TeVPA 2025 - Valencia, Spain

3 nov. 2025 8:00 → 7 nov. 2025 18:30 Europe/Madrid

Valencia, Spain

Olga Mena (IFIC (CSIC-UV)), Sergio Palomares-Ruiz (IFIC (CSIC-UV)), Juande Zornoza (IFIC (CSIC-UV))

Descripción

TeVPA is an international conference focused on the field of Particle Astrophysics, covering exciting and timely topics such as cosmic ray physics, gamma-ray astronomy, neutrino astronomy, cosmology, dark matter searches, gravitational waves, and connections to particle physics. Plenary and parallel sessions will be devoted to explore the current status and the future perspectives of these topics. This year the conference will take place in Valencia, Spain, where we will celebrate the 20th anniversary of the series, initiated in Fermilab in 2005.

The meeting will take place at the Bancaja Foundation, an emblematic building of the city of Valencia, and at the ADEIT Foundation, the University-Enterprise Foundation of the University of Valencia.

Please, note that registration on both sites, Indico and ADEIT, is required.

Fee payment and social program are managed from the ADEIT site. The fee includes conference materials, coffee breaks, lunches from Monday (Nov 3) thru Thursday (Nov 6), reception cocktail on Monday (Nov 3) and gala dinner on Thursday (Nov 6).

Note that onsite payment will not be available.

Important dates

JULY 31: Deadline for abstract submission (extended)

AUGUST 31: Abstracts selection

SEPTEMBER 21: Deadline for early registration fee (400€) (last extension)

OCTOBER 5: Deadline for late registration fee (450€)

Important notice: Beware of scam attempts

We have received reports of fraudulent requests related to travel, accommodation and fees. If you are contacted by third parties claiming to arrange these services on our behalf and requiring information from you, please be aware that these are scams.

Only trust communications from the official organizers or from email addresses ending in @ific.uv.es or @fundacions.uv.es. Be especially cautious with unsolicited emails that do not come from these sources.

Contact

tevpa2025@ific.uv.es

lunes, 3 noviembre
- 8:15 → 9:00
  
  Registration 45m Hall (Fundación Bancaja)
  
  Hall
  
  Fundación Bancaja
- 9:00 → 9:30
  
  Welcome
  
  Moderador: Juan José Hernández-Rey (IFIC (Univ. of Valencia and CSIC) ES)
- 9:30 → 10:30
  Plenary Session: I Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Juan José Hernández-Rey (IFIC (Univ. of Valencia and CSIC) ES)
  - 9:30
    
    Galactic sources 30m
    
    A new era in gamma-ray astronomy is upon us, thanks to a combination of instruments covering an unprecedented energy range from GeV to PeV. Space-based missions such as Fermi, ground-based Imaging Air Cherenkov Telescopes (IACTs), and extensive air shower arrays now provide a unified view of the most energetic sky. This multi-instrument approach has revealed over 300 sources, all of which are driven by extreme particle acceleration in violent cosmic environments. This contribution will provide a review of the Galactic gamma-ray sky, highlighting the characteristics of persistent, variable and transient sources as observed across this full energy spectrum.
    
    Ponente: Alicia López-Oramas (Instituto de Astrofísica de Canarias (IAC))
    
    Galactic_Sources_TeVPa_Lopez-Oramas.pdf
  - 10:00
    
    High Energy Neutrinos 30m
    
    More than a decade after the discovery of cosmic neutrinos by the IceCube observatory, the sources of cosmic neutrinos are still largely unknown. Yet, the first neutrino sources have been established over recent years. At the same time, new instruments like KM3NeT and GVD are growing in size and are starting to observe cosmic neutrinos. Sparked on by these successes, initiatives for even larger detectors are emerging. This talk will review the status of high energy neutrino astronomy and plans for the future, with emphasis on the domain of cubic-kilometer-scale water and ice Cherenkov detectors.
    
    Ponente: Aart Heijboer (nikhef)
    
    tevpa_heijboer2.pptx
- 10:30 → 11:00
  
  Coffee Break 30m Dome (Fundación Bancaja)
  
  Dome
  
  Fundación Bancaja
- 11:00 → 12:30
  Plenary Session: II Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Bryan Zaldivar (IFIC)
  - 11:00
    
    Stochastic Gravitational Wave Backgrounds 30m
    
    In this talk I will present the general characteristics of stochastic gravitational wave signals from the early universe and discuss some interesting sources, with a particular focus on first order phase transitions.
    
    Ponente: Chiara Caprini (CERN and University of Geneva)
    
    Caprini_TeVPA.pdf
  - 11:30
    
    Indirect dark matter searches 30m
    
    Indirect dark matter searches can probe a wide range of DM candidates, from ultra-light particles like axions, to heavy candidates like primordial black holes, by leveraging multi-messenger and multi-wavelength astrophysical and cosmological observations.
    In this talk, I will review the current status of these searches, and I will discuss how suitable strategies and future data will advance the quest for dark matter.
    
    Ponente: Marco Taoso (INFN Torino)
    
    MTaoso_TeVPa.pdf
  - 12:00
    
    Primordial Black Holes 30m
    
    While black holes are typically known as the remnants of stellar collapse, some may have formed in the early universe—these are known as primordial black holes (PBHs). Unlike most dark matter candidates, primordial black holes do not require the introduction of new fundamental physics, making them a compelling possibility. In this talk, I will outline the current observational constraints on PBHs as dark matter, explore their potential connections to gravitational wave signals, and discuss how Hawking evaporation of light primordial black holes could produce high-energy particles.
    
    Ponente: Christian Byrnes (University of Sussex)
    
    Byrnes-PBH-3Nov25.pdf
- 12:30 → 14:30
  
  Lunch break 2h ADEIT
  
  ADEIT
- 14:30 → 16:15
  Dark Matter: Direct Detection Room 3.1+3.2 (ADEIT )
  
  Room 3.1+3.2
  
  ADEIT
  
  Moderador: Madeleine Zurowski (University of Toronto)
  - 14:30
    
    Latest WIMPs and CEvNS result from XENONnT 15m
    
    XENONnT, located at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy, is a direct dark matter detection experiment designed to search primarily for Weakly Interacting Massive Particles (WIMPs) using a dual-phase xenon Time Projection Chamber (TPC). Thanks to its ultra-low background environment, the XENONnT detector is also sensitive to a variety of other rare-event physics channels. In this talk, I will present the latest results from the XENONnT experiment, including an overview of the current results from both WIMP and neutrino searches.
    
    Ponente: Federica Pompa (SUBATECH)
    
    TeVPA25_FPompa.pdf
  - 14:45
    
    PandaX-4T Experiment and its Recent Progress 15m
    
    PandaX-4T is a multi-tonne-scale dark matter direct searching experiment, utilizing 3.7 tonne liquid xenon as target material in sensitive volume. The experiment is located at China Jinping Underground Laboratory, with overburden of 2400 meter water equivalent. In 2021, the PandaX-4T experiment has released its first data and obtained various search result at the time. In this talk, I will introduce the recent results of PandaX-4T experiment with newly obtained data, including searches of the B8 solar neutrino CEvNS and light dark matter particles.
    
    Ponente: Qing Lin (University of Science and Technology of China)
    
    PandaX_Talk_v2.pptx
  - 15:00
    
    Latest results from the LUX-ZEPLIN Experiment 15m
    
    The LUX-ZEPLIN (LZ) experiment is primarily designed to search for interactions of dark matter in the form of weakly-interacting massive particles (WIMPs) using a 7 tonne dual-phase xenon time projection chamber. LZ is located at the Sanford Underground Research Facility in Lead, South Dakota, where it has been acquiring science data since 2021. Recently, with a combined exposure of 4.2 tonne-years from all science campaigns, LZ has placed the most stringent limits on spin-independent WIMP-nucleon cross section down to $2.2 \times 10^{-48}$ cm$^2$ for a 40 GeV/c$^2$ WIMP mass. This talk will discuss the current status of the LZ experiment and its latest endeavours in dark matter searches.
    
    Ponente: Paulo Brás (LIP Coimbra)
    
    Latest_results_from_the_LUX-ZEPLIN_Experiment_TeVPA2025.pdf
  - 15:15
    
    The PICO-40L Dark Matter Search 15m
    
    The PICO Collaboration uses bubble chamber technology for direct-detection searches of Weakly-Interacting Massive Particles (WIMP). Filled with superheated C$_3$F$_8$, the thermodynamic threshold of PICO detectors can be set such that the detectors are optimised for dark matter detection while being insensitive to gammas from electron recoils. The presence of fluorine atoms in the C$_3$F$_8$ gives PICO the potential to set world-leading exclusion limits for spin-dependent WIMP-proton interactions. PICO-40L is currently operating 2 km underground at SNOLAB in Sudbury, Ontario, Canada. It is the first large-scale implementation of the "right-side up" bubble chamber design, in which the absence of a buffer fluid in contact with the C$_3$F$_8$ minimises background rates from particulates entering the chamber. It acts as a proof-of-concept for the next generation PICO-500 detector, a 260-L bubble chamber with a projected ton-year exposure currently in the assembly phase at SNOLAB. This talk will present the status of the PICO-40L detector as well as an overview of preliminary analyses of PICO-40L data.
    
    Ponente: William Woodley (University of Alberta)
    
    TeVPA_2025_PICO.pdf
  - 15:30
    
    Status and prospects of the DEAP-3600 experiment 15m
    
    DEAP-3600 is an experiment performing direct dark matter searches since 2016. The detector is undergoing a third fill in order to achieve its goal sensitivity of 1e-46 cm2 for the WIMP-nucleon interaction cross section. This science case is achievable thanks to its location 2 km underground at SNOLAB, a thorough RnD to minimize its background and the background discrimination capabilities uniquely achievable with liquid Ar.
    
    Because of its uniqueness, DEAP is leading the search of some exotic candidates and is producing physically relevant results in the field of rare event searches. It is moreover playing a pivotal role in the framework of the Global Argon Dark Matter Collaboration. The expertise accumulated and the analyses performed are central for the success of the DarkSide-20k.
    
    In this talk I plan to address our last publications, the improvements introduced by the recently implemented hardware upgrades and our prospects for WIMP and neutrino searches.
    
    Ponente: Vicente Pesudo Fortes (CIEMAT / LSC)
    
    DEAP_TeVPA_2025_169.pdf DEAP_TeVPA_2025_43.pdf
  - 15:45
    
    The DarkSide-20k project updates and perspectives 15m
    
    The DarkSide-20k experiment is a next-generation multi-ton dark matter detector currently being built at the INFN Gran Sasso National Laboratory (LNGS) and designed for zero instrumental background direct detection of Weakly Interacting Massive Particle Dark Matter. The DarkSide-20k detector is a dual-phase time projection chamber (TPC) deploying 50 tonnes of underground low-radioactivity argon target instrumented with silicon photomultiplier (SiPM) arrays for precise light detection in both the TPC and in the two surrounding active veto systems.
    This general presentation on the DarkSide-20k project will provide an overview on the key design features and challenges that will be detailed in other talks at this conference, the main updates on the construction effort, and the expected world-class sensitivity in the search for both high and low-mass WIMP dark matter.
    
    Ponente: Sandro De Cecco (Sapienza Università di Roma)
    
    The DarkSide-20k project - TeVPA - Sandro De Cecco.pdf
  - 16:00
    
    The Underground Argon program of the Global Argon Dark Matter Collaboration 15m
    
    The DarkSide-20k experiment, currently under construction at the Laboratori Nazionali del Gran Sasso (LNGS), has been designed to lead the search for heavy WIMPs. While liquid argon offers powerful pulse-shape discrimination, its intrinsic cosmogenic Ar-39 activity (0.96 Bq/kg) poses is a show-stopper for multi-tonne dual-phase Time Projection Chambers. To address this, and following the successful experience of DarkSide-50, the Global Argon Dark Matter Collaboration (GADMC) has launched a program to procure and process underground argon (UAr) depleted in Ar-39 by a factor of at least 1400.
    
    Three key facilities are involved in this effort: extraction at the Urania plant in Colorado (USA), isotopic purification in the ARIA distillation column in Sardinia (Italy), and the characterization in the DArT-in-ArDM setup at the Canfranc Underground Laboratory (Spain). In this talk, we will present the status and prospects of these infrastructures, with a particular focus on DArT and its initial commissioning runs.
    
    Ponente: Daniel Díaz Mairena (CIEMAT)
    
    Underground_Ar_TeVPA.pdf Underground_Ar_TeVPA.ppt
- 14:30 → 16:15
  Gamma Rays: Experiments Salón de Actos (ADEIT)
  
  Salón de Actos
  
  ADEIT
  
  Moderador: Julian Sitarek (University of Lodz)
  - 14:30
    
    The GRAMS Project: Gamma Rays and Antimatter from Astrophysical and Dark Matter Sources 15m
    
    The Gamma-Ray and Antimatter Survey (GRAMS) project is a next-generation MeV-scale gamma-ray and antimatter experiment. The detector consists of a liquid argon time projection chamber (LArTPC), the largest of its kind in an astrophysics experiment. Surrounding the LArTPC are plastic scintillator bars for charged particle time-of-flight (TOF) measurement. The LArTPC is the main detector and will serve as both a Compton telescope and 3D charged particle tracker, while the TOF will help identify heavy charged particles and nuclei. The detector design facilitates the study of a wide variety of physics, from sources both known and beyond the Standard Model.
    
    One of the largest open questions in physics is the nature of dark matter, which gravitational observations suggest comprises nearly 27% of the mass-energy in the universe. Many dark matter models have been proposed, and GRAMS is positioned to empirically test a variety of them, in addition to studying astrophysical sources. For example, predictions from dark matter models such as antimatter from dark matter annihilation and gamma-rays from sterile neutrino radiative decays. Additionally, the GRAMS Compton telescope functionality will study gamma-rays, including those from the diffuse background, cosmic-ray accelerators, and nuclear transitions. The presentation will discuss the detector design, physics sensitivities, and experiment timeline.
    
    Ponente: Jonathon Sensenig (Columbia University)
    
    jsensenig_grams_tevpa_2025_v3.pdf
  - 14:45
    
    Crystal Eye: an instrument with a wide view of the MeV sky to study the astrophysical photons 15m
    
    Crystal Eye is a new concept of space-based all sky monitor for the observation of 10 keV $-$ 30 MeV photons exploiting novel detection techniques. It foresees enhanced localization capability and detection power of the astrophysical short-duration outburst phenomena in an unprecedented energy range with respect to other concurrent instruments. The instrument uses the advantage of new detector materials (scintillator crystals) and high-efficiency sensors (like silicon photo multipliers). The primary scientific goal is the detection of the electromagnetic signal from extreme phenomena in the Universe. In order to enhance the understanding about these phenomena through simultaneous multi-messenger study, the satellite will be able to provide real-time alerts with precise location information to both space and ground based experiments. The full scale design of the detector has been optimized and the engineering qualification model is going to be realized at this stage. Furthermore, a scaled down prototype made of three full size pixels is being realized to fly aboard the Space Rider (ESA) in a low-Earth orbit for a tentative life time of two months in 2027, with the aim to characterize the background at the orbit and verify the technology for space use. We present here the instrumental setup and its performances estimated using Monte Carlo simulation of the full detector configuration in a speculative working environment along with prototype tests.
    
    Ponente: Ritabrata Sarkar (Gran Sasso Science Institute)
    
    TeVPA25-CE-Sarkar.pdf
  - 15:00
    
    WINK, a pathfinder for a future all-sky X and gamma-ray space-based detector 15m
    
    Monitoring the sky in the MeV energy range is crucial for understanding the nature of explosive events in the Universe. Since the Universe is transparent to MeV gamma rays, we can observe the most distant transient phenomena, such as gamma-ray bursts (GRBs). In 2017, there was the first joint observation of gravitational waves (GW) events from binary neutron stars and a GRB that initiated a new multi-messenger era. In the coming decade, a rapidly growing of multi-messenger astronomy with GW is expected and corresponding improvements in electromagnetic observation capabilities are required. Crystal Eye (CE), an innovative all-sky monitor, has been designed to detect photons of energies ranging from 10 keV to 30 MeV with accurate localization across the entire sky. Its autonomous, real-time monitoring ability makes it uniquely suited for studying transient events and multi-messenger astrophysics in the MeV energy range. CE has an hemispherical shape and consists of 112 pixels of scintillating crystals. The CE pathfinder, WINK, composed of 3 CE pixels, will fly aboard Space Rider in 2027 with the goal of characterize the cosmic background and validating CE's innovative technologies. In this contribution, the results of the initial tests on the WINK qualification model, the future plans, and the mission's expectations will be presented.
    
    Ponente: Roberta Colalillo (University of Naples, Federico II)
    
    TeVPA2025_colalillo.pdf
  - 15:15
    
    Detecting Gamma-Ray Counterparts of High-Energy Neutrino Sources with CTAO: Prospects and Simulations 15m
    
    The identification of gamma rays in coincidence with high-energy neutrinos plays a fundamental role in multi-messenger astronomy, as such observations are essential for constraining source localization, determining source classes, and investigating emission mechanisms. The present study evaluates the prospects of Cherenkov Telescope Array Observatory (CTAO) for detecting very-high-energy (VHE) gamma-ray counterparts of neutrino-emitting extragalactic sources.
    The performance of CTAO is assessed under the “Alpha” configuration based on simulations of neutrino and gamma-ray emissions from both steady sources and flaring blazars. Detection probabilities for IceCube neutrino events are calculated for both the Northern and Southern CTAO sites, assuming 30-minute follow-up observations. The detectability of blazars is further analyzed for extended observation windows of 1 to 5 hours.
    Additionally, preliminary results are presented for a parallel analysis based on the KM3NeT ARCA neutrino telescope. Due to its improved sensitivity to Southern Hemisphere sources, ARCA offers complementary capabilities that enhance the multi-messenger potential of CTAO when combined with next-generation neutrino observatories.
    
    Ponente: Gloria Maria Cicciari (University of Palermo - INFN Catania)
    
    TEVPA_2025_Cicciari.pdf
  - 15:30
    
    Implementation and Optimization Studies of the Divergent Pointing Mode for CTAO 15m
    
    The Cherenkov Telescope Array Observatory (CTAO) will be the next-generation ground-based gamma-ray observatory, with two arrays in both hemispheres offering full-sky coverage and improved sensitivity over a broad energy range, from 20 GeV to 300 TeV. The standard pointing mode, where all telescopes are aligned to observe the same sky region, provides excellent performance in terms of sensitivity and reconstruction accuracy. These high-level capabilities make CTAO particularly effective for targeted observations and short-exposure surveys, enabling high-quality sky mapping with high angular resolution and accurate background separation.
    
