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:20260611T042629Z UID:indico-contribution-2326-15718@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: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:20260611T042629Z UID:indico-contribution-2326-15924@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:20260611T042629Z UID:indico-contribution-2326-15879@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:20260611T042629Z UID:indico-contribution-2326-15711@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: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:20260611T042629Z UID:indico-contribution-2326-16018@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:20260611T042629Z UID:indico-contribution-2326-16016@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:20260611T042629Z UID:indico-contribution-2326-15972@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:20260611T042629Z UID:indico-contribution-2326-15923@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:20260611T042629Z UID:indico-contribution-2326-15915@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:20260611T042629Z UID:indico-contribution-2326-15907@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:20260611T042629Z UID:indico-contribution-2326-15904@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:20260611T042629Z UID:indico-contribution-2326-15890@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:20260611T042629Z UID:indico-contribution-2326-15885@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:20260611T042629Z UID:indico-contribution-2326-15876@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:20260611T042629Z UID:indico-contribution-2326-15870@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:20260611T042629Z UID:indico-contribution-2326-15761@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:20260611T042629Z UID:indico-contribution-2326-15759@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:20260611T042629Z UID:indico-contribution-2326-15756@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:20260611T042629Z UID:indico-contribution-2326-15741@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:20260611T042629Z UID:indico-contribution-2326-15737@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:20260611T042629Z UID:indico-contribution-2326-15731@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:20260611T042629Z UID:indico-contribution-2326-15724@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:20260611T042629Z UID:indico-contribution-2326-15719@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:20260611T042629Z UID:indico-contribution-2326-15700@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:20260611T042629Z UID:indico-contribution-2326-15659@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:20260611T042629Z UID:indico-contribution-2326-15658@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:20260611T042629Z UID:indico-contribution-2326-15657@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:20260611T042629Z UID:indico-contribution-2326-15656@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:20260611T042629Z UID:indico-contribution-2326-15655@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:20260611T042629Z UID:indico-contribution-2326-15653@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:20260611T042629Z UID:indico-contribution-2326-15652@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:20260611T042629Z UID:indico-contribution-2326-15622@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:20260611T042629Z UID:indico-contribution-2326-15620@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:20260611T042629Z UID:indico-contribution-2326-15615@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:20260611T042629Z UID:indico-contribution-2326-15614@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:20260611T042629Z UID:indico-contribution-2326-15611@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:20260611T042629Z UID:indico-contribution-2326-15609@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:20260611T042629Z UID:indico-contribution-2326-15603@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:20260611T042629Z UID:indico-contribution-2326-15602@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:20260611T042629Z UID:indico-contribution-2326-15598@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:20260611T042629Z UID:indico-contribution-2326-15562@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:20260611T042629Z UID:indico-contribution-2326-15559@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:20260611T042629Z UID:indico-contribution-2326-15558@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:20260611T042629Z UID:indico-contribution-2326-15557@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:20260611T042629Z UID:indico-contribution-2326-15556@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:20260611T042629Z UID:indico-contribution-2326-15554@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:20260611T042629Z UID:indico-contribution-2326-15553@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:20260611T042629Z UID:indico-contribution-2326-15544@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:20260611T042629Z UID:indico-contribution-2326-15538@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:20260611T042629Z UID:indico-contribution-2326-15508@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:20260611T042629Z UID:indico-contribution-2326-15492@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:20260611T042629Z UID:indico-contribution-2326-15488@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:20260611T042629Z UID:indico-contribution-2326-15487@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:20260611T042629Z UID:indico-contribution-2326-15481@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 END:VCALENDAR