent direct measurement that has com pletely different systematic uncertainties. The most suitable detectors f or this type of measurement are low-temperature thermal detectors\, where all the energy released in an absorber is converted into a temperature inc rease that can be measured by a sensitive thermometer directly coupled wit h the absorber. HOLMES will deploy a large array of low temperature micro calorimeters with ion-implanted $^{163}$Ho nuclei. \nThe ultimate goal of HOLMES is a statistical neutrino mass sensitivity of 1 eV to be achieved w ith an array of 1000 pixels\, each with a $^{163}$Ho ion-implanted activi ty of about 300 Bq. As a near-term goal\, HOLMES is preparing to ion-impl ant a lower dose to give an activity of a few Bequerels per pixel. A meas urement with such an array is planned to begin by 2021 and will provide a sensitivity of less than 10 eV.\nIn this contribution we outline the HOLME S project with its physics reach and technical challenges\, along with its status and prospects. In particular\, we will present the status of HOLM ES activities aiming at the production of the first low-dose ion-implanted TES array and at the first neutrino mass measurement campaign. We will a lso discuss the prospects and strategies for a future $^{163}$Ho experimen t with a sub-eV neutrino mass sensitivity.\n\nhttps://indico.ific.uv.es/ev ent/6178/contributions/15715/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15715/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino mass determination with Holmium-163 - the ECHo experiment DTSTART;VALUE=DATE-TIME:20210827T115500Z DTEND;VALUE=DATE-TIME:20210827T120500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15470@indico.ific.uv.es DESCRIPTION:Speakers: Loredana Gastaldo (Kirchhoff-Institute for Physics\, Heidelberg University)\nThe Electron Capture in $^{163}$Ho experiment\, E CHo\, is a running experiment for the determination of the neutrino mass s cale via the analysis of the end point region of the $^{163}$Ho electron c apture spectrum. In the first phase\, ECHo-1k\, about 60 MMCs pixels enclo sing $^{163}$Ho ions for an activity of about 1Bq per pixel have been oper ated for several months. The goal of this first phase is to reach a sensit ivity on the effective electron neutrino mass below 20 eV/c$^2$ by the ana lysis of a $^{163}$Ho spectrum with more than 10$^8$ events. We discuss th e characterization of the single pixel performance and the stability over the measuring period. Results from the analysis of the acquired data will be presented with focus on data reduction efficiency and on the procedures to obtain the final high statistics spectrum. A preliminary analysis of t he $^{163}$Ho spectral shape will be described and the expected sensitivit y on the effective electron neutrino mass\, on the basis of the properties of the presented spectrum\, will be discussed. In conclusion\, we will pr esent how the performance obtained by the MMC arrays used during the first phase of the ECHo experiment have led to the design of the MMC arrays for the second phase\, ECHo-100K. In ECHo-100k about 12000 MMC pixels each ho sting $^{163}$Ho for an activity of 10 Bq will be simultaneously operated thanks to the microwave SQUID multiplexing readout. Operating these arrays for three years will allow for reaching a sensitivity on the electron neu trino mass at the 1 eV/c$^2$ level.\n\nhttps://indico.ific.uv.es/event/617 8/contributions/15470/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15470/ END:VEVENT BEGIN:VEVENT SUMMARY:Project 8: the path to improved neutrino mass DTSTART;VALUE=DATE-TIME:20210827T114500Z DTEND;VALUE=DATE-TIME:20210827T115500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15484@indico.ific.uv.es DESCRIPTION:Speakers: Elise Novitski (University of Washington)\nProject 8 is a direct neutrino mass experiment that has developed a new technique\, Cyclotron Radiation Emission Spectroscopy (CRES)\, to make a differential measurement of the tritium $\\beta^{-}$ spectrum. Project 8 aims to use t he advantages of CRES to surmount the systematic and statistical limitatio ns of current-generation direct neutrino mass measurement methods\, procee ding in a phased approach toward a goal of effective electron antineutrino mass sensitivity of ${\\sim}$40 meV/c$^2$ using atomic tritium. This talk will report on the progress toward Phase III free-space CRES and atomic t ritium demonstrations\, which will enable the advances in energy resolutio n and statistics needed to achieve full Phase IV sensitivity.