    As a complementary approach, a divergent pointing strategy has been proposed, where telescopes are slightly offset from a central direction to increase the array’s instantaneous field of view. This mode is particularly promising for wide-area surveys, such as the extra-galactic survey, and for the follow-up of loosely localized transient events (e.g., gravitational wave or neutrino alerts). The increased sky coverage, however, results in a reduction of angular and energy resolution, requiring dedicated performance optimization strategy. In this contribution, we present simulation-based studies aimed at implementing and optimizing divergent pointing configurations. We focus on evaluating the array performance across the extended field of view, in view of their application to CTAO science use cases.
    
    Ponente: Daniele Ambrosino (Università degli Studi di Napoli Federico II)
    
    Ambrosino_Divergent_TeVPA.pdf
  - 15:45
    
    Development of a multiPMT detector for the SWGO experiment: Simulation and performance study on muon tagging with machine learning techniques 15m
    
    Imaging Air Cherenkov Telescopes and Ground Based Arrays are the major contributors to Gamma
    Ray astronomy at ground level. The Southern Wide-Field Gamma-ray Observatory (SWGO) will be a
    water Cherenkov Array located in the Atacama Desert in Chile that will monitor the VHE and UHE sky.
    The Naples group has proposed a multi-photomultiplier (multiPMT) detector for SWGO, based on
    KM3NeT and HyperKamiokande designs, consisting of seven 3-inch outward-facing PMTs. A multiPMT
    photosensor offers intrinsic sensitivity to the directionality of incoming particles Cherenkov light cone,
    large dynamical range and increased time resolution. My work demonstrates the advantages of the
    multiPMT over the single-PMT alternative. I developed a detailed simulation of the multiPMT and
    studied ways to improve Cherenkov light collection and upgrade the original design of the prototype. I
    also investigated the muon tagging capabilities of multiPMTs in water Cherenkov tanks using various
    machine learning models and explored the potential of using the multiPMT's directional sensitivity for
    neutrino detection in the context of Multimessenger Astronomy.
    
    Ponente: Vincenzo Maria Grieco (Scuola Superiore Meridionale)
    
    grieco_mpmt_tevpa.pdf
  - 16:00
    
    Probing Extreme PeVatron Sources (PEPS) 15m
    
    The project Probing Extreme PeVatron Sources (PEPS) aims at measuring the most energetic gamma rays from our Galaxy in the energy range between 10¹⁵eV and 5x10¹⁶ eV, opening a new energy window for multimessenger astroparticle physics. PEPS will consist of an array of 10 km² placed in the southern hemisphere, at the location of the Pierre Auger Observatory. It will be built in two phases, with the first phase covering a surface of 2 km². The location offers an excellent view of the Galactic Plane and the Galactic Center while taking advantage of the existing infrastructure of the Pierre Auger Observatory. The design is based on an array of water-Cherenkov particle detectors with a horizontal segmentation of the optical volume into two. We present the performances of two prototype detectors that are functioning in the field. The science case for PEPS will be presented.
    
    Ponente: Ioana Maris (Université Libre de Bruxelles)
    
    peps_tevpa.pdf
- 14:30 → 16:15
  Gamma Rays: Galactic Salón de Grados (ADEIT)
  
  Salón de Grados
  
  ADEIT
  
  Moderador: Giulia Brunelli (University and INAF-OAS Bologna)
  - 14:30
    
    A new view of the high-energy gamma-ray structure of the W51 complex with Fermi: identification of two extended components associated with W51B and W51C 15m
    
    W51 is one of the most massive and active star-forming complexes in the Milky Way. Multiple experiments, including Fermi-LAT, MAGIC, HESS, HAWC, and most recently LHAASO, have detected gamma-ray emission associated with this region. The complex hosts two major star-forming regions, W51A and W51B, and the middle-aged supernova remnant (SNR) W51C. The latter has been associated with the high-energy (HE) gamma-ray source 4FGL J1923.2+1408e. The characteristic pion-decay spectral feature shown by Fermi-LAT data suggests that protons accelerated by the SNR shock are interacting with dense molecular material. The detection by LHAASO of a spectral cutoff near 400 TeV indicates the presence of cosmic-ray accelerations reaching PeV energies. However, due to its limited angular resolution, LHAASO did not manage to unambiguously resolve the emission’s morphology, leaving open the possibility that young stellar clusters (YSC) within W51B (notably G48.9-0.3 and G49.2-0.3) might also contribute to the ultra-high-energy (UHE) gamma-ray signal.
    In this work, we present an analysis of 16 years of Fermi-LAT data targeting the W51 region. Through a binned likelihood analysis, we refined the spatial and spectral modelling of the gamma-ray emission, using asymmetric spatial distributions between 10 GeV and 1 TeV. We tested multiple spatial configurations, including templates based on radio observations, to explore correlations between the gamma-ray emission and molecular cloud distributions near W51C and W51B. Our results reveal two extended, elliptical sources aligned with the respective radio structures. We managed to disentangle the high-energy gamma-ray emission between 1 GeV and 1 TeV into two components: a softer LogParabola spectrum associated with W51C and a harder Power Law component associated with W51B.
    Our multi-wavelength modelling confirms the hadronic origin of the emission. The W51C component revealed the presence of hadronic acceleration characterised by a few per cent cosmic-ray (CR) acceleration efficiency and an energy cutoff at the TeV level. However, since the estimated shock size is smaller than the identified gamma-ray region, we modelled the HE emission also assuming a CR escape scenario. Regarding the gamma-ray emission associated with W51B, we identified 3 spatially coincident stellar clusters with the necessary properties required to explain the UHE emission detected by LHAASO: G48.9-0.3, G49.2-0.3 and G49.0-0.3. We jointly fitted the Fermi-LAT and LHAASO data and identified the acceleration and diffusion properties of the three clusters.
    
    Ponente: Giorgio Pirola (Max-Planck-Institut für Physik)
    
    TeVpa_2025_gpirola_W51.pdf
  - 14:45
    
    Very High Energy gamma-ray observations of the PeVatron candidate 1LHAASO J0056+6346u with the first CTAO Large-Sized Telescope 15m
    
    The first LHAASO catalogue, published in 2023, reported the detection of 90 sources above 1 TeV, with angular extensions up to 2 deg. Among the unknown sources detected above 100 TeV by KM2A, 1LHAASO J0056+6346u appears as one of the most promising PeVatron candidates.
    More recently, the LHAASO collaboration performed a dedicated study on the source, confirming the detection of the source down to 8 TeV, with a >10σ significance above 100 TeV, and a mild extension of ∼0.2-0.3 deg. The performed modelling suggests that the gamma-ray emission is likely to be generated by a TeV Pulsar Wind Nebula (PWN), powered by an unknown pulsar. However, the hadronic scenario associated with nearby CR accelerators, such as the SNR candidate G124.0+1.4, could not be excluded.
    Between 2024 and 2025, the first Large-Sized Telescope (LST-1) of the Cherenkov Telescope Array Observatory (CTAO) started a follow-up observation campaign, collecting data on 1LHAASO J0056+6346u. We performed a 3D likelihood analysis by using and comparing different tools for the background estimation and identified hints of signal over a region overlapping with the WCDA and KM2A reported extended emissions. We analysed 16 years of Fermi-LAT data, but no significant signal was detected in the LHAASO emission regions. In this contribution, we will present the first results of the LST-1 data analysis and the comparison with the Fermi-LAT and LHAASO results.
    
    Ponente: Alessandra Briscioli (CPPM)
    
    TeVPA_2025_1LHAASOJ0056+6346u.pdf
  - 15:00
    
    Search for the GeV Counterpart of PeVatron LHAASO J1912+1014u using Fermi-LAT and FUGIN CO Data 15m
    
    LHAASO reported 43 ultra-high-energy sources that are either proton or electron PeVatrons (Cao+24), and multi-wavelength data are crucial for determining particle species and the CR energy density of the source. In this project, we study the LHAASO J1912+1014u (and HESS J1912+101) region using Fermi-LAT and FUGIN CO data to investigate the “proton PeVatron” scenario. We analyzed 15 years of Fermi-LAT data in 400 MeV to 400 GeV. We improved the standard Fermi-LAT diffuse model by adding a template to reduce large residuals around the source in 1-10 GeV. We found a significant signal in excess of the diffuse model that may represent the >10 GeV emission of the LHAASO/H.E.S.S. source. We also found that 12CO maps with velocities of about 60 km/s (Su+17) and 25 km/s (Sano+18, Sano+ in preparation) represent the excess emission better than a simple Gaussian model, indicating that proton acceleration is a feasible scenario. In this contribution, we present the details of the analysis and its implications for the object.
    
    Ponente: Tsunefumi Mizuno (Hiroshima University)
    
    LHAASOJ1912-Fermi_2025-11_v0.9.pdf LHAASOJ1912-Fermi_2025-11_v0.9.pptx
  - 15:15
    
    Deep H.E.S.S. Observations of the SNR W44 and Its Surroundings 15m
    
    The supernova remnant (SNR) W44, one of the first sources firmly established as a hadronic accelerator in the GeV regime, has been observed for over 200 hours with the H.E.S.S. telescope array. We present the results of a deep analysis of this dataset, revealing new insights into the gamma-ray emission from W44 and its interaction with the surrounding interstellar medium. In particular, we discuss the implications of W44's contribution to the local cosmic-ray population and its role in shaping the observed gamma-ray morphology. These results will be put in the context of theories of particle acceleration and escape processes in middle-aged SNRs.
    
    Ponente: Wenjuan Zhong (Deutsches Elektronen-Synchrotron DESY)
    
    W44_TeVPA_v3.pdf
  - 15:30
    
    Young supernova remnants interacting with dense CSM shells 15m
    
    Supernova remnants are discussed as the main sources for Galactic cosmic-rays. However, observational and theoretical developments in the last decade have lead to the idea that only supernova explosions in very dense circumstellar media are able to accelerate particles to the relevant energies and only in the first decades after the explosion.
    The medium around massive stars tends to be highly structured on account of the non-steady mass-loss history of the progenitor stars and the interaction of the stellar winds with the medium around them. We used RATPaC to simulate the propagation of and particle acceleration at supernova remnants shocks in the medium around Red Supergiants and Luminous Blue Variable stars, that can feature very dense circumstellar shells. We find that the shock-shell interactions can boost the achievable particle energy beyond a few PeV. Based on our simulations, we discuss the multi-wavelength signatures that can be expected from radio to gamma-ray energies and propose a revised observation strategy for current and future gamma-ray observatories to catch such events.
    
    Ponente: Robert Brose (Universität Potsdam)
    
    Brose_ISN.pptx
  - 15:45
    
    Probing the PeVatron Candidate VER J2019+368 in the Cygnus Region with the SST-1M Stereoscopic System 15m
    
    The Cygnus region is one of the richest and most complex areas on the Galactic plane, known for its intense star formation and the presence of numerous very-high-energy gamma-ray sources. Among these sources, VER J2019+368 ranks as one of the brightest, exhibiting a hard spectrum and complex morphology that suggests the presence of powerful particle accelerators. First discovered by MILAGRO and later resolved by VERITAS, its origin remains unclear. The recent detection of photons above 25 TeV by LHAASO has renewed interest in VER J2019+368 as a potential PeVatron. Since April 2024, the Single-Mirror Small-Size Telescopes (SST-1M), installed in Ondřejov, Czech Republic, have been conducting a stereoscopic observing campaign focused on the Cygnus region, with particular attention to VER J2019+368. The SST-1M telescopes are designed to cover an energy range from a few TeV to several hundred TeV, featuring a wide 9° field of view and a compact Davies-Cotton optical design optimized for good off-axis performance, making them well suited for the study of hard, extended sources. In this contribution, we present preliminary results from our campaign, including morphological and spectroscopic analyses of VER J2019+368, and discuss possible scenarios for the origin and nature of its emission.
    
    Ponente: Ana Laura Müller (FZU - Institute of Physics of the Czech Academy of Science)
    
    TeVPA-Mueller-SST1M.pdf
  - 16:00
    
    Supernova explosion within an extragalactic jet and the theoretical radiative output of such an event 15m
    
    Relativistic jets interact with multiple obstacles as they cross their host galaxies, before interacting with the interstellar or intergalactic medium at hotspots, in powerful sources, or plumes, in low power ones. We assume the possibility that a supernova explosion happens within the jet, and this may have a strong impact not only on the jet dynamics during the evolution of the supernova remnant, but also in terms of radiative output via acceleration at the shock region. We expect the particles acceleration to be enough to reach detectable emissions up to gamma rays.
    In this contribution, we present relativistic hydrodynamics simulations of a supernova explosion within an extragalactic jet, with a focus on the dynamics of the interaction and the theoretical radiative output of such events.
    
    Ponente: Bruno Longo (Universitat de València)
    
    tevpa2025_longo.pdf
- 14:30 → 16:15
  Gravitational Waves Room 2.1+2.2 (ADEIT)
  
  Room 2.1+2.2
  
  ADEIT
  
  Moderador: Mauro Pieroni
  - 14:30
    
    GWTC-4.0: constraints on the cosmic expansion rate and modified gravitational-wave propagation 15m
    
    We analyze data from 142 gravitational wave (GW) sources in the fourth LVK Gravitational-Wave Transient Catalog (GWTC-4.0) to estimate the Hubble constant $H_0$ jointly with the population properties of merging compact binaries. We measure the luminosity distance and redshifted masses of GW sources, and combine this with redshift information obtained by leveraging features in the binary mass spectrum and merger rate evolution, as well as by identifying potential host galaxies in the GW localization volume. Probing the relationship between luminosity distance and redshift in this way yields constraints on cosmological parameters. We also constrain parameterized deviations from general relativity which affect GW propagation, and hence the dependence of GW signals on the luminosity distance to their sources. Assuming a model for the source-frame mass distribution which is able to describe the full spectrum of coalescing compact objects and using GW candidates detected up to the end of the O4a, together with redshift data from the GLADE+ all-sky galaxy catalog and the inclusion of GW170817 with its electromagnetic counterpart, we provide the latest and most precise measurements of $H_{0}$ and the GW propagation parameter $\Xi_{0}$ to date using GW data.
    
    Ponente: Grégoire Pierra (Sezione di Roma, INFN, La Sapienza)
    
    TeVPA_2025.pdf
  - 14:45
    
    Gravitational-wave background searches in LVK: updates from the fourth observing run 15m
    
    In 10 years since the first direct observation of a gravitational wave (GW), GW astronomy has made giant leaps, going from detecting loud binary black hole (BBH) coalescences, to binary neutron star (BNS) and black hole -- neutron star (BHNS) binary events, all the way to large-volume population analyses. Yet the vast majority of events are too faint to be directly detected with coherent matched filter searches, and moreover there are a slew of potential GW sources that have yet to be identified. The collection of all GWs that may not be directly resolved by our detectors build up incoherently, giving rise to a cumulative gravitational-wave background (GWB) signal. Given its incoherent and indeterminate nature, the GWB is described as a mean-0 stochastic field. Distinct GW sources imprint different signatures in the background spectrum, hence stochastic analyses are tailored to search for specific hallmarks such as frequency dependence or directional dependence to perform component separation and give optimal results.
    In this talk, we describe the sources and signals contributing to the GWB, contextualising them within the fields of astrophysics, cosmology, and high energy physics. We then introduce the stochastic GW analysis methods routinely employed in the Laser Interferometer Gravitational-wave Observatory (LIGO), Virgo, and Kagra (LVK) collaboration searches for GWBs, and present recent search results using data from the first four observing runs, up to the first portion of observing run O4. These include upper limits on a number of different target signals including compact binary backgrounds, potential GWs from nearby radio sources, first-order phase transitions and cosmic string networks in the early Universe, and primordial black holes. We conclude by providing an outlook of the potential detections to come with future upgrades to the detector network.
    
    Ponente: Jishnu Suresh (Observatoire de la Côte d'Azur)
    
    SureshJishnu_TeVPA_VLC.pdf
  - 15:00
    
    LVK Searches for Subsolar-Mass Compact Objects: Methods and Constraints 15m
    
    The nature and formation mechanisms of subsolar-mass (SSM) black hole binaries remain an open question in astrophysics, as such objects fall outside the predictions of standard stellar evolution. The LIGO-Virgo-KAGRA (LVK) collaboration has conducted searches for compact binary mergers involving at least one subsolar-mass component, using data from recent observing runs. This search targets black holes with at least one component mass below the mass of the sun, probing for potential signatures of primordial black holes or exotic compact objects predicted in alternative gravitational theories. We employ matched-filtering techniques using waveform templates designed for the low-mass regime. For the first time, we also constrain the formation rate of sub-solar mass objects with tidal deformability. The results of our study set upper limits on the merger rate of binaries including a SSM object and improve constraints on their astrophysical and cosmological implications. Our findings contribute to the ongoing efforts to probe the origin of SSM black holes and their potential role in explaining dark matter. This presentation will provide an overview of the search methodology, key results, and their implications in gravitational wave astronomy.
    
    Ponente: Ines Bentara (Institut de Physique des Deux Infinis)
  - 15:15
    
    Exploring dense matter physics with gravitational waves 15m
    
    Highly dense and isospin asymmetric matter is partly out of the reach of nuclear laboratories on Earth. Our theoretical understanding of strong and nuclear forces at high density and relatively low temperatures is also limited such that the equation of state and properties of dense matter remain a mystery. However, this particular type of matter comprises the deepest shells of the highly compact astrophysical objects that are neutron stars. An entire field of nuclear astrophysics is devoted to exploring dense matter physics with multi-messenger observations of neutron stars throughout their lifetime. A boost to this field recently occurred with the construction of several gravitational wave detectors that can observe the ripples of space time originating from the coalescence of compact objects.
    In this talk, we discuss the advances made on the subject of dense matter physics thanks to the detection of the gravitational waves emitted by neutron star mergers. FIrst, I will present the key sources gathered in the recent catalog GWTC-3 of the LIGO-Virgo-KAGRA collaboration, and discuss in details the link between dense matter and neutron star deformation of neutron stars, and its imprint on the gravitational waveform. Particular attention is paid to the most informative source to date, GW170817, and how it has constrained the equation of state of dense matter. I will quickly expand on the ability of binary coalescences to help us understand heavy-element nucleosynthesis, using the example of the mass-gap event that occurred during the fourth observing run of the LIGO-Virgo-KAGRA collaboration. Finally, I will discuss what to expect from future observations and the next generation of ground based gravitational wave detectors (Cosmic Explorer and Einstein Telescope) and some of the challenges we shall face in an era of high precision gravitational waves detections.
    
    Ponente: Lami Suleiman (Deutsches Elektronen Synchrotron)
    
    TeVPA.pdf
  - 15:30
    
    Gravitational waves from supermassive black holes at pulsar timing arrays 15m
    
    Inspiralling supermassive black hole (SMBH) binaries provide a natural explanation for the gravitational wave (GW) background observed in pulsar timing array (PTA) data. In this talk, I present a semi-analytical estimate of the GW background from SMBH binaries and discuss how the SMBH-based fit to the PTA data reveals evidence of environmental effects or binary eccentricities. I also explore potential observational signatures that could help distinguish between these effects and confirm whether the signal indeed originates from SMBH binaries.
    
    Ponente: Ville Vaskonen
    
    SMBH_Valencia.pdf
  - 15:45
    
    Extracting new physics from extreme mass ratio inspirals in LISA data 15m
    
    Extreme mass ratio inspirals are a key target for next generation space-based gravitational wave detectors because they have a rich phenomenology that could offer new astrophysics and fundamental physics insights. However, their dynamics are complicated to model, and they will be buried amongst a large population of other sources in the milliHertz frequency band. Searching for these systems and measuring their parameters therefore presents a difficult challenge, even in vacuum.
    
    Simulation-based inference methods could offer solutions to some of these challenges. I will show parameter estimation results for extreme mass ratio inspiral systems achieved with sequential simulation-based inference, specifically truncated marginal neural ratio estimation. I will highlight the benefits of this approach with respect to traditional likelihood-based methods, and discuss the broader context in which such a pipeline will need to be embedded as well as how and when environmental effects should be considered.
    
    Ponente: Philippa Cole
    
    SBI_EMRIs_TeVPA.pdf
  - 16:00
    
    Complete Gravitational-Wave Spectrum of the Sun 15m
    
    The solar plasma is a natural source of gravitational waves at high frequencies, a spectral range that is attracting increasing interest due to its potential to reveal new physical phenomena. Motivated by this, in this talk, I will present the first comprenhensive calculation of the gravitational-wave power spectrum emitted by the Sun. This includes both microscopic processes—such as bremsstrahlung and photoproduction—and macroscopic contributions from hydrodynamic fluctuations, each computed using methods adapted from axion physics.
    
    Based on arXiv:2407.18297 (accepted for publication in PRL)
    
    Ponente: Camilo Garcia Cely (IFIC, CSIC-UV)
    
    TeVPA.pdf
- 14:30 → 16:15
  Neutrinos: The first ultra-high-energy neutrino & Neutrino production Room 1.1+1.2 (ADEIT)
  
  Room 1.1+1.2
  
  ADEIT
  
  Moderador: Mauricio Bustamante (Niels Bohr Institute, University of Copenhagen)
  - 14:30
    
    Scrutinising the cosmogenic origin of KM3-230213A with the cosmic-ray proton fraction and gamma-ray constraints 15m
    
    The recent detection of a multi-PeV neutrino event by KM3NeT/ARCA opens a new window into the origin of high-energy neutrinos and ultra-high-energy cosmic rays. We revise the possibility of a cosmogenic origin of this neutrino by analysing the constraints induced by cascaded photons onto the isotropic gamma-ray background measured by the Fermi-LAT collaboration.
    We consider two scenarios: the first one, at low energies, with a primary proton population saturating the proton content inferred in the data of the Pierre Auger Observatory. The second one consists of a sub-population of protons contaminating the UHECR flux at the highest energies. Remarkably, the cascaded photons constrain the low-energy scenario which cannot explain the KM3-230213A event, if the cosmological evolution of the sources is too strong, because the corresponding gamma-ray spectrum would overshoot the measurements. By contrast, the high-energy scenario is allowed by current cosmic-rays, neutrinos and gamma-rays data and only future measurements of the UHECR composition will further constrain this scenario.
    
    Ponente: Denise Boncioli (University of L'Aquila and INFN-LNGS)
    
    Boncioli_TeVPA_NeutrinoSession_2025.pdf
  - 14:45
    
    A strike of luck: the KM3Net neutrino produced by evaporating burdened PBHs 15m
    
    Primordial black holes (PBHs) may constitute part of all the Dark Matter, and as they evaporate they should emit an all particle spectrum, including neutrinos. The recently suggested theoretical framework of "memory burden" would allow the survival until today of PBHs with masses low enough to evaporate into particles of energy at the PeV and above.
    In this talk we explore the scenario in which the ultra-high-energy neutrino event recently detected by KM3NeT could have originated from an evaporating PBH. Using the IceCube data, we place constraints on the combined parameter space of PBH masses and memory burden effects, by systematically scanning the parameter space of burdened PBHs.
    We predict the occurrence rate of events similar to the KM3Net ones under current constraints on PBH dark matter fraction.
    Future neutrino telescopes such as IceCube-Gen2 and GRAND will provide crucial tests of these scenarios, with the potential to probe
    highly suppressed evaporation regimes and light PBH masses.
    
    Ponente: Andrea Boccia (Scuola Superiore Meridionale)
    
    A.Boccia_TeVPA25.pdf
  - 15:00
    
    Investigation of a Muon Burst Coincident with KM3-230213A 15m
    
    On February 13 2023, at 01:16:46 UTC, the KM3NeT/ARCA neutrino telescope detected the $\sim 220$ PeV neutrino candidate KM3-230213A. Remarkably, the Yangbajing muon telescope in Tibet recorded a simultaneous burst of muons, showing a 5.7σ excess from a compatible direction. The burst exhibits a statistically significant exponential time profile, with a decay constant of τ = 7.0 ± 1.5 minutes, a peak flux of 55 ± 10 Hz/m², and a total of 2300 ± 400 excess events detected over 30 minutes.
    Assuming a common source characterized by a spectrum $\propto E^{-3.2}$, typical of $\sim 200$ PeV cosmic rays, the observed low-energy muon excess appears consistent with the single high-energy neutrino event. These findings suggest the possible presence of a transient astrophysical source and highlight the importance of correlating data from surface muon detectors with neutrino telescopes to strengthen the discovery potential in high-energy astrophysics
    
    Ponente: Francesco Nozzoli (Istituto Nazionale Fisica Nucleare (INFN) - TIFPA)
    
    NOZZOLI_YBJ_TeVPA.pdf
  - 15:15
    
    Ultra-high-energy neutrino searches at the Pierre Auger Observatory 15m
    
    The detection of Ultra-High-Energy (UHE) neutrinos is key for the understanding of cosmic-ray acceleration mechanisms and the identification of their astrophysical sources. The Surface Detector of the Pierre Auger Observatory, comprising 1660 water-Cherenkov particle detectors deployed over an area of 3000 km$^2$, has operated continuously for over two decades, providing some of the most stringent limits on UHE neutrino fluxes above 100 PeV. Neutrino identification is possible through the showers they induce, which are generally more penetrating in the atmosphere than cosmic-ray-induced showers and still retain an electromagnetic component when reaching the detector, even for large zenith angles. Exploiting these features, searches for both diffuse and point source fluxes have been performed. In this contribution, we will discuss the results from these searches and their implications for possible astrophysical sources.
    
    Ponente: Juan Ammerman-Yebra (Radboud University)
    
    UHE_neutrino_tevpa_v2.pdf
  - 15:30
    
    Numerical Studies of High-Energy Neutrino Emission from a Radiatively Inefficient Accretion Flow with a 3D GRMHD Simulation 15m
    
    High-energy neutrino emission from black hole accretion flows is a promising probe of extreme plasma environments and cosmic-ray acceleration in active galactic nuclei (AGNs). While many previous studies have relied on simplified single-zone models, the influence of large-scale plasma inhomogeneity and turbulence remains poorly understood. In this study, we perform the first global simulations of cosmic-ray acceleration and high-energy neutrino production via hadronuclear (pp) interactions in radiatively inefficient accretion flows (RIAFs) and outflows surrounding a supermassive black hole (Kawashima & Asano 2025, ApJ in press). Our calculations are based on three-dimensional general relativistic magnetohydrodynamic (GRMHD) simulation data. To describe turbulent acceleration, we solve the Fokker-Planck equation for cosmic-ray protons using a sub-grid energy diffusion model. The resulting particle energy distributions reflect the highly complex, time-dependent nature of the flow. Compared to the single-zone approximation, the resulting neutrino spectra are flatter and predominantly originate from cosmic rays transported with outflows rather than inflows. These findings suggest that low-luminosity AGNs and quiescent galactic nuclei can act as efficient sources of cosmic rays and may significantly contribute to the observed high-energy neutrino background.
    
    Ponente: Tomohisa Kawashima (National Institute of Technology, Ichinoseki College)
    
    Kawashima_TeVPA2025.pptx Kawashima_TeVPA2025_ver2.pdf
  - 15:45
    
    Exploring ultra-high energy neutrino experiments through the lens of the transport equation 15m
    
    We develop a first-principles formalism, based on the transport equation in the line-of-sight approximation, to link the expected number of muons at neutrino telescopes to the flux of neutrinos at the Earth's surface. We compute the distribution of muons inside Earth, arising from the up-scattering of neutrinos close to the detector, as well as from the decay of taus produced farther away. This framework allows one to account for systematic uncertainties, as well as to clarify the assumptions behind definitions commonly used in the literature, such as the effective area. We apply this formalism to analyze the high-energy muon event recorded by KM3NeT, with a reconstructed energy of $\left(120^{+110}_{-60}\right)\,\rm{PeV}$ and an elevation angle of $\left(0.54 \pm 2.4\right)^\circ$, in comparison with the non-observation of similar events by IceCube. We find a $3.1\sigma$ tension between the two experiments, assuming a diffuse neutrino source with a power-law energy dependence. Combining both datasets leads to a preference for a very low number of expected events at KM3NeT, in stark contrast to the observed data. The tension increases both in the case of a diffuse source peaking at the KM3NeT energy and of a steady point source, whereas a transient source may reduce the tension down to $1.6\sigma$. The formalism allows one to treat potential beyond-the-Standard-Model sources of muons, and we speculate on this possibility to explain the tension.
    
    Ponente: Stefano Palmisano (Galileo Galilei Institute for Theoretical Physics)
    
    presentazione.pdf
  - 16:00
    
    Predicting the outcome of neutrino flavor instabilities 15m
    
    Accurately modeling neutrino flavor oscillations in global simulations of core-collapse supernovae or neutron star mergers remains a major challenge, albeit a potentially crucial one for making reliable predictions. Indeed, it is now widely recognized that flavor instabilities—in which classically computed neutrino distributions are dramatically altered when including quantum effects—are expected to occur commonly in such environments. A promising strategy is the development of subgrid models of neutrino flavor transformation. In this approach, insights from detailed studies of local quantum neutrino transport are used to formulate effective prescriptions that modify classical neutrino distributions, enabling their incorporation into large-scale simulations.
    
    In this talk, I will present recent progress on determining the asymptotic states reached after the onset of a flavor instability, a key ingredient for subgrid models. I will focus in particular on two classes of instabilities that have garnered significant attention, namely, "fast" and "collisional" flavor instabilities.
    
    Ponente: Julien Froustey (IFIC, CSIC-UV)
    
    JFroustey_TeVPA2025_compressed.pdf
- 16:15 → 16:45
  
  Coffee break 30m ADEIT
  
  ADEIT
- 16:45 → 18:30
  COS / DMI Room 1.1+1.2 (ADEIT)
  
  Room 1.1+1.2
  
  ADEIT
  
  Moderador: Martin Hirsch (Instituto de Fisica Corpuscular, CSIC - Universidad de Valencia)
  - 16:45
    
    Invited: Mapping Gravity with Extragalactic Streams and Citizen Science 15m
    
    Wide-field surveys like Euclid mark a new era of extragalactic stellar stream studies, with exciting applications in measuring baryon and dark matter distributions, and connecting galaxies to their cosmological context.
    
    I present results from a pilot study combining Euclid imaging with Zooniverse classifications to detect and analyze stellar streams of extragalactic systems. We use projected stream morphologies to constrain the shape and barycenter of each host galaxy’s potential, jointly probing baryonic and dark matter distributions. These inferences complement lensing, with sensitivity to halo geometry on tens of kpc scales. The method enables both stacked, population-level constraints on halo triaxiality and barycenters, and individual-halo inference on the same. Already, we find promising agreement with ΛCDM predictions. Our program will identify thousands of streams, enabling precise constraints on halo shapes and barycenters across large samples and redshifts, offering a new dynamical test of dark structures.
    
    Ponente: Nathaniel Starkman (Massachusetts Institute of Technology)
    
    Starkman_TeVPA_2025.pdf Starkman_TeVPA_2025.pptx
  - 17:00
    
    Dark Matter distribution in galaxies, and machine learning 15m
    
    I will illustrate the development of new methods, and their results, to determine the dark matter distribution in field galaxies.
    Machine learning algorithms trained within the synthetic environment of numerical cosmological simulations -such as the IllustrisTNG- offer the potential to validate and test the reliability of the Dark Matter distribution in such controlled environment, before being applied to real Universe targets.
    I will show recent developments in this field commenting on advantages and drawbacks of this innovative methodology.
    
    Ponente: Fabio Iocco (Università di Napoli "Federico II")
    
    iocco-AI-TeVPA-Valencia25.pdf
  - 17:15
    
    Cosmological parameters inference via galaxy clustering and dark sirens cross-correlation 15m
    
    Gravitational Waves (GW) from compact binary coalescence like Black Holes or Neutron Stars behave like standard sirens and can be used to perform cosmological inference, in particular on the Hubble constant. In order to build the Hubble diagram, however, an independent measurement of the redshift is required, which is not always available. Here we propose a novel methodology which does not require knowledge of the redshift, and which is, instead, based on the calculation of the cross-correlation (cross-correlation function or cross-correlation power spectrum) between catalogs of GW events and large-area galaxy catalogs like the forthcoming Euclid.
    In particular, we consider forecasts based on characteristics of future third generation GW observatories like the Einstein Telescope and Cosmic Explorers. We show that in 10 years of data-taking the achievable error on the Hubble constant is about 0.5 per cent, which is enough to solve the Hubble constant tension.
    
    Ponente: Alessandro Cuoco (University of Turin & INFN)
    
    TeVPA_Valencia_Nov2025.pdf
  - 17:30
    
    Probes of dark matter and physics beyond the Standard Model with the Pierre Auger Observatory 15m
    
    Charged ultra-high-energy cosmic rays are thought to be produced by astrophysical
    processes such as shock acceleration. Their subsequent interactions also contribute to
    the production of secondary gamma rays and neutrinos. However, physics beyond the Standard Model
    at very high energy scales could also contribute to the fluxes of both charged and neutral
    ultra-high-energy particles. Examples include the decay of metastable superheavy dark matter
    through non-perturbative effects such as instantons. Since such processes tend to predict a
    higher fraction of gamma rays and neutrinos compared to astrophysical scenarios, they
    can be constrained by the stringent upper bounds on gamma-ray and neutrino fluxes
    from the Pierre Auger Observatory. In this contribution, we will review these "top-down"
    physics scenarios and discuss how they are probed by data from the Pierre Auger Observatory.
    
    Ponente: Günter Sigl (University of Hamburg)
    
    bsm-auger.pdf
  - 17:45
    
    Invited: Recent Results and Perspectives on Dark Matter Searches with the IceCube Neutrino Observatory 15m
    
    Despite extensive astrophysical evidence supporting its existence, the nature of dark matter remains one of the most compelling open questions in modern physics. One promising approach for probing its properties is indirect detection, which involves searching for its signals from regions of the universe where dark matter is expected to be concentrated. Such searches often target astrophysical objects where the gravitational effects lead to the accumulation of significant amounts of dark matter, such as galaxies, the Sun, or the Earth. The IceCube Neutrino Observatory, located at the South Pole, has been detecting a steady flux of astrophysical neutrinos, spanning an energy range of a few GeV to PeV, over the last decade. These data have enabled IceCube to conduct indirect detection searches for dark matter, placing competitive constraints on various theoretical models across different target objects. This talk will highlight recent results from these searches, especially with the Earth, the Sun, and the neighbouring galaxies, and discuss future perspectives for probing dark matter with IceCube.
    
    Ponente: Woosik Kang (Drexel University)
    
    TeVPA2025-IceCube_DM_Overview-WKang.pdf
  - 18:00
    
    Indirect searches for dark matter signals from the Galactic Center with IceCube DeepCore and IceCube Upgrade 15m
    
    Understanding the nature of dark matter remains one of the central challenges in modern physics. A promising strategy to probe its properties is indirect detection which searches for excesses of Standard Model particles produced by dark matter annihilation or decay in astrophysical objects. The Galactic Center is a particularly compelling target due to its high dark matter density and relative proximity to the Earth. In this work, we report on a search for neutrinos originating from GeV-scale dark matter in the Galactic Center using nearly a decade of data from IceCube DeepCore. We also present sensitivity projections for the upcoming IceCube Upgrade, designed to significantly enhance detection capabilities in the sub-TeV energy range. These efforts expand IceCube’s reach toward sub-TeV dark matter masses and yield world-leading limits for some dark matter scenarios.
    
    Ponente: Nhan Chau (IIHE, ULB, Brussels)
    
    2025-11-003-TeVPA-2025-NChau.pdf
  - 18:15
    
    Indirect dark matter searches towards the Sun using the full ANTARES dataset 15m
    
    Weakly interacting massive particles (WIMPs) are among the leading candidates for dark matter. According to theoretical models, they could accumulate over time within massive astrophysical bodies such as the Sun and annihilate into Standard Model particles, including neutrinos. Neutrino telescopes, consisting of large arrays of photodetectors immersed in a transparent medium, allow us to search for this indirect signature of dark matter by detecting neutrinos originating from the solar core.
    In this contribution we will report on an indirect search for dark matter toward the Sun that was performed using 15 years of data collected by the ANTARES neutrino telescope, from 2007 to 2022. Three different reconstruction methodologies were applied to the neutrino events: two standard algorithms developed by the Collaboration and used in various analyses, and a new method based on Machine Learning techniques. An unbinned likelihood analysis was conducted to determine upper limits on the spin-dependent and spin-independent WIMP-nucleon scattering cross-sections for WIMP masses ranging from 35 GeV/c² to 10 TeV/c² and for three different annihilation channels.
    
    Ponente: Chiara Poirè
    
    Talk_ANTARES_DMSun_TeVPA_CPoire-JGarciaMendez.pdf
- 16:45 → 18:30
  Dark Matter: Direct Detection Room 3.1+3.2 (ADEIT)
  
  Room 3.1+3.2
  
  ADEIT
  
  Moderador: Madeleine Zurowski (University of Toronto)
  - 16:45
    
    Backgrounds in LZ and Radon Tagging 15m
    
    LUX-ZEPLIN (LZ) is a dark matter experiment located at the Sanford Underground Research Facility in South Dakota, USA, employing a 7 tonne active volume of liquid xenon in a dual-phase time projection chamber. Its deep underground location and an extensive material assay program enable LZ to have achieved an observed background level of 6.3±0.5×10$^{−5}$ events/keVee/kg/day in the WIMP search region. With a combined exposure of 4.2 tonne-years from all science campaigns, LZ has placed the most stringent limits on spin-independent WIMP-nucleon cross section down to 2.2×10${}^{−48}$ cm$^2$ for a 40 GeV/c$^2$ WIMP mass. This talk will include innovations in background assessment and mitigation, highlighting the flow-based tagging of radon-chain decays in the LZ TPC, as applied in LZ's 2024 WIMP search.
    