\n\nThis work is supported by the US DOE Office of Nuclear Physics\, the US NSF\, the P RISMA+ Cluster of Excellence at the University of Mainz\, and internal inv estments at all institutions.\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15484/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15484/ END:VEVENT BEGIN:VEVENT SUMMARY:The KATRIN experiment: neutrino mass measurements with sub-eV sens itivity DTSTART;VALUE=DATE-TIME:20210827T113000Z DTEND;VALUE=DATE-TIME:20210827T114500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15710@indico.ific.uv.es DESCRIPTION:Speakers: Alexey Lokhov (University of Muenster & INR\, Troits k)\nThe KArlsruhe TRItium Neutrino experiment (KATRIN) is searching for th e signature of the neutrino mass in the endpoint region of the tritium bet a-decay spectrum. KATRIN combines a high-intensity gaseous molecular triti um source with a high-resolution spectroscopy using electrostatic filter w ith magnetic adiabatic collimation to reach the target neutrino-mass sensi tivity of 0.2 eV/$c^2$\, improving on the previous measurements by an orde r of magnitude. With the first science run of KATRIN the previous neutrino mass bounds were improved by a factor of two\, with the first upper limit of 1.1 eV/$c^2$ (90% CL).\n\nIn this talk an overview of the KATRIN exper iment and its very recent results are presented. Our new results reaching a sub-eV neutrino-mass sensitivity based on the whole 2019 data-set will b e discussed. In addition\, the talk reports on the KATRIN exploration of i nteresting BSM physics cases and closes with an outlook on the future pros pects of KATRIN.\n\nhttps://indico.ific.uv.es/event/6178/contributions/157 10/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15710/ END:VEVENT BEGIN:VEVENT SUMMARY:Panel on Diversity and Inclusion in Astroparticle Physics DTSTART;VALUE=DATE-TIME:20210903T143000Z DTEND;VALUE=DATE-TIME:20210903T153000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16017@indico.ific.uv.es DESCRIPTION:Speakers: Alba Fernández-Barral (CTA Observatory)\, Inés Gil Botella (CIEMAT)\, Jonas H. Rademacker (University of Bristol)\, Kamiel J anssens (Universiteit Antwerpen)\, Mayly Sanchez (Iowa State University)\, Srubabati Goswami (Physical Research Laboratory)\, Summer Blot (DESY-Zeut hen)\nParticipants: Alba Fernández-Barral\, Kamiel Janssens\, Mayly Sanch ez\, Srubabati Goswami\, Summer Blot and Jonas Rademacker\n\nModerator: In és Gil Botella\n\nhttps://indico.ific.uv.es/event/6178/contributions/1601 7/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16017/ END:VEVENT BEGIN:VEVENT SUMMARY:Welcome and Opening remarks DTSTART;VALUE=DATE-TIME:20210826T120000Z DTEND;VALUE=DATE-TIME:20210826T123000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16012@indico.ific.uv.es DESCRIPTION:Speakers: Mariam Tórtola (IFIC (CSIC-Univ. Valencia))\, Sergi o Pastor (IFIC (CSIC-Univ. Valencia))\nhttps://indico.ific.uv.es/event/617 8/contributions/16012/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16012/ END:VEVENT BEGIN:VEVENT SUMMARY:Coherent elastic neutrino-nucleus scattering DTSTART;VALUE=DATE-TIME:20210826T150000Z DTEND;VALUE=DATE-TIME:20210826T153000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15985@indico.ific.uv.es DESCRIPTION:Speakers: Carla Bonifazi (ICAS - ICIFI - UNSAM / CONICET)\nCha ir: Carlo Giunti\n\nhttps://indico.ific.uv.es/event/6178/contributions/159 85/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15985/ END:VEVENT BEGIN:VEVENT SUMMARY:Long-baseline neutrino oscillations review (including future) DTSTART;VALUE=DATE-TIME:20210826T143000Z DTEND;VALUE=DATE-TIME:20210826T150000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15983@indico.ific.uv.es DESCRIPTION:Speakers: Patricia Vahle (College of William and Mary)\nChair: Carlo Giunti\n\nhttps://indico.ific.uv.es/event/6178/contributions/15983/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15983/ END:VEVENT BEGIN:VEVENT SUMMARY:Light sterile neutrinos DTSTART;VALUE=DATE-TIME:20210826T140000Z DTEND;VALUE=DATE-TIME:20210826T143000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15982@indico.ific.uv.es DESCRIPTION:Speakers: Stefano Gariazzo (INFN Torino)\nChair: Carlo Giunti\ n\nhttps://indico.ific.uv.es/event/6178/contributions/15982/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15982/ END:VEVENT BEGIN:VEVENT SUMMARY:Solar and geoneutrinos DTSTART;VALUE=DATE-TIME:20210826T130000Z DTEND;VALUE=DATE-TIME:20210826T133000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15981@indico.ific.uv.es DESCRIPTION:Speakers: Livia Ludhova (Forschungszentrum Juelich and RWTH Aa chen)\nChair: Sandhya