    Ponente: Nicolas Angelides (University of Zurich)
    
    TevPa LZ-Nicolas 2025.pdf
  - 17:00
    
    Dark Matter Detection in the DarkSide-20k Era: The Challenge of Radiopurity and Low Background 15m
    
    DarkSide-20k is a next-generation, direct dark matter search experiment
    located at LNGS (Italy), aiming for a background-free exposure of 200 tonne-years,
    i.e < 0.1 neutron WIMP-like event. The core of the detector is a dual-phase
    Time Projection Chamber (TPC) filled with 50 tonnes of low radioactivity
    liquid argon. The entire TPC wall is surrounded by a 15 cm of pure
    polymethylmethacrylate (PMMA), which acts as a neutron veto, immersed in
    a second low-radioactivity liquid argon bath enclosed in a stainless steel
    vessel. The entire detector is enclosed in a protoDUNE-like cryostat filled with
    600 tons of atmospheric argon. TPC and neutron veto are equipped with
    large-area Silicon Photomultiplier (SiPM) array detectors. SiPMs are arranged
    in a compact design intended to minimise the material used for circuit boards,
    cables, and connectors, forming a photo-detection unit.
    A central challenge for achieving the experiment’s sensitivity goal, 7.4 x 10-48
    cm2 for 1 TeV WIMP, is ensuring a stringent radiopurity. In this talk, I will
    present the comprehensive radiopurity strategy adopted by DarkSide-20k,
    including the material assay campaign, selection procedures, and
    Implementation of a radiopurity protocol throughout the detector construction
    phase. I will also provide an overview of background sources and detail the
    mitigation techniques employed to reach the experiment’s ambitious
    background-free target.
    
    Ponente: Daria Santone (University of Oxford)
    
    TevPA_Santone.pdf
  - 17:15
    
    DarkSide-20k TPC Mockup: A Step Towards the Realization of DS-20k 15m
    
    The Global Argon Dark Matter Collaboration is currently developing its flagship detector,
    DarkSide-20k (DS-20k), a multi-tonne-scale experiment designed for the direct detection of the
    weakly interacting massive particles using a double-phase Liquid Argon Time Projection
    Chamber (LAr TPC) with 20.2 tonnes of fiducial mass. The shift from its predecessor,
    DarkSide-50, with 46.4 kg of active mass, to a significantly larger detector relies on intermediate
    prototypes for technical design validation. The DS-20k TPC Mockup is one such prototype
    detector intended to replicate the critical aspects of the functionality of DS-20k in a tonne-scale
    setup. The Mockup detector was assembled in a clean room of the Nuova Officina Assergi
    (NOA) facility at the Laboratori Nazionali del Gran Sasso (LNGS) above ground in early 2025,
    and was later transported to Hall C of the LNGS underground laboratory to be put inside a
    cryostat.
    The main tests focused on the long-term exposure of the Clevios coatings, an innovative
    conductive polymer, to LAr, analyzing gas-pocket formation, and conducting tests of the high
    voltage delivery. The detector is now decommissioned and transported back to the NOA facility
    for visual inspection for any possible damage or degradation. This talk presents the assembly,
    operation, ongoing analysis, findings, and future prospects of the Mockup project.
    
    Ponente: Clea Sunny (Astrocent, CAMK PAN)
    
    CleaSunny_Mockup_TeVPA.pdf
  - 17:30
    DarkSide-20k 26 m2 SiPM Detectors: Production and Characterisation 15m
    
    Darkside-20k is a global direct dark matter search experiment situated underground at LNGS (Italy), designed to reach a total exposure of 200 tonne-years, nearly free from instrumental backgrounds. The core of the detector is a dual-phase Time Projection Chamber (TPC) filled with 50 tonnes of low-radioactivity liquid argon. The entire TPC wall is surrounded by polymethylmethacrylate (PMMA), which acts as a neutron veto, immersed in a second low-radioactivity liquid argon bath enclosed in a stainless-steel vessel. The TPC and the neutron veto are enclosed within the cryostat volume, which is filled with 650 tonnes of atmospheric argon comprising the outer veto volume.
    
    Both TPC and vetoes are instrumented with large-area light detectors utilising a custom Silicon Photo-Multiplier (SiPM) technology optimised for high optical photon detection efficiency and low noise at liquid argon temperatures.
    
    SiPMs are arranged in a compact design meant to minimise the material (and hence the radioactive budget) used for the active electronics, cables and connectors: the PhotoDetection Units (PDUs). A PDU comprises 16 "Tiles", each containing 24 SIPMs, together with front-end electronics, and a motherboard (which distributes voltage and control signals, sums Tiles channels, and drives the electrical signal transmission), providing a single readout area of 10x10 cm$^2$. The TPC will be equipped with 518 PDUs and the neutron veto with another 120, for an unprecedented total active SiPM area of 26 m$^2$.
    
    The talk will focus on the production of the TPC and veto PDUs, describing the assembly chain in Italy and in the UK institutes, to underline the rigorous QA/QC procedures, up to the final characterisation between Italy, UK and Poland.
    
    Tests have been extensively performed at any stage of the production (mechanical tests, electrical functional tests, I-V curves, noise measurements, dust counting), and in particular in liquid nitrogen baths (pulsed laser response to check the photodetection efficiency), either for the single Tiles and for the fully assembled PDUs, with the purpose to assign a "quality passport" to each component, in order to meet the stringent requirements for the DarkSide-20k photosensors.
    
    References
    
    DarkSide-20k Collaboration, “Quality assurance and quality control of
    the 26 m$^2$ SiPM production for the DarkSide-20k dark matter
    experiment”, Eur.Phys.J.C 85 (2025) 5, 534
    
    DarkSide-20k
    Collaboration, “Production, Quality Assurance and Quality Control of
    the SiPM Tiles for the DarkSide-20k Time Projection Chamber",
    submitted
    
    DarkSide-20k Collaboration, “Construction and
    characterisation of the DarkSide-20k2 veto silicon photo-multiplier
    detectors”, in review
    
    Ponente: Paolo Franchini (University of Oxford)
    
    Franchini-TeVPA25.pdf
  - 17:45
    
    Exploring Axion Dark Matter in the RADES Collaboration 15m
    
    The Relic Axion Detector Exploratory Setup (RADES) collaboration works on the development of new techniques for axion searches. Axions are hypothetical pesudoscalar pseudoNambu-Goldstone bosons that appear as part of the solution to the the strong CP problem of QCD. At the same time they could also be the answer to one of the most puzzling questions on cosmology, the Dark Matter problem.
    In RADES we focus on haloscope detectors, a well-established technique that exploits the axion-photon conversion in strong magnetic fields and resonant cavities. Over the past years, we pioneered the development of novel microwave resonator arrays in order to reach a region of the parameter space very difficult to access for conventional haloscopes, and performed two consecutive data takings with high temperature superconducting (HTS) cavities at the SM18 magnet testing facility at CERN.
    Our current efforts are directed toward integrating quantum metrology technologies to significantly improve sensitivity. Specifically implementing superconducting transmon qubits as part of our readout system, these sensors would allow the detection of single microwave photons generated by axion conversion.
    In this talk I will present an overview of the RADES collaboration, briefly summarising our latest results with HTS coated cavities. And our developments on the implementation of a quantum-limited axion search.
    
    Ponente: Cristian Cogollos Triviño (Max Planck Institute for Physics)
    
    Cogollos_RADES_Talk_TeVPA2025.pdf
  - 18:00
    
    Axion searches with BabyIAXO 15m
    
    BabyIAXO is the initial stage of the International Axion Observatory (IAXO), designed to search for solar axions and axion-like particles (ALPs) with unprecedented sensitivity. It incorporates a straight, large-aperture dipole magnet, precision X-ray optics, and ultra-low background detectors, enabling both early-stage data acquisition and validation of the experimental approach for the full-scale IAXO. With projected sensitivity to axion–photon couplings down to gaγ∼10E−11 GeV−1, BabyIAXO will surpass current helioscope limits and explore previously inaccessible regions of ALP parameter space. Beyond its role in instrumentation development, BabyIAXO is expected to deliver meaningful physics results and contribute directly to the global effort to uncover the properties and existence of axions. In addition to solar axions, its infrastructure offers broad physics potential, including searches for dark matter axions with haloscopes, supernova axions, other WISPs such as hidden photons and chameleons, and even high-frequency gravitational waves.
    
    Ponente: Gloria Luzón Marco (Centro de Astropartículas y Física de Altas Energías (CAPA)-UNIZAR)
    
    BabyIAXO_TeVPA.pdf
  - 18:15
    
    Probing Benchmark Models of Hidden-Sector Dark Matter with DAMIC-M 15m
    
    The DAMIC-M (DArk MAtter in CCDs at a Modane) collaboration aims to directly detect dark matter in Charge-Coupled-Devices (CCDs). Utilizing fully depleted CCDs and a floating-gate (“skipper”) amplifier, the detector — operated deep underground at the Laboratoire Souterrain de Modane (LSM) — can resolve eV-scale interactions of Hidden Sector Dark Matter. The Low Background Chamber (LBC), the DAMIC-M prototype detector, features two Skipper-CCD modules with a combined mass of 25g. The LBC has set world leading limits on dark matter-electron scattering, excluding regions of parameter space corresponding to the freeze-in and freeze-out production mechanisms. We report on the science results from the LBC, the performance of the CCD Modules, and status of detector construction at LSM.
    
    Ponente: Sravan Munagavalasa (University of Chicago)
    
    TeVPa2025_DAMICM_openAdobe_Acrobat_Reader_only.pdf TeVPa2025_DAMICM.pdf
- 16:45 → 18:30
  GWA / CRA / CPP Room 2.1+2.2 (ADEIT)
  
  Room 2.1+2.2
  
  ADEIT
  
  Moderador: Jacobo López-Pavón (IFIC UV-CSIC)
  
  TeVPaNA62_BD_upload.pdf
  - 16:45
    
    Dark Matter Mounds from Supermassive Star Collapse: A General Relativistic Treatment 15m
    
    The formation history of supermassive black holes (SMBHs) influences the surrounding distribution of dark matter (DM). While slow, adiabatic growth is known to produce high DM density regions referred to as “spikes,” more realistic formation scenarios, such as collapse from a stellar progenitor, generate weaker overdensities called “mounds”. Upcoming gravitational wave (GW) detectors will be able to probe extreme mass-ratio inspirals (EMRIs) over hundreds of thousands of orbital cycles. Thanks to the long duration of these signals, it will be possible to measure with great precision any effects of the environment around SMBHs on the smaller companion black hole. If DM overdensities do form close to SMBHs, their environmental effects will be distinguishable from vacuum or baryonic matter. Recent studies have shown the importance of taking a fully relativistic approach in modeling the dephasing of GWs from EMRIs due to DM. However, relativistic studies have focused exclusively on the case of idealized adiabatic growth. In our research, we extend the calculation of DM mounds to the full general relativistic regime and consider how a more realistic treatment of stellar collapse may impact the evolution of DM orbits. We find that the distribution function of DM is significantly altered from the adiabatic case near the black hole, with a clear depletion in the low-energy regions of the parameter space. These results will be crucial in modeling future EMRI detections, potentially enhancing our understanding of both the behavior of dark matter in strong gravity regions and the formation history of supermassive black holes.
    
    Ponente: Roberto Caiozzo (SISSA)
    
    Valencia rel spike.pdf
  - 17:00
    
    MUTE: Calculations for Cosmic-Ray Muons in Deep Underground Laboratories 15m
    
    MUTE (MUon inTensity codE) is a Python program that performs calculations for cosmic-ray muons underground and underwater. It combines two state-of-the-art programs, DAEMONFLUX and PROPOSAL, to provide comprehensive calculations for muon intensities, total muon fluxes, energy and angular spectra, and mean muon energies at the surface, in deep underground laboratories — under both flat overburdens and mountains — and underwater. For precise modelling, the program takes into account rock densities and chemical compositions for various underground labs as well as topographic map profiles of mountainous overburdens. Our results show excellent agreement with available experimental data for most underground sites. Additionally, our model predicts the amplitude of seasonal variations in the atmospheric muon flux to a high degree of precision. MUTE is an open-source, publicly available program, providing a solid framework for accurate muon flux predictions in various underground environments, essential for applications in cosmic ray physics and dark matter searches.
    
    Ponente: William Woodley (University of Alberta)
    
    TeVPA_2025_MUTE.pdf
  - 17:15
    
    New physics searches at the NA62 experiment 15m
    
    The NA62 experiment at CERN is designed to measure the highly-suppressed decay $K^{+} \to \pi^{+}\nu\bar{\nu}$ and has collected a large sample of $K^+$ decays in flight during Run 1 (2016-2018) and Run 2 (since 2021). Searches for the decay $K^{+}\rightarrow\pi^{+}X$ using data from 2016-2022, set upper limits on the branching ratio at the $10^{-11}$ level, constraining a broad range of New Physics scenarios, including Dark Photon, Scalars and Axion-Like Particles.
    The NA62 experiment at CERN can also operate in beam-dump mode, enabling searches for long-lived particles produced in 400 GeV proton interactions with the dump. A blind analysis of a sample of $1.4 \times 10^{17}$ protons on dump collected in 2021 led to the first NA62 search for long-lived New Physics particles decaying in flight to hadronic final states.
    
    Ponente: Babette Döbrich (Max Planck Institute for Physics, Germany)
    
    TeVPaNA62_BD_upload.pdf
  - 17:30
    
    Up-scattering production of a sterile fermion at neutrino experiments 15m
    
    We consider the possible production of a new MeV-scale fermion at the COHERENT, LZ and XENONnT experiments, and the future DUNE detector. The new fermion, belonging to a dark sector, can be produced through the up-scattering process of neutrinos off the nuclei and the electrons of the detector material, via the exchange of a light mediator. We explore the possibility of generalized interactions, that is a scalar, pseudoscalar, vector, axial or tensor mediator. We perform a detailed statistical analysis of the COHERENT, LZ and XENONnT datasets and obtain up-to-date constraints on the couplings and masses of the dark fermion and mediators. Likewise, we include sensitivities for the DUNE detector. Finally, we briefly comment on the stability of the dark fermion.
    
    Ponente: Pablo Muñoz Candela (IFIC, CSIC-UV)
    
    Pablo_Munoz_Candela.pdf
  - 17:45
    
    Clearing the Fog: Constraining Light Mediators with CEνNS Signals 15m
    
    The recent observation of Coherent Elastic Neutrino–Nucleus Scattering (CE$\nu$NS) from solar $\rm ^8B$ neutrinos by dark matter direct detection experiments marks the first identification of the so-called “neutrino floor”. Far from being a mere background for dark matter searches, this signal opens a novel window to probe light new physics.
    
    In this talk, I will present new constraints on light scalar and vector mediators coupling to neutrinos and quarks, derived from recent data from these experiments. I will show that they already provide competitive — and in some cases leading — bounds in the sub-GeV mass range. I will also discuss subdominant but non-negligible contributions from neutrino–electron scattering and the Migdal effect, which can noticeably impact the detected event rates.
    
    These results highlight the growing potential of dark matter detectors as precision neutrino observatories, capable of testing a wide class of light mediator scenarios.
    
    Ponente: Pablo Blanco Mas (IFT CSIC/UAM)
    
    pbm_tevpa_talk.pdf
  - 18:00
    
    The LEGEND Project for the search of Neutrinoless Double Beta Decay 15m
    
    Neutrinoless double-beta decay is a hypothetical nuclear process, (A,Z) → (A,Z+2) + 2e⁻, that is not allowed by the Standard Model since it violates the total lepton number conservation by two units.
    The discovery of 0νββ would have profound theoretical implications: it could help explain the matter-antimatter asymmetry in the universe and it is the only practical way to determine if the neutrino is its own antiparticle (a Majorana neutrino), providing important insight into the origin of neutrino mass and access to the absolute neutrino mass scale through the measurement of the effective Majorana mass.
    An extensive experimental effort is underway worldwide, with numerous projects employing a variety of detection technologies to search for this rare transition.
    One of the most promising international experimental projects dedicated to the search for neutrinoless double beta decay is the LEGEND (Large Enriched Germanium Experiment for Neutrinoless ββ Decay) experiment aiming to detect the 0νββ decay Germanium-76 (⁷⁶Ge).
    Two phases are foreseen for this experimental project.
    LEGEND-200, the initial phase, currently collecting data at the INFN Gran Sasso National Laboratory in Italy, has 142 kg of enriched germanium detectors installed and aims to achieve a half-life sensitivity for neutrinoless double-beta decay in 76Ge of approximately 10²⁷ years. This may be possible by a projected background index of 0.6 counts/(FWHM·t·yr) and a total exposure of 1 tonne·year.
    The subsequent phase, LEGEND-1000, is designed to surpass a sensitivity of 10²⁸ years by operating 1 tonne of enriched germanium detectors, accumulating more than 10 tonne·years of exposure at a background index of about 0.025 counts/(FWHM·t·yr). With this level of sensitivity, LEGEND-1000 will be capable of probing the entire inverted neutrino mass ordering region.
    
    Ponente: Nicola Canci (INFN-Naples)
    
    2025-11-03_Canci_TeVPA2025_Valencia.pdf
  - 18:15
    
    A portal to the SM for resonant SIMPS 15m
    
    Strong Interacting Massive Particles are a well motivated DM candidate. In particular we took into consideration a QCD-like theory with three flavours, where the DM candidate is a dark pion. In Ref[2405.10367], it has been found that a non-vanishing theta angle would trigger resonant processes which would give rise to the observed relic density, together with providing velocity dependent self-interactions without a light mediator. In this work, we studied its interactions with SM particles in the case of a dark photon portal, focusing on the thermalizations and the stability issues of the dark pions. In the scenario we considered, a dark pion mass in the window of 10-50 MeV would be consistent with all bounds, and would explain successfully astrophysical observations in the context of SIDM.
    