Choubey\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15981/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15981/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino theory DTSTART;VALUE=DATE-TIME:20210826T123000Z DTEND;VALUE=DATE-TIME:20210826T130000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15979@indico.ific.uv.es DESCRIPTION:Speakers: Raymond R. Volkas (Univ Melbourne)\nChair: Sandhya C houbey\n\nhttps://indico.ific.uv.es/event/6178/contributions/15979/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15979/ END:VEVENT BEGIN:VEVENT SUMMARY:Tribute to Samoil Bilenky DTSTART;VALUE=DATE-TIME:20210903T121500Z DTEND;VALUE=DATE-TIME:20210903T123000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16015@indico.ific.uv.es DESCRIPTION:Speakers: Carlo Giunti (INFN Turin)\nChair: Juan José Hernand ez-Rey\n\nhttps://indico.ific.uv.es/event/6178/contributions/16015/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16015/ END:VEVENT BEGIN:VEVENT SUMMARY:Tribute to Masatoshi Koshiba DTSTART;VALUE=DATE-TIME:20210903T120000Z DTEND;VALUE=DATE-TIME:20210903T121500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16014@indico.ific.uv.es DESCRIPTION:Speakers: Takaaki Kajita (ICRR and IPMU\, Univ Tokyo)\nChair: Juan José Hernandez-Rey\n\nhttps://indico.ific.uv.es/event/6178/contribut ions/16014/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16014/ END:VEVENT BEGIN:VEVENT SUMMARY:Closing and Farewell DTSTART;VALUE=DATE-TIME:20210903T153000Z DTEND;VALUE=DATE-TIME:20210903T154500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16013@indico.ific.uv.es DESCRIPTION:Speakers: Nicolao Fornengo (Univ Torino and INFN)\nChair: Jos é W.F. Valle\n\nhttps://indico.ific.uv.es/event/6178/contributions/16013/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16013/ END:VEVENT BEGIN:VEVENT SUMMARY:Ultra-high energy cosmic rays DTSTART;VALUE=DATE-TIME:20210903T140000Z DTEND;VALUE=DATE-TIME:20210903T143000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16011@indico.ific.uv.es DESCRIPTION:Speakers: Silvia Mollerach (Centro Atómico Bariloche\, CONICE T)\nChair: M.D. Rodríguez Frías\n\nhttps://indico.ific.uv.es/event/6178/ contributions/16011/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16011/ END:VEVENT BEGIN:VEVENT SUMMARY:High-energy neutrinos DTSTART;VALUE=DATE-TIME:20210903T130000Z DTEND;VALUE=DATE-TIME:20210903T133000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16010@indico.ific.uv.es DESCRIPTION:Speakers: Justin A. Vandenbroucke (Univ Wisconsin)\nChair: Jua n José Hernandez-Rey\n\nhttps://indico.ific.uv.es/event/6178/contribution s/16010/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16010/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct measurements of cosmic rays from space DTSTART;VALUE=DATE-TIME:20210903T123000Z DTEND;VALUE=DATE-TIME:20210903T130000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16009@indico.ific.uv.es DESCRIPTION:Speakers: Valerio Formato (INFN - Roma Tor Vergata)\nChair: J uan José Hernandez-Rey\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/16009/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16009/ END:VEVENT BEGIN:VEVENT SUMMARY:Gravitational waves: technology and current detectors DTSTART;VALUE=DATE-TIME:20210902T143000Z DTEND;VALUE=DATE-TIME:20210902T150000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16008@indico.ific.uv.es DESCRIPTION:Speakers: Lisa Barsotti (MIT Cambridge)\nChair: Jan Harms\n\nh ttps://indico.ific.uv.es/event/6178/contributions/16008/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16008/ END:VEVENT BEGIN:VEVENT SUMMARY:Future GW detectors in space and ground DTSTART;VALUE=DATE-TIME:20210902T140000Z DTEND;VALUE=DATE-TIME:20210902T143000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16007@indico.ific.uv.es DESCRIPTION:Speakers: Harald Lück (MPI for Gravitational Physics)\nChair: Jan Harms\n\nhttps://indico.ific.uv.es/event/6178/contributions/16007/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16007/ END:VEVENT BEGIN:VEVENT SUMMARY:Gravitational-wave and multi-messenger observations: results and p rospects DTSTART;VALUE=DATE-TIME:20210901T130000Z DTEND;VALUE=DATE-TIME:20210901T133000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16006@indico.ific.uv.es DESCRIPTION:Speakers: Marica Branchesi (GSSI and Gran Sasso Lab)\nChair: C laudia Lazzaro\n\nhttps://indico.ific.uv.es/event/6178/contributions/16006 / LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16006/ END:VEVENT BEGIN:VEVENT SUMMARY:GW astrophysics (future discoveries) DTSTART;VALUE=DATE-TIME:20210901T123000Z