    Ponente: Luca Marsili (IFIC, CSIC-UV)
    
    SIMPS_TevPA.pdf
- 16:45 → 18:30
  Gamma Rays: Experiments Salón de Actos (ADEIT)
  
  Salón de Actos
  
  ADEIT
  
  Moderador: Rubén López-Coto
  - 16:45
    
    Science program of the MAGIC telescopes 15m
    
    MAGIC is a system of two 17-m Cherenkov telescopes located at the Observatorio Roque de los Muchachos on the Canary Island of La Palma, Spain. The telescopes have been in operations for two decades and during that time, the observation program evolved, adjusting to the new discoveries and ideas in astrophysics. Every year the telescopes observe a mixture of Galactic and Extragalactic targets. Ample time is devoted to transient events and observations of Targets of Opportunity, including also multi-messenger triggers. Selected sources are also covered in multi-year monitoring programs. Since a few years, the call for observation time is partially open, allowing for external scientists to submit MAGIC observation proposals. In 2025 the MAGIC and LST Collaborations agreed on a common observational strategy and a single Time Allocation Committee.
    I will present the summary of the MAGIC observation program and present a few recent highlights of the observations of Galactic and extragalactic physics, as well as of using gamma-ray observations in studies of the fundamental physics
    
    Ponente: Julian Sitarek (University of Lodz)
    
    202511_tevpa_science_MAGIC.pdf
  - 17:00
    
    Analysis of joint MAGIC+LST-1 observations 15m
    
    In 2019, the first Large-Sized Telescope (LST-1) of the Cherenkov Telescope Array Observatory (CTAO) for the Northern Hemisphere array site started observations next to the two MAGIC telescopes at the Roque de los Muchachos Observatory in La Palma, Canary Islands. Since 2020 an increasing number of joint observations involving all three telescopes have been carried out. Joint MAGIC+LST-1 observations show a clear improved performance compared to MAGIC or LST-1 alone: indeed, the increase in sensitivity allows for the detection of about 30% weaker sources with respect to the sole MAGIC observation.
    
    To analyze data from these joint observations, a dedicated analysis pipeline, magic-cta-pipe, has been developed. This software looks for MAGIC events which are coincident with LST-1 events, using their timestamps; then, it uses random forests trained on Monte Carlo simulations to reconstruct, for these events, the main properties of the primary: energy, direction and particle type (gamma or hadron). Given the large volume of data collected since 2020 and the complexity of the joint analysis in itself, significant effort has been directed towards automation of the low-level data selection and of the generation of high-level data products, from which physical results can be easily retrieved. This automation has already been used to process archival data that are actively being used to study gamma-ray emission from numerous astrophysical sources.
    
    We present the status of the joint pipeline and some selected scientific results obtained with it.
    
    Ponente: Elisa Visentin (University of Torino, INFN Torino)
    
    TeVPA_joint_Visentin.pdf
  - 17:15
    
    The ASTRI Mini-Array: Overview and first results 15m
    
    The ASTRI Mini-Array is an international project led by the Italian National Institute for Astrophysics (INAF) to develop, build, and operate nine Cherenkov telescopes at the Observatorio del Teide, on the island of Tenerife. The array is planned to operate for at least 8 years, performing deep observations of Galactic and extragalactic sources in the energy range from 1 to 200 TeV. These observations will provide key information on some open questions in very-high-energy astrophysics like the nature of the so-called PeVatrons, extreme Galactic accelerators able to produce particles with energies above the PeV, and thought to be the main contributors to the cosmic-ray spectrum at those energies.
    
    Out of the nine telescopes of the array, one of them is already installed and performing observations since November 2024, having accumulated around 300h of technical and scientific data. The remaining eight telescopes are expected to become operational in different phases starting from the second half of 2025 and until their expected completion by 2026. This contribution will overview the ASTRI Mini-Array design, technologies, and science cases, as well as present the results from the calibration and scientific observations performed with the already operating telescopes.
    
    Ponente: Edgar Molina (Instituto de Astrofísica de Canarias (IAC))
    
    TeVPA_ASTRI_EdgarMolina.pdf
  - 17:30
    
    The ASTRI Mini-Array follow-up of transient events in TeV band 15m
    
    The LHAASO detection of the very high-energy (VHE) emission component from gamma-ray bursts (GRBs) up to the multi-TeV regime proved the importance of ground-based gamma-ray facilities in exploring the physics of these enigmatic objects up to the extreme energies. In recent years, significant efforts in improving the strategies for follow-up of transient events have been performed within the VHE community, particularly in the current era of multi-messenger triggers. The association of high-energy neutrinos and gravitational waves with transient astrophysical sources will indeed provide insights into the physics of extreme cosmic accelerators. The ASTRI Mini-Array experiment, composed of nine imaging atmospheric Cherenkov telescopes in dual-mirror configuration, will play an important role in studying the TeV emission in transient events. The array is being completed at the Teide Observatory site, where the first telescopes are already acquiring data. The ASTRI Mini-Array will be equipped with a dedicated transient handler that will allow us to perform specific follow-up campaigns on a wide range of astrophysical sources like GRBs, galactic transients, and the possible VHE electromagnetic counterpart of neutrinos and gravitational waves. The presence of multiple observing facilities at the Teide Observatory and the closeness to the Northern site of the Cherenkov Telescope Array Observatory will guarantee the unique opportunity to perform simultaneous follow-up in a wide energy range and in a multi-band context. We studied the performance of the ASTRI Mini-Array in detecting the possible TeV signatures from nearby on- and off-axis GRBs. The implementation and optimization of a possible ASTRI Mini-Array observational strategy based on specific science cases will also be discussed.
    
    Ponente: Alessandro Carosi (INAF-OAR)
    
    TEVPA2025ASTRI-AC-V2.pdf
  - 17:45
    
    Towards the evaluation of a candidate layout for the SWGO outer array to events above 30 TeV 15m
    
    The Southern Wide-field Gamma-ray Observatory (SWGO) will be a next generation ground array experiment probing the Southern sky in search of gamma-ray sources from the Galactic plane. The collaboration has chosen as primary site Pampa la Bola in the Atacama Astronomical Park (Chile) at 4770 m above the sea level. SWGO will detect the secondary particles through Water Cherenkov Detectors (WCD). The experiment will have a wide field-of-view and almost 100% duty cycle. A central dense core of WCDs will make SWGO capable of studying events of energy as low as 100 GeV, but the recent results of both HAWC and LHAASO (both in the northern hemisphere) have opened the discussion of the PeV range and the science case of PeVatrons. SWGO will be the first ground-based experiment of its kind operating in the TeV to PeV range in the southern hemisphere. The collaboration is evaluating multiple options for the outer array. In this contribution we will show the performance of the current candidate design of SWGO from 30 TeV up to PeV scale, discussing both energy (15%) and angular resolution (0.15 deg).
    
    Ponente: Andrea Negro (University of Turin & INFN Turin)
    
    TeVPa-Andrea-Negro-UHE-SWGO-1.pdf
  - 18:00
    
    Status of ALPACA to explore southern sub-PeV gamma-ray sky from Bolivia 15m
    
    ALPACA is a new air shower array experiment under construction in Bolivia. Surface array with 401 scintillating counters covers an area of 82,800 m^2. Together with the underground water-Cherenkov muon detectors covering 3600 m^2 established by the Tibet ASgamma group, a high CR/gamma separation power is achieved. ALPACA realizes a wide-field gamma-ray survey at 10-1000TeV energy range for the first time in the southern hemisphere. Currently a prototype ALPAQUITA array with 97 surface detectors is operating and the construction of the first muon detector will start soon.
    In this contribution, we will outline the project of ALPACA and present the performance of ALPAQUITA and the status of the muon detector construction.
    
    Ponente: Takashi Sako (ICRR, University of Tokyo)
    
    TeVPA2025_ALPACA_Sako_20251103.pdf
  - 18:15
    
    Deployment of Imaging Air Cherenkov Telescopes for 10 TeV - PeV Gamma-Ray Astronomy 15m
    
    To explore the largely uncharted dark matter mass range between 10 TeV and several PeV, the Dark100 experiment aims to deploy an array of six Imaging Air Cherenkov Telescopes (IACTs) optimized for detecting gamma rays at these extreme energies. These telescopes, originally developed for the Panoramic Search for Extraterrestrial Intelligence (PANOSETI), provide a scalable and cost-effective platform for dark matter annihilation studies, designed to complement and enhance the collective sensitivity of current and future gamma-ray observatories.
    
    In addition to the three-telescope demonstrator array currently operating at Lick Observatory, a new four-telescope array is being installed at Palomar Observatory. The instruments follow the same core PANOSETI design, with minor enhancements to optics, electronics, and control software for improved autonomous operation.
    
    We report on the ongoing deployment at the Palomar site, and present first data, along with an outlook on future science goals for PANOSETI and Dark100.
    
    Ponente: Yuriy Popovych (Ruhr University Bochum)
    
    TevPA_25_Popovych.pdf
- 16:45 → 18:30
  Gamma Rays: Extragalactic Salón de Grados (ADEIT)
  
  Salón de Grados
  
  ADEIT
  
  Moderador: Mónica Seglar-Arroyo (IFAE)
  - 16:45
    
    Probing Extreme Particle Acceleration in Blazars: A New Population of EHSP Candidates and Their TeV Prospects 15m
    
    Extreme high-synchrotron peaked blazars (EHSPs), defined by
    synchrotron peak frequencies exceeding 10^{17} Hz, represent a particularly elusive and energetic subclass of blazars. Their spectral properties challenge standard emission models and offer valuable constraints on particle acceleration processes in relativistic jets. In this work, we present a systematic study of 124 gamma-ray blazars selected for high synchrotron peaks and low variability. Using multi-wavelength data from Swift-UVOT/XRT, Fermi-LAT, and archival observations via the SSDC SED Builder, we model their spectral energy distributions with a one-zone synchrotron/synchrotron-self-Compton framework. We identify 66 new EHSP candidates, significantly enlarging the known sample. A clear correlation emerges between synchrotron peak frequency and the magnetic-to-kinetic energy density ratio, with the most extreme EHSPs approaching equipartition. This indicates that as the synchrotron peak shifts to higher frequencies, the energy stored in the magnetic field
    becomes comparable to that of the radiating electrons, pointing to a more balanced and energetically efficient jet configuration in the most extreme sources. We also confirm that the synchrotron peak frequency is inversely correlated with Compton dominance, consistent with expectations from the blazar sequence. Finally, we assess detectability with CTAO and identify up to nine EHSPs that could be detected at >5σ in
    20-hour exposures, supporting targeted follow-up by next-generation TeV observatories.
    
    Ponente: María Láinez (IPARCOS-UCM)
    
    EHSPs_talk_TeVPA.pdf
  - 17:00
    
    VHE gamma-ray observations of bright Blazars with CTAO LST-1 15m
    
    Blazars are a sub-class of Active Galactic Nuclei (AGN) and constitute the most populous class of sources in the extragalactic very-high-energy (VHE) sky. They are characterized by stochastic variability that spans from radio to VHE gamma rays (E > 100 GeV), whose origins are still being debated. Detecting more VHE blazars at different energies and distances is crucial for a better understanding of their emission mechanisms.
    The Large-Sized Telescope prototype (LST-1) of the Cherenkov Telescope Array Observatory (CTAO) is located on the Roque de los Muchachos in La Palma, Spain. Due to its large photon collection area, it is sensitive to energies down to tens of GeV, making it the best-suited instrument to observe gamma-ray sources such as distant AGN that are affected by the photon-photon interactions with the extragalactic background light (EBL). From 2020 to 2022, we accumulated more than 150 hours of data of several well-known AGN with redshifts in the range 0.03 to 0.45: Mrk 421, Mrk 501, 1ES 1959+650, 1ES 0647+250, PG 1553+113. We present here the results on the spectral variability from early observations of bright AGN with LST-1. We perform a time-resolved spectral analysis using a Bayesian block algorithm for the brightest sources. We present joint analyses of contemporaneous Fermi-LAT and LST-1 data, covering the energy range from 300 MeV to 10 TeV, demonstrating good overall agreement between the two instruments. We also evaluated the potential of the LST-1 to detect flares from AGN by simulations of historical flares.
    
    Ponente: Chaitanya Priyadarshi (Instytut Fizyki Jadrowej PAN, Kraków)
    
    CTAO_LST1_5_bllacs_Priyadarshi.pdf
  - 17:15
    
    The Most Distant VHE Quasar: Probing OP 313’s power with LST-1 and MAGIC 15m
    
    Flat Spectrum Radio Quasars (FSRQs) are rarely detected at very-high-energy (VHE, E > 100 GeV) gamma rays due to their distance, soft spectra, and strong absorption from the Extragalactic Background Light (EBL). In December 2023, the Large-Sized Telescope prototype (LST-1) of the Cherenkov Telescope Array Observatory (CTAO) and the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) simultaneously detected for the first time VHE emission from the FSRQ OP 313 during an exceptionally bright emission phase, which is still echoing today. With a redshift of z = 0.997, OP 313 is the most distant blazar ever detected in this energy band, and among the most luminous persistent sources ever detected in the gamma-ray band. The detection marks a milestone for LST-1 and offers a unique opportunity to study both the extreme physics of FSRQs and the opacity of the Universe to gamma rays due to interaction with low energy EBL photons.
    
    OP 313 triggered one of the most extensive and productive multi-wavelength campaigns ever carried out on a flaring FSRQ, resulting in an exceptional dataset spanning from radio to VHE gamma rays. In this contribution, we present the first in a series of multi-wavelength studies of OP 313 extending to the VHE regime, combining data from LST-1, MAGIC, Fermi-LAT, Swift-XRT, and complementary optical and IR observations. We model the broadband emission using two leptonic scenarios and investigate the contribution of various external photon fields to the gamma-ray output. The unprecedented brightness of the flare and the high redshift of the source also allow us to place new constraints on the EBL intensity in the optical-to-near-IR range. This detection highlights the scientific potential of CTAO to probe the distant Universe and capture the most extreme blazar outbursts.
    
    Ponente: Mireia Nievas Rosillo (Instituto de Astrofisica de Canarias (IAC))
    
    OP313_TeVPA2025_v2.pdf
  - 17:30
    
    LST-1 Observations of Radio Galaxies: a study of flaring and quiescent states for NGC 1275 and IC 310 15m
    
    The discovery of radio galaxies as very high-energy (VHE, E > 100 GeV) gamma-ray emitters is one of the most significant legacy results from the current generation of Cherenkov telescopes. Contrary to the majority of TeV-detected active galactic nuclei, radio galaxies have misaligned jets (θ >10°). Thus, they offer unique views across multiple wavelengths to explore particle acceleration processes and zones without extreme relativistic beaming effects, as well as tools to test fundamental physics and cosmology (e.g. Extragalactic Background Light, Axion-Like Particles, Lorentz Invariance Violation). Bright and rapid TeV flares in nearby radio galaxies reveal intriguing phenomena, challenging conventional models that rely on strong Doppler enhancement.
    Here we present the first broadband multi-wavelength study of radio galaxies led by the first Large-Sized Telescope (LST-1) of the Cherenkov Telescope Array Observatory (CTAO), with > 50 hrs from 2022 to 2025 of very-high-energy observations of two nearby (z<0.019) radio galaxies in the Perseus cluster:
    NGC 1275 is the bright central galaxy of the Perseus cluster, for which we detect two bright flares, in December 2022 and January 2023, followed by longer quiescent states until present time. Collected contemporary multi-wavelength data reveal the broadband evolution of the source.
    IC 310 is a transitional object halfway between a blazar and a radio galaxy, with one of the fastest variabilities recorded in the VHE domain. Our observations reveal a long quiescent state briefly broken by a minor flare in December 2023.
    
    Ponente: Tora T.H. Arnesen (Instituto de Astrofísica de Canarias)
    
    251103_TeVPA_LST-1_Radio_Galaxies_v3.pdf 251103_TeVPA_LST-1_Radio_Galaxies_v3.pptx
  - 17:45
    
    Gamma-Ray Emission from AGN Disk Winds: A Case Study of the Nearby Seyfert Galaxy GRS 1734−292 15m
    
    Recent Fermi-LAT observations have revealed GeV gamma-ray emission from several radio-quiet Seyfert galaxies, challenging the traditional view that powerful jets are required to produce high-energy gamma rays in active galactic nuclei (AGNs). One such object, GRS 1734-292, is a nearby Seyfert galaxy with empirically weak starburst and jet activity, yet it exhibits a significant gamma-ray signal. In this talk, we present the first comprehensive multiwavelength modeling of GRS 1734−292 and investigate whether its gamma-ray emission can be attributed to an AGN disk wind. We model lepto-hadronic emission from a shocked interstellar medium (ISM) and a shocked wind region created by the interaction between the disk wind and the surrounding ISM. We identify two viable emission scenarios: a hadronic (pp-dominated) scenario and a leptonic (external-Compton-dominated) scenario, both consistent with the observed Fermi-LAT spectrum and multiwavelength constraints. Our results suggest that future observations with CTAO and SWGO could detect TeV emission from a disk wind in this source. Moreover, in the pp-dominated scenario, the disk wind could accelerate cosmic-ray protons beyond 1 EeV, offering new insights into the role of radio-quiet Seyfert galaxies as potential sources of ultrahigh-energy cosmic rays.
    
    Ponente: Nobuyuki Sakai (The University of Osaka)
    
    TeVPA2025_Sakai.pdf
  - 18:00
    
    Detection of Extra-galactic sources and Transients from LHAASO-WCDA 15m
    
    Key extragalactic sources of very-high-energy (VHE) gamma rays include blazars, gamma-ray bursts (GRBs), and transient phenomena. Studying these targets provides critical insights into astrophysical processes such as black hole accretion, particle acceleration, and explosion dynamics. The Large High Altitude Air Shower Observatory (LHAASO), located in China, is a multi-purpose facility designed to detect cosmic rays and gamma rays with energies ranging from a few hundred GeV to several hundred PeV. One of LHAASO's three sub-arrays, the Water Cherenkov Detector Array (WCDA), offers an ideal platform for capturing such flaring activity due to its wide field of view, high duty cycle, and sensitivity. This capability enables deeper understanding of the underlying astrophysical phenomena. In this talk, we will review extragalactic sources detected by LHAASO-WCDA and discuss transient event analysis, covering the monitoring framework, analysis pipeline, and preliminary results.
    
    Ponente: Min Zha (IHEP)
    
    tevpa2025_20251103_wcda.pdf tevpa2025_20251103_wcda.pdf
  - 18:15
    
    From Photons to Neutrinos: Advancing Multi-Messenger Blazar Modeling with Gammapy 15m
    
    Blazars are among the most powerful objects in the Universe and are prime candidates for producing ultra-high-energy cosmic rays and astrophysical neutrinos. Yet, despite decades of observations across the full electromagnetic spectrum, their emission mechanisms remain elusive. In today’s multi-messenger era, combining data from different cosmic messengers with advanced modeling tools is key to unlocking the secrets of these extreme sources.
    In this contribution, we present first results from a novel, user-friendly multi-messenger modeling approach built on the open-source package Gammapy. Our framework brings together observations from optical to very-high-energy gamma rays and operates directly on instrumental counts, minimizing biases introduced by intermediate flux extraction steps. We then introduce a new implementation in Gammapy that enables direct fitting of theoretical models, starting with Synchrotron Self-Compton scenarios, to these data.
    Focusing on blazars as key multi-messenger targets, we showcase how our framework enhances the ability to constraint emission models and present its extension to (lepto-)hadronic models and neutrino data. With this novel approach, we take a significant step toward true multi-messenger modeling and are paving the way to better understand extreme particle accelerators in the Universe.
    