DTEND;VALUE=DATE-TIME:20210901T130000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16005@indico.ific.uv.es DESCRIPTION:Speakers: Paul Lasky (Monash Univ)\nChair: Claudia Lazzaro\n\n https://indico.ific.uv.es/event/6178/contributions/16005/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16005/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter search in accelerators and beyond DTSTART;VALUE=DATE-TIME:20210902T123000Z DTEND;VALUE=DATE-TIME:20210902T130000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16004@indico.ific.uv.es DESCRIPTION:Speakers: Gaia Lanfranchi (LNF)\nChair: Carlos Muñoz\n\nhttps ://indico.ific.uv.es/event/6178/contributions/16004/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16004/ END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray astronomy from the ground DTSTART;VALUE=DATE-TIME:20210901T143000Z DTEND;VALUE=DATE-TIME:20210901T150000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16003@indico.ific.uv.es DESCRIPTION:Speakers: Gabrijela Zaharijaš (Nova Gorica U)\nChair: Carlos Delgado\n\nhttps://indico.ific.uv.es/event/6178/contributions/16003/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16003/ END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray astronomy from space DTSTART;VALUE=DATE-TIME:20210901T140000Z DTEND;VALUE=DATE-TIME:20210901T143000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16002@indico.ific.uv.es DESCRIPTION:Speakers: Regina Caputo (NASA Goddard Space Flight Center)\nCh air: Carlos Delgado\n\nhttps://indico.ific.uv.es/event/6178/contributions/ 16002/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16002/ END:VEVENT BEGIN:VEVENT SUMMARY:Indirect detection of dark matter DTSTART;VALUE=DATE-TIME:20210902T130000Z DTEND;VALUE=DATE-TIME:20210902T133000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16001@indico.ific.uv.es DESCRIPTION:Speakers: Francesca Calore (LAPTH Annecy)\nChair: Carlos Muño z\n\nhttps://indico.ific.uv.es/event/6178/contributions/16001/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16001/ END:VEVENT BEGIN:VEVENT SUMMARY:Light dark matter (theory & exp) DTSTART;VALUE=DATE-TIME:20210831T143000Z DTEND;VALUE=DATE-TIME:20210831T150000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-16000@indico.ific.uv.es DESCRIPTION:Speakers: Yonit Hochberg (Hebrew U\, Jerusalem)\nChair: Jodi C ooley\n\nhttps://indico.ific.uv.es/event/6178/contributions/16000/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/16000/ END:VEVENT BEGIN:VEVENT SUMMARY:Axions as dark matter (theory & exp) DTSTART;VALUE=DATE-TIME:20210831T140000Z DTEND;VALUE=DATE-TIME:20210831T143000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15999@indico.ific.uv.es DESCRIPTION:Speakers: Javier Redondo (Univ Zaragoza)\nChair: Jodi Cooley\n \nhttps://indico.ific.uv.es/event/6178/contributions/15999/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15999/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct detection of dark matter (experimental review) DTSTART;VALUE=DATE-TIME:20210831T130000Z DTEND;VALUE=DATE-TIME:20210831T133000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15998@indico.ific.uv.es DESCRIPTION:Speakers: Marc Schumann (Univ Freiburg)\nChair: Masaki Yamashi ta\n\nhttps://indico.ific.uv.es/event/6178/contributions/15998/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15998/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter models (theory review) DTSTART;VALUE=DATE-TIME:20210831T123000Z DTEND;VALUE=DATE-TIME:20210831T130000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15997@indico.ific.uv.es DESCRIPTION:Speakers: Maxim Pospelov (Univ Minnesota)\nChair: Masaki Yamas hita\n\nhttps://indico.ific.uv.es/event/6178/contributions/15997/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15997/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter and structure formation DTSTART;VALUE=DATE-TIME:20210830T140000Z DTEND;VALUE=DATE-TIME:20210830T143000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15996@indico.ific.uv.es DESCRIPTION:Speakers: Matteo Viel (SISSA Trieste)\nChair: Martina Gerbino\ n\nhttps://indico.ific.uv.es/event/6178/contributions/15996/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15996/ END:VEVENT BEGIN:VEVENT SUMMARY:Multimessenger astronomy DTSTART;VALUE=DATE-TIME:20210830T143000Z DTEND;VALUE=DATE-TIME:20210830T150000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15995@indico.ific.uv.es DESCRIPTION:Speakers: Andrii Neronov (APC Paris & Univ Geneve)\nChair: Mar tina Gerbino\n\nhttps://indico.ific.uv.es/event/6178/contributions/15995/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15995/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmology overview DTSTART;VALUE=DATE-TIME:20210830T130000Z DTEND;VALUE=DATE-TIME:20210830T133000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15994@indico.ific.uv.es DESCRIPTION:Speakers: Licia Verde (ICC\, IEEC-Univ Barcelona - ICREA)\nCha ir: Olga Mena\n\nhttps://indico.ific.uv.es/event/6178/contributions/15994/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15994/ END:VEVENT BEGIN:VEVENT SUMMARY:Inflation overview DTSTART;VALUE=DATE-TIME:20210830T123000Z DTEND;VALUE=DATE-TIME:20210830T130000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15993@indico.ific.uv.es DESCRIPTION:Speakers: Richard Easther (Univ Auckland)\nChair: Olga Mena\n\ nhttps://indico.ific.uv.es/event/6178/contributions/15993/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15993/ END:VEVENT BEGIN:VEVENT SUMMARY:Review on underground laboratories DTSTART;VALUE=DATE-TIME:20210827T150000Z DTEND;VALUE=DATE-TIME:20210827T153000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15990@indico.ific.uv.es DESCRIPTION:Speakers: Ezio Previtali (Univ Milano Bicocca & Gran Sasso Lab )\nChair: Junpei Shirai\n\nhttps://indico.ific.uv.es/event/6178/contributi ons/15990/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15990/ END:VEVENT BEGIN:VEVENT SUMMARY:Reactor experiments review (including short-baseline) DTSTART;VALUE=DATE-TIME:20210827T143000Z DTEND;VALUE=DATE-TIME:20210827T150000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15989@indico.ific.uv.es DESCRIPTION:Speakers: Cécile Jollet (Univ Bordeaux)\nChair: Junpei Shirai \n\nhttps://indico.ific.uv.es/event/6178/contributions/15989/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15989/ END:VEVENT BEGIN:VEVENT SUMMARY:Supernovae: neutrinos and gravitational waves DTSTART;VALUE=DATE-TIME:20210827T140000Z DTEND;VALUE=DATE-TIME:20210827T143000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15988@indico.ific.uv.es DESCRIPTION:Speakers: Kei Kotake (Fukuoka University)\nChair: Junpei Shira i\n\nhttps://indico.ific.uv.es/event/6178/contributions/15988/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15988/ END:VEVENT BEGIN:VEVENT SUMMARY:Double beta decay: experimental review DTSTART;VALUE=DATE-TIME:20210827T130000Z DTEND;VALUE=DATE-TIME:20210827T133000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15987@indico.ific.uv.es DESCRIPTION:Speakers: Andrea Giuliani (IJCLab\, U Paris-Saclay\, Orsay)\nC hair: Martin Hirsch\n\nhttps://indico.ific.uv.es/event/6178/contributions/ 15987/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15987/ END:VEVENT BEGIN:VEVENT SUMMARY:Double beta decay: theory review DTSTART;VALUE=DATE-TIME:20210827T123000Z DTEND;VALUE=DATE-TIME:20210827T130000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15986@indico.ific.uv.es DESCRIPTION:Speakers: Frank Deppisch (University College London)\nChair: M artin Hirsch\n\nhttps://indico.ific.uv.es/event/6178/contributions/15986/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15986/ END:VEVENT BEGIN:VEVENT SUMMARY:Measuring high-energy neutrinos with FASERnu in the LHC Run-3 DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15785@indico.ific.uv.es DESCRIPTION:Speakers: Umut Kose (CERN EP-NU)\nFASER$\\nu$ at the LHC is de signed to directly detect collider neutrinos for the first time and study their cross sections at high energies\, where no such measurements current ly exist. The detector will be located in the far-forward region of ATLAS. Deployment on the beam collision axis maximizes the flux of all three neu trino flavors\, and allows FASER$\\nu$ to measure their interaction cross- sections in the currently unexplored TeV energy range. For electron and ta u neutrinos\, these measurements will extend existing cross section measur ements to significantly higher energies. In 2018 we performed a pilot run with the aims of measuring particle fluxes at the proposed detector locati on and of possibly detecting neutrino interactions for the first time at t he LHC. We installed a 30-kg lead/tungsten emulsion detector and collected data of 12.2 fb$^{-1}$. The analysis of this data has yielded several neu trino interaction candidates\, excluding the no-signal hypothesis at the 2 $\\sigma$ level. During Run-3 of the LHC starting from 2022\, we will depl oy an emulsion detector with a target mass of 1.1 tons\, coupled with the FASER magnetic spectrometer. This would yield roughly 2\,000 $\\nu_e$\, 8\ ,000 $\\nu_{\\mu}$\, and 50 $\\nu_{\\tau}$ interacting in the detector. We present the status and prospects of FASER$\\nu$\, as well as the neutrino detection in the pilot run data.