    Ponente: Lea Heckmann (Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France)
    
    TeVPa_2025.pdf
- 18:45 → 21:00
  
  Welcome Cocktail 2h 15m ADEIT
  
  ADEIT
martes, 4 noviembre
- 9:00 → 10:30
  Plenary Session: III Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Michela Negro (Louisiana State University)
  - 9:00
    
    Recent developments in studies of extragalactic high-energy phenomena 30m
    
    In this talk, I will review recent developments in high-energy extragalactic astrophysics, particularly concerning high-energy particles, including gamma-rays and neutrinos, in supermassive black holes, blazars, gamma-ray bursts, tidal disruption events, and binary neutron star mergers. We have not found a significant correlation between the arrival directions of ultra-high-energy cosmic rays (UHECRs) and any type of astronomical objects yet. On the other hand, interestingly, the significance of neutrino signals from Seyfert galaxies is gradually increasing, and particle acceleration near black hole accretion disks is being seriously considered. It is possible that UHECRs also originate from such unexpected celestial bodies. Reviewing recent observational and theoretical studies for possible high-energy particle sources, I will discuss the particle acceleration mechanism, secondary particle production, and jet dynamics.
    
    Ponente: Katsuaki Asano (ICRR, The University of Tokyo)
    
    KA-Valencia25.pdf
  - 9:30
    
    Recent Results in Cosmic Rays Direct Detection 30m
    
    In recent years, remarkable progresses have been made with the direct detection of cosmic rays in space, reshaping our understanding of the origin, acceleration, and propagation of cosmic rays. This talk will summarize the latest experimental findings, including the matter and antimatter in cosmic rays, the primary and secondary components of cosmic nuclei, isotopic energy spectra, and the temporal variations in cosmic ray flux caused by solar activities. These new phenomena pose challenges to existing cosmic ray theories and also provide an experimental basis for the development of new and comprehensive cosmic ray models.
    
    Ponente: Weiwei Xu (Shandong Institute of Advanced Technology)
    
    TeVPA_CRD_Review.pdf
  - 10:00
    
    Atmospheric Lepton Fluxes 30m
    
    Accurate modeling of cosmic ray spectra and atmospheric lepton fluxes is fundamental to interpreting astrophysical neutrino observations, understanding neutrino oscillations, constraining hadronic interaction models, and enabling applications from new physics searches to muon tomography. This talk presents recent advances in modeling atmospheric muon and neutrino fluxes at multi-GeV to TeV energies. I will discuss the data-driven daemonflux model, a muon-calibrated approach designed to quantify theoretical uncertainties, and review early experimental validation suggesting accurate flux descriptions. Central to this framework is the Global Spline Fit (GSF) model of cosmic ray spectra, recently updated in 2025 to incorporate the latest direct measurements since its 2017 inception. I will present the impact of GSF2025 on current lepton flux predictions and outline the development roadmap for the Matrix Cascade Equations (MCEq) computational framework.
    
    Ponente: Anatoli Fedynitch (Institute of Physics, Academia Sinica)
    
    20251104_TeVPa_Anatoli_pdf.pdf
- 10:30 → 11:00
  
  Coffee Break 30m Dome (Fundación Bancaja)
  
  Dome
  
  Fundación Bancaja
- 11:00 → 12:30
  Plenary Session: IV Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Laura Lopez-Honorez (VUB)
  - 11:00
    
    Gravitational-Wave Astrophysics: From GW150914 to GWTC-4.0 30m
    
    The observation of gravitational waves (GWs) by the LIGO-Virgo-KAGRA (LVK) Collaboration has opened an entirely new window to study the universe. The landmark detection of the first signal in 2015, GW150914, confirmed a century-old prediction of General Relativity, initiating the field of Gravitational-Wave Astronomy. Ten years after this first detection, the LVK Collaboration has published over 300 public alerts across its four observing runs, corresponding to significant detection candidates. In August 2025, the LVK Collaboration published its fourth Gravitational-Wave Transient Catalog, GWTC-4.0. This catalog contains 128 new significant GW candidates, all of them associated with coalescing compact binaries. This talk presents a brief overview of the impact of the LVK detections in astrophysics, discussing, in particular, the most recent results obtained in the first part of the O4 run.
    
    Ponente: José Antonio Font (University of Valencia)
    
    talk-2025-TEVPA.pdf
  - 11:30
    
    Direct dark matter searches: an eclectic overview 30m
    
    With bigger and more sensitive detectors, the direct search for dark matter (DM) has experienced a very exciting transformation in the last years, which is enabling us to test candidates beyond the WIMP paradigm. In this talk I will give an overview of the current status of direct DM searches and future directions. I will address the new opportunities for low-mass candidates, non-standard DM production mechanisms, the Migdal effect and the possibility of testing new neutrino physics with DM detectors.
    
    Ponente: David Cerdeño (IFT UAM/CSIC)
    
    2025-11-TeVPA-Cerdeno_compressed.pdf
  - 12:00
    
    Cosmological dark matter simulations with baryons: recent developments at the smallest, dwarf-galaxy scales 30m
    
    We use state-of-the-art cosmological hydrodynamical simulations of galaxies within a cold dark matter context, to study recent ‘hot topics’ in galaxy formation at the smallest scales: the existence of low-surface-brightness, ultra diffuse galaxies, the emergence of 'dark galaxies' as well as the role of AGN feedback in the evolution of dwarfs. These predictions, together with future observations, will provide critical tests of the ΛCDM model.
    
    Ponente: Arianna Di Cintio (Universidad de La Laguna/ Instituto de Astrofisica de Canarias)
    
    TEVPA_dicintio_2025.pdf
- 12:30 → 14:30
  
  Lunch Break 2h ADEIT
  
  ADEIT
- 14:30 → 16:15
  Cosmic Rays Room 2.1+2.2 (ADEIT)
  
  Room 2.1+2.2
  
  ADEIT
  
  Moderador: Mercedes Paniccia (University of Geneva (CH))
  - 14:30
    
    Latest Results from the Alpha Magnetic Spectrometer on the International Space Station 15m
    
    The Alpha Magnetic Spectrometer (AMS) is a precision particle physics detector operating on the International Space Station. Since 2011, AMS has collected more than 250 billion charged cosmic rays with energies up to multi-TeV. The high-precision measurements with ~1% accuracy have led to many surprising observations. The latest results on cosmic elementary particles (electrons, positrons, antiprotons, and protons) reveal unique properties and indicate new sources of particles and antiparticles. The data on nuclei and isotopes exhibit characteristic energy dependences that are not explained by current theories. The comprehensive AMS data requires a new model of the cosmos.
    
    Ponente: Zhili Weng (Massachusetts Inst. of Technology)
    
    TeVPA-2025_AMS_ZhiliWeng_v4.pdf
  - 14:45
    
    A Decade of CALET Observations: Cosmic-Ray Results from the ISS 15m
    
    The CALorimetric Electron Telescope (CALET) has been in operation on the International Space Station (ISS) since October 2015, providing nearly ten years of high-precision, continuous observations of cosmic rays. The CALET mission aims to search for signatures of nearby sources and dark matter through observations of high-energy cosmic-ray electrons, and to contribute to the study of cosmic-ray acceleration and propagation via precise measurements of nuclei from protons to heavy elements.
    Over nearly a decade of observations, CALET has reported notable spectral features including a spectral break around 1 TeV in the all-electron spectrum, as well as spectral hardening and softening in the TeV region for protons, helium, and heavier nuclei. A preliminary all-particle spectrum extending to the PeV region has also been derived by combining a wide range of nuclei. Precise charge identification enables the measurement of energy spectra of individual elements, contributing to the study of cosmic-ray acceleration and propagation mechanisms. In addition, CALET provides data on the relative abundances of ultra-heavy galactic cosmic rays beyond Z=28. This presentation summarizes the latest CALET results based on nearly ten years of operation, including recent measurements of spectral features and on-orbit detector performance.
    
    Ponente: Yosui Akaike (Waseda University, Japan)
    
    TeVPA2025_akaike.pdf
  - 15:00
    
    Latest results from the DAMPE space mission 15m
    
    The space-based DAMPE (DArk Matter Particle Explorer) detector has been taking data since its successful launch in December 2015. Its main scientific goals include the indirect search for dark matter signatures in the cosmic electron and gamma-ray spectra, the measurements of galactic cosmic ray fluxes from tens of GeV up to hundreds of TeV and high energy gamma ray astronomy above a few GeV. Updated results on all the mission science goals will be given, with particular focus on spectral measurements of single cosmic ray species up to the sub-PeV region.
    
    Ponente: Ivan De Mitri (GSSI and INFN)
    
    DeMitri-DAMPE-TeVPA2025.pdf
  - 15:15
    
    The design, flight and current analysis of HELIX 15m
    
    Measurements of clock isotopes, particularly that of the Be-10/Be-9 ratio, can be used to provide unique information on galactic cosmic ray propagation. The High Energy Light Isotope eXperiment (HELIX) is a balloon-borne magnet spectrometer designed to measure cosmic ray isotopes with an event-by-event mass resolution of 3%. The experiment aims to improve the statistics and extend measurements of beryllium isotopes up to 10 GeV/n. HELIX measures the velocity of incident cosmic rays using time-of-flight scintillators and an aerogel ring-imaging Cherenkov detector. Housed within a 1 Tesla superconducting magnet is a drift chamber tracker, which is used to measure the magnetic rigidity of incident cosmic rays. In the boreal spring of 2024, HELIX underwent a successful engineering flight from Sweden, landing just over six days later in Northern Canada from where it was safely recovered. We will discuss the design of the payload, an overview of its first engineering flight, and the current analysis and refurbishment efforts.
    
    Ponente: Conor McGrath (Queen's University)
    
    HELIXTeVPa-6.pdf
  - 15:30
    
    Ultra-Heavy Galactic Cosmic Ray Measurements with TIGERs 15m
    
    The Trans-Iron Galactic Element Recorder (TIGER) family of instruments are designed to make the best single-element resolution measurements of the Ultra-Heavy Galactic Cosmic Rays (UHGCRs) to probe their origins and the sources of nucleosynthesis. The TIGER and SuperTIGER stratospheric long-duration balloon-borne detectors have each had two successful flights from Antarctica, with TIGER making preliminary cosmic-ray (CR) abundance measurements through $_{40}$Zr and SuperTIGER through $_{56}$Ba. Maximizing exposure is critical for observing the very rare UHGCR, which these balloon missions achieved with extended flight time and by flying the largest detector area possible. The successor to these instruments will be the TIGER for the International Space Station (TIGERISS), a NASA Astrophysics Pioneers mission with a planned 2027 launch. TIGERISS will measure the abundances of individual CR elements from $_{5}$B to $_{82}$Pb with unprecedented charge resolution and detector linearity, improving on its predecessors by using silicon strip detectors (SSDs) in place of scintillator detectors for ionization energy measurements and using silicon photomultipliers instead of photomultiplier tubes for lower-voltage and more compact read out of the acrylic and silica aerogel Cherenkov-light-radiator detectors. The superior resolution of the SSDs over the scintillator detectors has been demonstrated in component accelerator tests at CERN, allowing TIGERISS to identify UHGCR nuclei with charge resolution $\sigma_{Z}$ < 0.25. UHGCR observations cover those synthesized in stellar fusion and in s-process and r-process neutron capture nucleosynthesis, which will add to the multi-messenger effort to answer the question of the degree that r-process elements are synthesized in supernovae or neutron star merger events.
    
    Ponente: Brian Rauch (Washington University in St. Louis)
    
    Rauch_TeVPA2025_TIGER.pdf Rauch_TeVPA2025_TIGER.pptx
  - 15:45
    
    Anisotropy of Cosmic Elementary particles measured with the Alpha Magnetic Spectrometer on the ISS 15m
    
    Analysis of anisotropy of the arrival directions of galactic positrons, electrons and protons has been performed with the Alpha Magnetic Spectrometer on the International Space Station. This measurement allows to differentiate between point-like and diffuse sources of cosmic rays for the understanding of the origin of high energy positrons or the hardening in the proton flux. The AMS results of the dipole anisotropy are presented along with the discussion of the implications of these measurements.
    
    Ponente: Iñaki Rodríguez García (Centro de Investigaciones Energéticas Medioambientales y Tecnológicas)
    
    TalkTeVPA2025_InakiRodriguez.pdf
  - 16:00
    
    Antiprotons and Elementary Particles over a Solar Cycle: Results from the Alpha Magnetic Spectrometer 15m
    
    We present results over an 11-year Solar cycle of cosmic antiprotons in the rigidity range from 1.00 to 41.9 GV. The antiproton fluxes exhibit distinct properties. Compared with other cosmic elementary particle fluxes (proton, electron, and positron), the magnitude of the antiproton flux temporal variation is significantly smaller. A hysteresis between the antiproton fluxes and the proton fluxes is observed, whereas the antiproton and electron fluxes show a linear correlation. With a model-independent analysis, we found a universal relation between the shape of the rigidity spectrum and the magnitude of flux temporal variation over an 11-year Solar cycle for both positively and negatively charged particles. The simultaneous results on antiproton, proton, electron and positron provide unique information for understanding particle transport in the Solar System as a function of mass, charge, and spectral shape.
    
    Ponente: Hsin-Yi Chou (Institute of Physics, Academia Sinica, Taiwan)
    
    TeVPA_pbar_HYChou_v3.pdf
- 14:30 → 16:15
  Cosmology Salón de Grados (ADEIT)
  
  Salón de Grados
  
  ADEIT
  
  Moderador: Ali Rida Khalife (IAP-CNRS and Sorbonne University)
  - 14:30
    
    Invited Talk: Cosmology from the CMB with ACT DR6 15m
    
    We present power spectra of the cosmic microwave background (CMB) anisotropy in temperature and polarization, and the most recent constraints on cosmology from these, as measured from the Data Release 6 (DR6) of the Atacama Cosmology Telescope (ACT) data. ACT DR6 measures the CMB power spectra over a quarter of the sky in multiple bands in both temperature and polarization with arcminute resolution. We find that the ACT angular power spectra are well fit by the sum of CMB and foregrounds, where the CMB spectra are described by the ΛCDM model. Combining ACT with larger-scale Planck data, the joint P-ACT dataset provides tight limits on the ingredients, expansion rate, and initial conditions of the universe. We find similar constraining power, and consistent results, from either the Planck power spectra or from ACT combined with WMAP data, as well as from either temperature or polarization in the joint P-ACT dataset. We use these new cosmic microwave background measurements to test foundational assumptions of the standard cosmological model, ΛCDM, and set constraints on extensions to it. We derive constraints from the ACT DR6 power spectra alone, as well as in combination with legacy data from the Planck mission, measurements of the CMB lensing from ACT and Planck, baryon acoustic oscillation measurements, and supernovae data. Together, these measurements provide the newest, tightest constraints on the ΛCDM model and a broad range of extensions.
    
    Ponente: Hidde Jense (Cardiff University)
    
    HTJense_TeVPa_251104.pdf
  - 14:45
    
    Boosting 21-cm constraints on Dark Matter 15m
    
    The 21-cm signal is emerging as a promising probe of dark matter. However, heating-based constraints are strongly affected by astrophysical uncertainties entering in the choice of fiducial model. I will illustrate this effect for accreting primordial black holes with masses in the range $1-10^3 \, M_{\odot}$. To address this issue, I will then introduce a novel mechanism in which dark matter can boost the 21-cm signal through exotic Lyman-$\alpha$ photons, potentially offering a more robust avenue for constraining dark matter.
    
    Ponente: Dominic Agius (IFIC, CSIC-UV)
    
    TeVPA_Agius.pdf
  - 15:00
    
    Cosmological bounds on ALPs from strings 15m
    
    Axion-like particles (ALPs), radiated from a network of cosmic strings, may be a large part of Dark Matter (DM). In the era of precision cosmology, it is possible to characterize the effect of such particles - which almost scale invariant distribution function spans many orders of magnitudes in momentum - on the observables. In this work, we employ the CLASS code and cosmological data to place bounds on the abundance and on other distinctive parameters of ALPs from strings. We focus on the mass range $10^{-20} -10^{-15} $ eV, and we find the strongest constraint on the ALP decay constant $f_a$ if the ALP mass is between $10^{-20}-10^{-18}$ eV, where we are able to improve the overabundance of DM bound on $f_a$ by more than a factor of 3. As a result, ALPs from strings cannot account for more than one-tenth of DM at three sigma if $m_a $ is between $10^{-20}- 10^{-18}$ eV.
    
    Ponente: Riccardo Impavido (Università di Ferrara, INFN Ferrara)
    
    tevpav2.pdf
  - 15:15
    
    A "Global" Solution to the Cosmological Monopole Problem 15m
    
    Magnetic monopoles are a long-sought prediction of Grand Unified Theories (GUTs), yet their efficient production in the early universe would lead to a monopole abundance that far exceeds observational limits—a challenge known as the cosmological monopole problem. The standard resolution invokes inflation occurring after monopole production, diluting their density to undetectable levels and eliminating any possibility of present-day observation. In this talk, we propose an alternative solution based on a minimal breaking of conformal symmetry in the gauge kinetic sector, effective in the early universe before BBN. This mechanism enhances monopole annihilation, thereby reducing their abundance to acceptable levels without requiring inflation. This scenario predicts a residual monopole flux potentially within the sensitivity of current and upcoming cosmic ray detectors, opening new avenues for their discovery.
    
    Ponente: Daniele Perri (University of Warsaw)
    
    Valencia_TeVPA_Perri.pdf
  - 15:30
    
    Dark energy and neutrinos along the cosmic expansion history 15m
    
    In this work, we employ a model-independent approach to jointly reconstruct the dark energy equation of state $w_\mathrm{DE}$ and the sum of neutrino masses $\sum m_\nu$.
    We adopt the Piecewise Cubic Hermite Interpolating Polynomial (PCHIP) method with five fixed nodes in which we allow $w_\mathrm{DE}$ and $\sum m_\nu$ to vary. We employ CMB, BAO and SN data to constrain the values of $w_\mathrm{DE}$ and $\sum m_\nu$ at each node.
    To gain a full understanding of the degeneracy between dark energy and neutrinos, we conduct three different analysis: one in which we only reconstruct $w_\mathrm{DE}$, fixing the sum of neutrino masses to 0.06 eV; one in which we reconstruct $w_\mathrm{DE}$ and we allow $\sum m_\nu$ to vary; finally, one in which we reconstruct both $w_\mathrm{DE}$ and $\sum m_\nu$ using the PCHIP method.
    