\n\nhttps://indico.ific.uv.es/event/6178/ contributions/15785/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15785/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for exotic neutrino-electron interactions using solar neutr inos in XMASS-I DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15625@indico.ific.uv.es DESCRIPTION:Speakers: Hiroshi Ogawa (Nihon University)\nIn recent years\, the larger size and lower background of dark matter search detectors have opened up a new frontier of searching for new physics other than dark matt er search using these detectors. One of them is the search for new propert ies of neutrinos by observing the interaction of neutrinos at low energy. XMASS is multi-purpose experiment using single phase liquid xenon (LXe) an d is located at the Kamioka Observatory in Japan. We searched for exotic n eutrino-electron interactions that could be produced by a neutrino millich arge\, by a neutrino magnetic moment\, or by dark photons using solar neut rinos in XMASS. We analyzed the data between November 2013 and March 2016 for 711days dataset and no significant signals have been observed with pre dicting the backgrounds in detector. We obtained an upper limit of neutrin o millicharge of $5.4\\times10^{-11}$e for all flavors of neutrino. We als o set individual flavors which the limits for $\\nu_{\\mu}$ and $\\nu_{\\t au}$ are the best direct experimental limits. We also obtain an upper limi t for the neutrino magnetic moment of 1.8$\\times$10$^{-10} \\mu_{B}$. In addition\, we obtain upper limits for the coupling constant of dark photon s in the $U(1)_{B-L}$ model. This result almost excludes the possibility t o understand the muon $g-2$ anomaly by dark photons.\n\nhttps://indico.ifi c.uv.es/event/6178/contributions/15625/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15625/ END:VEVENT BEGIN:VEVENT SUMMARY:The role of leptonic CPV phases in cLFV observables DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15624@indico.ific.uv.es DESCRIPTION:Speakers: Jonathan Kriewald (LPC Clermont-Ferrand)\nIn models where the Standard Model is extended by Majorana fermions\, interference e ffects due to the presence of\nCP violating phases have been shown to play a crucial role in lepton number violating processes.\nHowever\, important interference effects can also arise in lepton number conserving\, but cha rged lepton flavour violating (cLFV) transitions and decays.\nIn this work we show that in the presence of CP violating (Dirac and Majorana) phases important interference effects might arise\, with a striking\nimpact for t he predicted rates of cLFV observables.\nWe explore the interference effec ts in several cLFV observables\, carrying for the first time a thorough an alysis of the different observables and the implications for future observ ation.\nWe show in this talk how the presence of leptonic CP violating pha ses might lead to a loss of correlation between observables (typically pre sent in simple SM extensions via heavy sterile fermions)\,\nor even to the suppression of certain channels\; these effects can be interpreted as sug gestive of non-vanishing phases.\n\nhttps://indico.ific.uv.es/event/6178/c ontributions/15624/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15624/ END:VEVENT BEGIN:VEVENT SUMMARY:First Neutron Capture Results of ANNIE DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15593@indico.ific.uv.es DESCRIPTION:Speakers: Leon Pickard (UC Davis)\nANNIE is a 26 ton Gd-loaded water Cherenkov detector installed in the Booster Neutrino Beam at Fermil ab. It will measure the neutron multiplicity\, as a function of momentum t ransfer\, of neutrino-neutron interactions on water. To achieve this\, it is imperative that the neutron capture characteristics in the detector vol ume are well parameterised. This talk will introduce the Americium Berylli um calibration source\, highlight its successful deployment\, and present the resulting neutron detection efficiency map and measured neutron captur e time.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15593/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15593/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent neutrino cross-section results from MicroBooNE DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15581@indico.ific.uv.es DESCRIPTION:Speakers: Lu Ren (New Mexico State University)\nMicroBooNE is a liquid argon time projection chamber that operates in the Booster Neutri no Beam at Fermilab. The detector provides high-resolution imaging of neut rino interactions with a low threshold and full angular coverage. Thanks t o a high event rate and several years of continuous operation\, the MicroB ooNE collaboration has obtained the world’s largest dataset of neutrino- argon scattering events. A detailed understanding of these interactions\, especially the impact of nuclear physics effects\, will be critical to the success of future precision neutrino oscillation efforts\, particularly t he argon-based Deep Underground Neutrino Experiment (DUNE) and the Short-B aseline Neutrino (SBN) program. This talk presents an overview of the late st neutrino-argon cross section measurements in MicroBooNE\, including mea surements of protons produced in muon neutrino interactions\, measurements of the electron neutrino inclusive cross section\, and progress towards m easurements of rare channels.\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15581/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15581/ END:VEVENT BEGIN:VEVENT SUMMARY:T2K latest results on neutrino-nucleus cross sections DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15576@indico.ific.uv.es DESCRIPTION:Speakers: Samuel Jenkins ()\nA detailed understanding of neutr ino(ν)-nucleus interactions is essential for the precise measurement of n eutrino oscillations at long baseline experiments\, such as T2K. The T2K n ear detector complex\, designed to constrain the T2K flux and cross sectio n models\, also provides a complementary program of neutrino interaction c ross-section measurements. Through the use of multiple target materials (c arbon\, water\, argon\, iron\, lead)\, and the ability to sample different neutrino spectra (with detectors located on- and off-axis with respected to the flux)\, T2K is able to investigate atomic number and energy depende nce of interaction cross sections in single experiment. An overview of the T2K measurement strategy\, adopted to reduce the model dependence\, and t he most recent results\, as well as future planned analyses\, will be pres ented.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15576/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15576/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutron Beam Test with a Scintillator Tracker for Long-Baseline Ne utrino Experiments DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15564@indico.ific.uv.es DESCRIPTION:Speakers: Martin Tzanov (Louisiana State University)\nThe focu s of the long-baseline neutrino oscillation experiments that are currently being built is the precise measurement of the neutrino oscillation parame ters which will require good control of the systematic uncertainties inclu ding those of the neutrino interaction models. A novel three-dimensional p rojection scintillation tracker will be the active target of the ND280 nea r detector upgrade for the T2K experiment and is being considered as one o f the on-axis near detector modules for the DUNE experiment. This detector features fine granularity and good timing resolution allowing for better reconstruction of the final state products of neutrino interactions on eve nt-by-event basis including the ability to reconstruct neutrons. Two proto types took neutron beam data in 2019 and 2020 at the Los Alamos National L ab (LANL) to study the detector response to neutrons with energies from 0 to 800MeV. The details of the detector response calibration and the measur ement of the total neutron cross section are presented.\n\nhttps://indico. ific.uv.es/event/6178/contributions/15564/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15564/ END:VEVENT BEGIN:VEVENT SUMMARY:Study of tau neutrino production with nuclear emulsion at CERN-SPS DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15543@indico.ific.uv.es DESCRIPTION:Speakers: Svetlana Vasina (JINR\, Dubna)\nThe data on tau neut rino is very scarce\, only a few experiments have detected its interaction s. At FNAL beam dump experiment DONUT\, tau neutrino interaction cross-sec tion was directly measured with a large systematical (~50%) and statistica l (~30%) errors. The main source of systematical error is due to a poor kn owledge of the tau neutrino flux. The effective way for tau neutrino produ ction is the decay of Ds mesons\, produced in proton-nucleus interactions. The DsTau experiment at CERN-SPS has been proposed to measure an inclusiv e differential cross-section of a Ds production with a consecutive decay t o tau lepton in p-A interactions. The goal of experiment is to reduce the systematic uncertainty to 10% level. A precise measurement of the tau neu trino cross section would enable a search for new physics effects such as testing the Lepton