    Ponente: Pietro Ghedini (IFIC, CSIC-UV)
    
    Ghedini_TeVPA.pdf
  - 15:45
    
    Generic isocurvature fluctuations of scalar spectators 15m
    
    Light scalar fields acquire isocurvature fluctuations during inflation. While these fluctuations could lead to interesting observable signatures at small scales, they are strongly constrained on large scales by cosmic microwave background (CMB) observations. When the mass of the scalar is much lighter than the inflationary Hubble scale, $m\ll H_I$, the spectrum of these fluctuations is flat. Meanwhile, if $m\gg H_I$, the fluctuations are suppressed. A blue-tilted isocurvature spectrum which exhibits enhanced structure on small scales but avoids observational constraints on large scales therefore requires a coincidence of scales $m\sim H_I$ for a free massive scalar. In this talk, I will show that if a scalar field possesses a nontrivial potential, its inflationary dynamics naturally cause this condition to be satisfied, and so a blue-tilted spectrum is generically expected for a large class of potentials. Specifically, if its potential $V$ exhibits a region which satisfies the slow-roll condition $V''< H_I^2$ the scalar will spend most of inflation close to the boundary of this region, so that its effective mass is typically close to $H_I$. Depending on the length of inflation, this can generically lead to an isocurvature spectrum with an $\mathcal O(0.1)$ blue tilt, regardless of the initial inflationary conditions of the scalar or its final mass in the late universe. If the scalar is long-lived, this mechanism leads to an attractor prediction for its relic abundance. In particular, a scalar field with quartic self-interactions can achieve the correct abundance to constitute all of the dark matter for a wide range of masses, while avoiding isocurvature constraints and exhibiting enhanced structure on small scales.
    
    Ponente: Saarik Kalia (IFAE Barcelona)
    
    tevpatalk.pdf tevpatalk.pptx
  - 16:00
    
    Fitting the DESI BAO Data with Dark Energy Driven by the Cohen–Kaplan–Nelson Bound 15m
    
    Motivated by the work of Cohen, Kaplan and Nelson (CKN) in which the authors argue that gravity restricts the range of validity of a QFT, we consider a time-dependent dark energy density, scaling proportional to the squared Hubble parameter $H(z)$.
    These models are of particular interest in the light of the recent data release of the DESI collaboration, since the measurements show an increasing preference for time-depending dark energy models in comparison to the $\Lambda$CDM model.
    In our work, we compare the generalized CKN models to DESI BAO,
    supernova datasets and model-independent Hubble measurements and find a
    preference of up to $2.6\,\sigma$ over the $\Lambda$CDM model.
    
    Ponente: Patrick Adolf
    
    TeVPA_PA.pdf
- 14:30 → 16:15
  Dark Matter: Direct Detection Room 3.1+3.2 (ADEIT)
  
  Room 3.1+3.2
  
  ADEIT
  
  Moderador: Karoline Schäffner (Max-Planck Institute for Physics)
  - 14:30
    
    The SuperCDMS experiment at SNOLAB 15m
    
    The SuperCDMS SNOLAB experiment is an upcoming direct detection dark matter experiment using semiconductor crystal detectors operated at cryogenic temperatures. The experiment is located 2 km underground in the Creighton mine at Sudbury, Canada. With low background from cosmic sources, SNOLAB is ideal for rare event searches. The experiment uses 24 detectors, made of silicon and germanium, comprising of two detector types: one with phonon channels that is operated at high voltage (∼100 V), utilizing the Neganov-Trofimov-Luke (NTL) effect to amplify the phonon signal and achieve a low energy threshold, and another with phonon and charge sensors that enables effective background rejection. The experiment will probe low-mass WIMPs, dark photon absorption, and Axion-Like Particles. The commissioning phase is underway later this year, and science data-taking is expected to begin by mid-2026. This talk gives an overview of the experiment, its science goals, and a status update of the experiment at SNOLAB.
    
    Ponente: Sukeerthi Dharani (University of British Columbia)
    
    The SuperCDMS Experiment_at_SNOLAB _ TeVPA_SDharani.pdf
  - 14:45
    
    The TESSERACT Low Mass DM Experiment 15m
    
    The TESSERACT experiment, a novel and fully funded new type of low-mass DM experiment, is achieving new sensitivities in the search for sub-GeV dark matter. We're deploying multiple complementary targets read out via ultra-sensitive TES-based athermal phonon detectors Each detector is uniquely tailored to detect nuclear-, electron-, and dark photon-type dark matter interactions. By using different targets such as liquid helium (HeRALD) and the polar crystals GaAs and Sapphire (SPICE), and ensuring identical readout and experimental settings across all detectors, TESSERACT will achieve both, unparalleled sensitivity and a the capability to identify and discriminate against novel backgrounds. While full operations will begin at the Modane underground laboratory in 2029, we've already performed first dark matter searches on the surface, achieving leading low-mass sensitivities. We will present the current status of the experiments and sensors, discuss new insights into the "low energy excess background," and highlight the first sensitivities obtained from our surface background runs.
    
    Ponente: Bjoern Penning (University of Zurich)
    
    TEVPA_Penning_2025.pdf
  - 15:00
    
    DELight: Direct search Experiment for Light Dark Matter with superfluid helium 15m
    
    Tonne-scale noble liquid detectors have set strong limits on Dark Matter (DM) candidates particularly above a few GeV/c², while the parameter space for Light Dark Matter (LDM) remains largely unexplored. A sub-keV energy threshold and large exposures are essential to tackle this challenge. Solid state detectors can achieve energy thresholds in the order of 1 eV, but their relatively small masses and complicated scalability limit the possible exposure. The “Direct search Experiment for Light dark matter” (DELight) aims to overcome these challenges by employing a superfluid helium-4 target instrumented with Large Area Microcalorimeters (LAMCALs), based on Magnetic MicroCalorimeter (MMC) technology. Superfluid helium offers a more easily scalable target with low nuclear mass, ideal for LDM searches. It also provides both photon and quasiparticle signals, allowing for the discrimination of the interaction types, further reducing the background. The LAMCALs achieve the energy resolution needed to reach the 20 eV threshold in the phase-I of DELight. With an exposure of just 1 kg·day, DELight will probe new regions of the parameter space during phase-I, achieving sensitivities below 10⁻³⁹ cm² at a DM mass of 200 MeV/c².
    We will present the working principle of the DELight experiment and an overview of the latest progress towards its realization.
    
    Ponente: Francesco Toschi (Kirchhoff-Institut für Physik, Heidelberg University)
    
    Toschi_DELight_TeVPA_04112025.pdf
  - 15:15
    
    ANAIS-112 six-year results in the search for annual modulation and future prospects 15m
    
    The ANAIS (Annual modulation with NaI(Tl) Scintillators) experiment is intended to search for dark matter annual modulation with ultrapure NaI(Tl) scintillators in order to provide a model independent confirmation or refutation of the long-standing DAMA/LIBRA positive annual modulation signal in the low energy detection rate, using the same target and technique. Other experiments exclude the region of parameters singled out by DAMA/LIBRA. However, these experiments use different target materials, so the comparison of their results depends on the models assumed for the dark matter particle and its velocity distribution in the galactic halo. ANAIS-112, consisting of nine 12.5 kg NaI(Tl) modules produced by Alpha Spectra Inc., disposed in a 3×3 matrix configuration, is taking data smoothly with excellent performance at the Canfranc Underground Laboratory, Spain, since August 2017, accumulating over 800 kg·yr of exposure. In this talk, I will present the six-year results from ANAIS-112, which lead the international, model-independent effort to test the DAMA/LIBRA signal, and are compatible with the absence of modulation and incompatible with DAMA/LIBRA for a sensitivity above 4σ, with the potential to reach 5σ level by the end of 2025. Systematics affecting the comparison will also be reviewed, particularly those related to the response of detectors to nuclear recoils.
    
    Ponente: Iván Coarasa Casas (CAPA - Universidad de Zaragoza)
    
    TeVPA2025_ANAIS_IvanCoarasa.pdf
  - 15:30
    
    The SABRE South Experiment at the Stawell Underground Physics Laboratory 15m
    
    SABRE is an international collaboration that will operate similar particle de-
    tectors in the Northern (SABRE North) and Southern Hemispheres (SABRE
    South). This innovative approach distinguishes possible dark matter signals
    from seasonal backgrounds, a pioneering strategy only possible with a southern
    hemisphere experiment. SABRE South is located at the Stawell Underground
    Physics Laboratory (SUPL), in regional Victoria, Australia.
    SUPL is a newly built facility located 1024 m underground (∼2900 m water
    equivalent) within the Stawell Gold Mine and its construction has been com-
    pleted in 2023.
    SABRE South employs ultra-high purity NaI(Tl) crystals immersed in a Linear
    Alkyl Benzene (LAB) based liquid scintillator veto, enveloped by passive steel
    and polyethylene shielding alongside a plastic scintillator muon veto. Signifi-
    cant progress has been made in the procurement, testing, and preparation of
    equipment for installation of SABRE South. The SABRE South muon detector
    and the data acquisition systems are actively collecting data at SUPL and the
    SABRE South’s commissioning is planned to be completed by the end of 2025.
    This presentation will provide an update on the overall progress of the SABRE
    South construction, its anticipated performance, and its potential physics reach.
    
    Ponente: Kyle Leaver (The University of Adelaide & ARC Centre of Excellence for Dark Matter and Particle Physics)
    
    TeVPA_2025_Kyle_Leaver.pdf
  - 15:45
    
    Status of the COSINUS Experiment at Gran Sasso 15m
    
    By employing high-purity NaI as a cryogenic bolometer target material, the upcoming COSINUS experiment aims at providing a definitive crosscheck of the DAMA/LIBRA dark matter claim within the next few years. This approach is made possible through the dedicated „remoTES" detector design, which allows to readout the NaI crystal using a transition edge sensor without exposing it to fabrication processes. In combination, with ultrathin Si beaker light detectors, COSINUS modules provide event-by-event particle identification and low nuclear recoil detection thresholds on the order of few keV. Construction of the COSINUS facility at Laboratori Nazionali del Gran Sasso is finished, and commissioning of the setup is ongoing, while the final detector design is being prepared. This contribution will give an overview on the characteristics and features of the new COSINUS facility, which includes a modern, „dry“ dilution refrigeration cryostat, specialized vibration decoupling solutions, and a dedicated water cherenkov muon veto system. The ongoing R&D efforts for COSINUS detectors will be presented, with an outlook to possible future applications of the readout concept.
    
    Ponente: Martin Stahlberg (Max Planck Institute for Physics)
    
    cosinus_status_2025_tevpa_mstahlb.pdf
  - 16:00
    
    Development of superfluid He-3 bolometry for the QUEST-DMC project using nanowires with SQUID readout 15m
    
    Superfluid helium-3 bolometers can exploit the extremely low superfluid gap ($10^{-7}$ eV) to give ultra-low energy threshold dark matter direct detection searches. These can probe dark matter models with sub-GeV/c$^2$ masses, in particular offering world-leading sensitivity to spin-dependent interactions. Realising this requires operation at ultra-low temperatures in the 100s μK regime, where helium-3 in the B phase has extremely low specific heat, coupled with low noise detector readout.
    
    The detection scheme for the QUEST-DMC programme is based on the measurement of quasiparticle density in superfluid helium-3, using novel vibrating wire resonators with sub-micron diameter and SQUID readout [1]. We demonstrate resonator characterisation and bolometry, including non-linear operation. Energy calibration using direct heat injection from a second vibrating wire has been carried out and a gamma radiation source has been installed for complimentary calibration. Noise performance and the resultant energy resolution of the bolometer will be discussed. The measured bolometer energy spectrum will be compared to Monte Carlo simulations of the cosmic ray and radiogenic backgrounds incident on the helium-3 bolometer.
    
    [1] S. Autti et al. European Physical Journal C 84, 248 (2024).
    
    Ponente: Elizabeth Leason
    
    TeVPA25_QUEST_ELeason.pdf
- 14:30 → 16:15
  Gamma Rays: Extragalactic Salón de Actos (ADEIT)
  
  Salón de Actos
  
  ADEIT
  
  Moderador: Mireia Nievas Rosillo (Instituto de Astrofisica de Canarias (IAC))
  - 14:30
    
    Bridging Gravitational Waves and High-Energy Gamma Rays: Searching for sGRB Afterglows from Compact Binary Coalescences with CTAO 15m
    
    A complete understanding of compact binary coalescences requires combining gravitational wave (GW) observations with broadband electromagnetic data. The detection of GeV-TeV gamma rays will be crucial for probing the acceleration processes and environments near compact object mergers. The binary neutron star (BNS) merger GW170817 provided the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (sGRBs) with the detection of its electromagnetic counterpart. We present our approach to establish the prospects on binary neutron star (BNS) mergers that emit GeV-TeV gamma rays and are detectable by the Cherenkov Telescope Array Observatory (CTAO). With its unparalleled sensitivity, broad energy coverage (20 GeV - 300 TeV), and rapid slewing capabilities, CTAO is uniquely positioned to play a key role in these searches. Using simulations of CTAO’s response to phenomenological models describing sGRB afterglows associated with GW events, we address the challenge of large source localization uncertainties through a real-time strategy designed to coordinate searches over vast sky regions. We optimize potential multi-site follow-up strategies and provide an estimate of the number of joint sGRB-GW events from BNS mergers that CTAO could detect during future LIGO-Virgo-KAGRA (LVK) observing run O5. In addition, our study aims to maximize the scientific return of CTAO observations by examining how key physical parameters—such as jet opening angle, luminosity, distance, and off-axis viewing angle—change the gamma-ray emission and the detection prospects.
    
    Ponente: Mónica Seglar-Arroyo (IFAE)
    
    GW_CTAO_MSA_vF1.pdf
  - 14:45
    
    Follow-up of LVK O4 Gravitational Wave events with MAGIC and LST-1: Constraints on GW VHE Gamma-Ray Counterparts 15m
    
    We present gamma-ray observations by Major Atmospheric Gamma-Ray Imaging Cherenkov Telescope (MAGIC) and Large Sized Telescope (LST-1) of two of the most compelling gravitational-wave events detected by LIGO-Virgo-KAGRA (LVK) during Observing Run 4 (O4b). Conducted with MAGIC and LST-1 in a multi-telescope configuration, the campaign enabled a sensitive search for very-high-energy counterparts. The results constrain gamma-ray emission models for Binary Black Hole (BBH) mergers, such as super-Eddington accretion and post-merger jets, and demonstrate the capability of current Imaging Atmospheric Cherenkov Telescopes (IACTs) to contribute to multi-messenger astronomy.
    
    The first source, S240615dg, currently the best-localized event of O4, was observed 15 hours after the alert under challenging conditions due to observations taken at high zenith angles and elevated Night Sky Background (NSB). A hybrid analysis approach was applied, deriving upper limits (ULs) that fully cover the source location (>99% C.R), with LST-1 helping to lower the energy threshold down to 0.15 TeV.
    
    The second source, S241125n, presented a special scenario given the X-ray counterpart candidate detected by Swift/GUANO. Observations began 19 hours after the BBH merger reported by LVK, targeting the reported X-ray position. Due to suboptimal weather, LIDAR-based atmospheric corrections and dedicated Monte Carlo simulations incorporating the cloud profile were used. The results place constraints on gamma-ray emission from the X-ray counterpart above 0.6 TeV.
    
    Ponente: Juan Jiménez Quiles (IFAE)
    
    20251104_bbh_analysis_lst_magic_v2.pdf
  - 15:00
    
    Detection of TeV emission from poorly localized GRBs with ground based IACTs, and future perspective in the era of CTAO 15m
    
    The prompt and early afterglow phases of gamma-ray bursts (GRBs) remain elusive, especially in the very-high-energy (VHE, E > 100 GeV) domain. While space-based instruments like Fermi/LAT have extended our view of GRB emission up to 100 GeV, the detection of the early TeV emission from GRBs remains challenging. Limitations including poor sky localization from Fermi/GBM detected GRBs, observational latency due to issuing, receiving, handling the alerts and repointing of telescopes to the GRB location,, and absorption by extragalactic background light significantly challenge the detection of the early-time VHE observations. In this talk, I will present observational strategies to enhance the detectability of TeV emission from GRBs in the context of current operating IACTs such as the MAGIC telescopes and CTAO/LST. In order to provide a realistic observation and detection prospects in the TeV band, we simulated a realistic long-GRB population typically detectable by Fermi/GBM in a year. Based on our knowledge of GRBs observations obtained during the 16 years of operation of Fermi/GBM and 20 years of Swift/XRT detections, we assign realistic fluence, isotropic equivalent energy in prompt (EISO), GBM localization, redshift, X-ray flux, and XRT-localization. I will discuss the relevant emission model of early afterglow that successfully predicts the X-ray emission and correlated X-ray and intrinsic VHE emission, used to simulate GRB emission above GeV energies. We test the detectability of the source, discuss the optimization of the tilling strategy of IACTs given the simulated GRB populations with GBM localization and the probability of pinpointing the source, thanks to the simulated XRT position. I will present the expected rates of VHE detections, which can be useful for future observational strategies aimed to increase the number of TeV GRBs.
    
    Ponente: Samanta Macera (GSSI)
    
    TeVPA_Samanta_Macera.pdf
  - 15:15
    
    Observation and characterization of the second spectral component in GRB 221009A 15m
    
    Gamma-ray bursts (GRBs) of long duration arise from ultra-relativistic jets that appear shortly after the collapse of massive stars. The highly variable prompt emission, lasting only a few minutes, results from internal dissipation within the jet and is followed by an afterglow that can last several days. This afterglow emission, observable at energies ranging from radio to TeV, is primarily generated by synchrotron and synchrotron self-Compton processes. Despite this, identifying a distinct prompt or early spectral component in GeV-TeV energies has been challenging because of the sensitivity constraints in the MeV-GeV range. This presentation will address the GeV-TeV spectral component of GRB 221009A, the brightest of all-time (BOAT) GRB, as observed in the initial 20 minutes. By modeling the GeV data observed simultaneously by Fermi/LAT from the early phase and AGILE in the later phase, with the TeV data from LHAASO, we can put limits on the magnetic fields and electron energies in the relativistic shock. Although prompt and early very high-energy gamma ray (VHE; E>100 GeV) emissions are crucial to understanding the emission mechanism, it remains understudied due to limitations such as the shorter duration of GRBs, delays between distribution of the triggers from the MeV instruments and notifications received by VHE pointing telescopes, and the slew-time of these telescopes. I will also discuss a novel observation strategy for the pointing VHE facilities (MAGIC, CTAO/LST) to capture prompt and early VHE emissions. This new method has been suggested for MAGIC telescopes, which includes rapid follow-up of the Fermi/GBM triggers to scan the sky localization with shorter exposures (subminute timescale) to cover sky localization of about 100 sq. deg.
    