Universality (LU) of Standard Model in neutrino interactions. The detector is based on nuclear emulsion providing a sub -micron spatial resolution for the detection of short length and small “ kink” decays. Therefore\, it is very suitable to search for peculiar dec ay topologies (“double kink”) of Ds→τ →X. After successful pilot runs and data analysis\, CERN had approved the DsTau project as a new exp eriment NA65 in 2019. During the physics runs\, 2.3×10^8 proton interact ions will be collected in the tungsten target\, and about 1000 Ds→τ dec ays will be detected. In this talk\, the results from the pilot run will b e presented and the prospect for physics runs in 2021-2022 will be given.\ n\nhttps://indico.ific.uv.es/event/6178/contributions/15543/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15543/ END:VEVENT BEGIN:VEVENT SUMMARY:Nonstandard neutrino Interactions as a solution to the NOvA and T2 K tension DTSTART;VALUE=DATE-TIME:20210902T154500Z DTEND;VALUE=DATE-TIME:20210902T160000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15535@indico.ific.uv.es DESCRIPTION:Speakers: Antonio Palazzo (University of Bari andINFN)\nThe la test data of the two long-baseline accelerator experiments NOvA and T2K\, interpreted in the standard 3-flavor scenario\, display a tension. A misma tch in the determination of the standard CP-phase delta_CP extracted by th e two experiments is evident in the normal neutrino mass ordering. In this talk\, we show that such a discrepancy can be resolved if one hypothesize s the existence of complex neutral-current non-standard interactions (NSI) of the flavor changing type.\n\nhttps://indico.ific.uv.es/event/6178/cont ributions/15535/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15535/ END:VEVENT BEGIN:VEVENT SUMMARY:The SND@LHC experiment at CERN DTSTART;VALUE=DATE-TIME:20210902T154000Z DTEND;VALUE=DATE-TIME:20210902T155500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15522@indico.ific.uv.es DESCRIPTION:Speakers: Dario De Simone (Univ Zürich)\nSND@LHC is a compact and stand-alone experiment to perform measurements with neutrinos produce d at the LHC in a hitherto unexplored pseudo-rapidity region of 7.2 \n\nht tps://indico.ific.uv.es/event/6178/contributions/15522/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15522/ END:VEVENT BEGIN:VEVENT SUMMARY:Heavy Dirac/Majorana Fermion Decays DTSTART;VALUE=DATE-TIME:20210902T152500Z DTEND;VALUE=DATE-TIME:20210902T154000Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15521@indico.ific.uv.es DESCRIPTION:Speakers: Kevin Kelly (Fermilab)\nIf a heavy neutrino is disco vered\, determining its nature\, i.e.\, whether it is a Dirac or a Majoran a fermion\, will be at the top of the list of the next questions to ask. A natural way to determine this is to analyze the particle's decays and to observe whether they violate lepton number. However\, if the final state i ncludes any light neutrinos\, this is impossible. In that event\, we may s till be able to determine the nature by measuring the distribution of deca y events. I will show how this procedure may be performed in the context o f three-body decays of heavy neutrinos into a light neutrino and a pair of charged leptons.\n\nhttps://indico.ific.uv.es/event/6178/contributions/15 521/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15521/ END:VEVENT BEGIN:VEVENT SUMMARY:Time delay distributions of neutrino echoes induced by secret neut rino interactions DTSTART;VALUE=DATE-TIME:20210902T151000Z DTEND;VALUE=DATE-TIME:20210902T152500Z DTSTAMP;VALUE=DATE-TIME:20260316T152827Z UID:indico-contribution-6178-15520@indico.ific.uv.es DESCRIPTION:Speakers: Jose Carpio (Penn State University)\nWe examine the time delay distribution of astrophysical neutrinos as a result of Beyond S tandard Model interactions with the cosmic neutrino background. We focus o n the case of neutrino-neutrino interactions with a scalar mediator\, and develop a framework to handle the sharp increase in the cross section at r esonance energy. For a 10 MeV mediator mass and neutrino mass of 0.1 eV\, we find that the neutrino characteristic time delay differs from analytic estimates at large optical depths\, both in the elastic and inelastic scat tering regimes. As an application of our simulations\, we assumed an $E^{- 2}$ power law spectrum at $z=1$\, and found typical delays of 10s--1000s\, for neutrinos above 1 TeV\, for coupling strengths between 0.01 and 0.2.\ n\nhttps://indico.ific.uv.es/event/6178/contributions/15520/ LOCATION: URL:https://indico.ific.uv.es/event/6178/contributions/15520/ END:VEVENT END:VCALENDAR