    Ponente: Biswajit Banerjee (Gran Sasso Science Institute (GSSI))
    
    TeVPA_Banerjee.pdf
  - 15:30
    
    Emission from Gamma-Ray Bursts at Very High Energy : Insights from 15 Years of H.E.S.S. Observations 15m
    
    The detection of Gamma-Ray Bursts (GRBs) at Very High Energy (E > 100 GeV) was a long-awaited result, and many observations were needed before achieving this goal. The study presented here is based on a complete re-analysis of 15 years of GRB observations with the High-Energy Stereoscopic System (H.E.S.S.) providing the most extensive set of VHE upper limits to date.
    
    This study contributes to the better understanding of the VHE emission of GRBs by showing that GRBs detected at VHE are not a distinct population but are bright events at low redshifts. For the most interesting events in our sample, we modeled the afterglow emission, combining the H.E.S.S. limits with publicly available multi-wavelength data to discuss the obtained microphysical parameters.
    
    These results place existing VHE detections into perspective and give insight on the ability of the Cherenkov Telescope Array Observatory (CTAO) to detect fainter and high-redshift GRBs at VHE.
    
    Ponente: Mathieu de Bony de Lavergne (CPPM, IN2P3, CNRS)
    
    tevpa_2025_hess_grb_catalog.pdf
  - 15:45
    
    Testing the ubiquitous presence of very high energy emission in gamma-ray bursts with the MAGIC telescopes 15m
    
    Gamma-ray bursts (GRBs) are among the most powerful transients in the Universe and a key science target for the MAGIC Collaboration. Despite the observational challenges inherent to Imaging Atmospheric Cherenkov Telescopes (IACTs), MAGIC has implemented a dedicated strategy for rapid follow-up of GRBs, enabling observations at a rate of ~10 GRBs per year since 2013. While two GRBs have been successfully detected at very high energies (VHE, E > 100 GeV), the majority remain undetected. We present the systematic analysis of 42 non-detected GRBs observed by MAGIC from 2013 to 2019. We derive upper limits on observed energy fluxes and on energy fluxes corrected for the effect of the extragalactic background light (EBL) investigating possible reasons for these non-detections, including the possible peculiar properties of TeV-detected GRBs. Our study highlights the critical role of EBL absorption in limiting VHE detections. For a subset of nearby GRBs (z < 2), we compare the VHE upper limits with contemporaneous X-ray fluxes and find that a VHE component with comparable luminosity to the X-rays cannot be excluded. These results provide new constraints on the presence and properties of VHE emission in GRBs and inform future observational strategies with current and next-generation of IACTs.
    
    Ponente: Davide Miceli (INFN Padova)
    
    MAGIC_UL_TeVPA.pdf
  - 16:00
    
    Characterization of early X-ray emission of Swift/XRT detected short-GRBs and multi-messenger perspective 15m
    
    Accurate modeling of the early X-ray emission in short GRBs is essential for probing the GRB engine, understanding jet physics, and improving electromagnetic follow-up of gravitational wave signals from binary neutron star mergers in the context of multi-messenger astronomy.
    Thanks to the operation of the Swift satellite over the last 20 years, we now have access to an extensive archive of GRB X-ray observations. The early X-ray light curves often present a bright and steep decay phase, whose physical origin remains poorly understood. In short GRBs, this phase is particularly prominent, as their fainter forward-shock emission, resulting from lower energy release and a less dense circumburst environment compared to long GRBs, makes the steep decay easier to detect. Short GRBs thus offer a unique opportunity to monitor the steep decline for an extended duration, up to 15 minutes.
    In this talk, I will present our systematic analysis of the early X-ray emission of short GRBs, including both the temporal and spectral evolution. We introduce a new modeling technique that accounts for both the curvature and the intrinsic evolution of the GRB spectrum in Swift/XRT data. For the first time, we fit the synchrotron emission model to the GRB spectra during the steep decay phase, enabling us to track the evolution of the synchrotron cooling frequency and the bolometric flux. Our study reveals a tight correlation between the synchrotron cooling frequency and the isotropic equivalent luminosity. This relation enables us to infer the intrinsic properties of short GRBs and assess the detectability of their early X-ray emission by wide-field X-ray cameras. In particular, our work can help to interpret the nature of some fast X-ray transients detected by Einstein Probe and suggest observational multi-messenger strategies.
    
    Ponente: Annarita Ierardi (Gran Sasso Science Institute)
    
    Annarita_TeVPA.pdf
- 14:30 → 16:15
  Neutrinos: Searches for extragalactic sources Room 1.1+1.2 (ADEIT)
  
  Room 1.1+1.2
  
  ADEIT
  
  Moderador: Aya Ishihara (ICEHAP, Chiba University)
  - 14:30
    
    IceCube all-sky neutrino source searches using combined tracks and cascades datasets 15m
    
    The IceCube Collaboration employs two primary detection channels: tracks and cascades. Point source searches with tracks, with their good angular resolution, are particularly sensitive to sources in the northern sky, while searches with cascades offer enhanced energy resolution and are more effective in the southern sky. Historically, high-energy neutrino point-source searches using IceCube data have relied on only one of these channels at a time. This analysis marks a significant advancement, being the first to combine both IceCube’s tracks and cascades datasets by constructing a unified maximum-likelihood framework that accounts for differences in signal and background distributions, energy resolutions, and event topologies across both datasets. Combining tracks and cascades improves sensitivity across the entire sky and, since both components are all-sky datasets, adds information where one channel alone is limited. The results of our all-sky point-source search combining 14 years of track data and 10 years of cascade data, the most sensitive all-sky search to date, will be presented.
    
    Ponente: Riya Shah (Drexel University, IceCube Collaboration)
    
    2025-11-012-TeVPA-2025-Shah.pdf
  - 14:45
    
    Search for High-Energy Neutrinos from Infrared Flares with IceCube archival data 15m
    
    IceCube has detected a diffuse flux of high energy neutrinos, with two significant observations of extragalactic sources identified to-date being the accreting supermassive black holes (SMBHs) TXS0506+056 and NGC1068. This suggests that other SMBHs may also contribute to the observed neutrino flux. It is possible that some fraction of the IceCube neutrinos originate in time-variable SMBH accretion events. External studies that made use of IceCube data identified candidate sources which include AT2019dsg, which is likely a stellar tidal disruption event (TDE), and AT2019dfr, an AGN flare. Both of these transients exhibit strong dust echoes, characterized by delayed infrared (IR) emission relative to the initial optical outburst. This emission can be interpreted as the reprocessing of X-rays to optical light of the flare by dust located in a torus around the SMBH. An additional study using an optically detected sample of 63 accretion flares revealed another candidate as a potential high-energy neutrino counterpart: AT2019aalc, which is also accompanied by a dust echo. However, follow-up stacking analysis of the 63 nuclear flares using the full IceCube data sample did not show any significant excess over background. Motivated by these three suggested neutrino-TDE correlations, we analyze a more extensive catalog of IR flares, 823 dust-echo-like flares identified using WISE satellite data, against the IceCube 10-year sample of track events from the Northern Sky to assess the potential detectability of neutrino emission from these types of accretion flares.
    
    Ponente: Teresa Pernice (DESY)
    
    Pernice_flaires_TeVPA.pdf
  - 15:00
    
    Bright blazar flares and their lagging neutrino counterparts 15m
    
    In 2017, the IceCube observatory associated (at a significance level of 3σ) a high-energy (HE, E ≥ 100 TeV) muon neutrino temporarily and spatially coinciding with an electromagnetic flare in blazar TXS 0506+056. Since then, no individual blazar-neutrino association at the same level of significance has been made. In November 2010, flat-spectrum radio quasar (FSRQ) 3C 454.3 had an exceptionally bright gamma-ray flare (~100 times brighter than the flare of TXS 0506+056), which made it the brightest object in the gamma-ray sky seen by Fermi-LAT. We analyse the rich set of then-collected multiwavelength data from 3C 454.3 by various telescopes (from optical to gamma-ray band) and model the observable electromagnetic and neutrino emission from 3C 454.3, enquiring what level of neutrino flux we could expect from such a flare. Utilising the Fermi-LAT light curves from the light curve repository and extrapolating the model of 3C 454.3 to all Fermi-LAT FSRQs we show that they can contribute to the HE astrophysical neutrino flux only at a level of $\sim 0.5$%, explaining the rarity of events such as the one from TXS 0506+056. We note also that the energy-loss and acceleration timescale of protons responsible for the production of HE neutrinos may be up to $\sim10^{3}$ times slower than the characteristic timescales of leptonic processes responsible for the electromagnetic flares. This may cause a substantial months-to-years delay of blazar-associated neutrino emission with respect to the major blazar flares. We present the results of our first search for this lagging blazar emission, cross-matching Fermi-LAT light curves with the IceCat-1 catalogue of HE neutrinos.
    
    Ponente: Egor Podlesnyi (Norwegian University of Science and Technology (NTNU))
    
    Podlesnyi and Oikonomou TeVPA 2025.pdf
  - 15:15
    
    Evidence of Neutrino Emission from Southern Sky X-ray Bright Seyfert Galaxies with IceCube 15m
    
    The IceCube Neutrino Observatory has detected TeV-scale neutrinos from NGC 1068, supporting the hypothesis that active galactic nuclei (AGN) may host high-energy neutrino production in obscured environments. Motivated by this, we investigate a catalog of intrinsically X-ray bright Seyfert galaxies in the Southern sky using a coronal model, which suggests cosmic-ray acceleration and hadronic interactions occur in the hot corona near the AGN engine. The coronal model links intrinsic X-ray and neutrino luminosities, providing a physically motivated spectral shape to guide source selection and provide stacking weights, which improves the discovery potential of our search. We use starting track events (ESTES) in our studies of the Southern sky. Some of our candidate neutrino sources, though extragalactic, lie near the Galactic plane in projection, challenging the analysis with significant background contamination. In this contribution, we present our background estimation methods developed for this region and show the evidence for collective neutrino emission from our selected sources. We also compare and discuss the search results of using the coronal model and using the generic power-law assumption.
    
    Ponente: Shiqi Yu (University of Utah)
    
    TeVPA25_ Southern sky seyfert galaxies (1).pdf
  - 15:30
    
    IceCube observations of northern Seyfert galaxies and implications for the extragalactic neutrino flux 15m
    
    Although the existence of a flux of high energy neutrinos emitted by extragalactic sources is well established, only two individual sources have been identified with high confidence: the blazar TXS 0506+056 and the Seyfert galaxy NGC 1068. We will review the results of observations of other Seyfert galaxies in the northern sky, and discuss the implications of both northern and southern observations for our understanding of the extragalactic neutrino flux. Although the observations do not line up perfectly with the most straightforward emission models, and the inferred spectral index and flux level cannot account for the entire extragalactic neutrino flux, these results suggest that Seyfert galaxies as a class may contribute to the quasi-diffuse extragalactic neutrino flux, and are consistent with the idea that a considerable portion of the flux arises from sources opaque to gamma rays.
    
    Ponente: Tyce DeYoung (Michigan State University)
    
    DeYoung_TeVPA.pdf
  - 15:45
    
    Search for X-ray transient counterparts for the IceCube neutrino events with MAXI 15m
    
    Multimessenger follow-up observations triggered by high-energy neutrino signals offer a powerful method for identifying cosmic ray sources, particularly when the sources are transient. In the energy range of neutrinos above 100 TeV, X-ray transients are a plausible source candidate, especially if the cosmic neutrino background radiation above 100 TeV originates from the same class of objects that emit ultrahigh-energy cosmic rays (UHECRs). We probe this hypothesis by searching for X-ray flashes associated with neutrino events detected by the IceCube Neutrino Observatory in archival data collected by the Monitor of All Sky X-ray Image (MAXI) mission. We present our findings on the combined analysis of neutrinos and soft X-rays, and the resulting constraints on the source parameter space. We also discuss the implications of the results for the characteristics of UHECR transient origins.
    
    Ponente: Shigeru Yoshida (Chiba University)
    
    IceCubeMAXITeVPA2025.pdf
  - 16:00
    
    Combined KM3NeT/ARCA and ANTARES searches for compact neutrino sources 15m
    
    Neutrino telescopes offer unique insights into some of the most extreme and energetic phenomena in the Universe. The ANTARES detector, which operated for 16 years off the coast of Toulon (France) until 2022, has played a pioneering role in deep-sea neutrino observations. The next-generation KM3NeT neutrino telescopes, ORCA and ARCA, designed to push the boundaries of atmospheric and astrophysical neutrino detection, are currently under construction.
    
    In recent years, the search for astrophysical neutrino sources has gained momentum, as their detection would provide crucial evidence of hadronic acceleration mechanisms at play in the most powerful cosmic environments. This study analyses the combined dataset from ANTARES and the available KM3NeT/ARCA observations, focusing on the detection of high-energy neutrinos from point-like sources.
    
    A comprehensive catalog of about 100 point-like sources and the ones with extensions up to few degrees has been examined for potential neutrino emissions. This selection includes prominent gamma-ray emitters, Galactic gamma-ray sources with possible hadronic components (TeVCat), extragalactic AGNs with intense radio flux detected by VLBI, and the most promising candidates previously investigated by IceCube and ANTARES. The results of this analysis represent a significant step toward uncovering the origin of cosmic neutrinos and advancing multi-messenger astronomy.
    
    Ponente: Vladimir Kulikovskiy (INFN - Sezione di Genova)
    
    Talk_TeVPA2025_VKulikovskiy_ANTARCA_final.pdf
- 16:15 → 16:45
  
  Coffee Break 30m ADEIT
  
  ADEIT
- 16:45 → 18:30
  Cosmic Rays Room 2.1+2.2 (ADEIT)
  
  Room 2.1+2.2
  
  ADEIT
  
  Moderador: Brian Rauch (Washington University in St. Louis)
  - 16:45
    
    Properties of Cosmic Phosphorus Nuclei Measured by the Alpha Magnetic Spectrometer 15m
    
    Phosphorus (P) nuclei in cosmic rays are secondary particles thought to be mainly produced by the collisions of heavier nuclei with the interstellar medium. The precise measurement of P nuclei is crucial for advancing the understanding of cosmic ray propagation. We present the latest results on the properties of P cosmic-ray nuclei flux in the rigidity range 2.15 GV to 1.2 TV based on 0.16 million nuclei collected by the AMS experiment during 13.5 years of operation from May 2011 to November 2024.
    
    Ponente: Zhen Liu (INFN-Roma2)
    
    AMS_Phosphorus_TeVPA2025_ZhenLIU.pdf
  - 17:00
    
    Unique Properties of Secondary Cosmic Rays: Results from the Alpha Magnetic Spectrometer 15m
    
    We present high statistics measurements of the secondary cosmic rays Lithium, Beryllium, Boron, and Fluorine based on 11.5 years of AMS data. The properties of the secondary cosmic ray fluxes and their ratios to the primary cosmic rays Li/C, Be/C, B/C, Li/O, Be/O, B/O, and F/Si are discussed. The systematic comparison with the latest GALPROP cosmic ray model is presented.
    
    Ponente: Jin Zhang (Shandong University)
    
    AMS_SecondaryCR_TeVPa2025.pdf
  - 17:15
    
    Impact of in-source production of Boron on the B/C ratio in cosmic rays 15m
    
    The current cosmic-ray(CR) measurements show anomalies in secondary CRs, for example a hardening of the ratio of boron to carbon at high energies, which deviates from the standard galactic CR propagation model: $B/C \propto E^{-\delta}$. It may suggest the generation of secondary CRs near or inside the accelerators, e.g, SNRs. The accumulated grammage in the sources may be non-negligible and contribute to the measured grammage. We calculate the boron production in different SNRs(Type-Ia & core-collapse), and simulate in two diffusion regimes: 1. Bohm diffusion. 2. Turbulence self-generated by the CRs, which realistically models the enhanced confinement of CRs close to the accelerators. Our preliminary results show a hard B/C ratio in the energy range up to $10^{3}$ GeV/n developing within the SNRs. The level, approximately $10^{-3}-10^{-2}$, depends on the diffusion model, the density of the source region, and the acceleration time. It suggests that a significant fraction of the observed high-energy boron at TeV energies may originate from near-source production in SNRs, potentially explaining the flattening of the B/C ratio reported by DAMPE and AMS-02.
    
    Ponente: Qiqi Jiang
    
    TEVPA2025-new.pdf
  - 17:30
    
    Precision Measurement of Cosmic Ray Deuterons with Alpha Magnetic Spectrometer 15m
    
    Precision measurements by the Alpha Magnetic Spectrometer (AMS) on the International Space Station of the deuteron ($D$) flux are presented. The measurements are based on 21 million $D$ nuclei in the rigidity range from 1.9 to 21 GV collected from May 2011 to April 2021. We observe that over the entire rigidity range the $D$ flux exhibits nearly identical time variations with the $p$, $^3$He , and $^4$He fluxes. Above 4.5 GV, the $D$/$^4$He flux ratio is time independent and its rigidity dependence is well described by a single power law $\propto R^\Delta$ with $\Delta_{D/{}^4\text{He}} =-0.108 \pm 0.005$. This is in contrast with the $^3$He/$^4$He flux ratio for which we find $\Delta_{{}^3\text{He}/{}^4\text{He}} =-0.289 \pm 0.003$. Above $\sim$13 GV we find a nearly identical rigidity dependence of the $D$ and $p$ fluxes with a $D/p$ flux ratio of $0.027 \pm 0.001$. These unexpected observations indicate that cosmic deuterons have a sizable primarylike component. With a method independent of cosmic ray propagation, we obtain the primary component of the $D$ flux equal to $9.4 \pm 0.5 \%$ of the $^4$He flux and the secondary component of the $D$ flux equal to $58 \pm 5 \%$ of the $^3\text{He}$ flux.
    
    Ponente: Francisco Hernández Nicolás (CIEMAT - Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas)
    
    TeVPA_2025_final.pdf
  - 17:45
    
    Properties of Cosmic Beryllium Isotopes Measured by the Alpha Magnetic Spectrometer 15m
    
    Beryllium nuclei in cosmic rays are expected to be secondaries produced by the fragmentation of primary cosmic rays during their propagation in the Galaxy. Therefore, their fluxes contain essential information on cosmic ray propagation and sources. As the radioactive isotope 10Be decays to 10B with a half-life comparable to the cosmic-ray residence time in the Galaxy, the 10Be/9Be ratio can be used to measure the cosmic-ray propagation volume. Current measurements of the 10Be/9Be ratios are limited to energies below 2 GeV/n and are affected by large uncertainties. We present the unique measurement of the fluxes of 7Be, 9Be, and 10Be and their ratios across an extended energy range, based on 13.5 years of AMS data.
    
    Ponente: Dimitrii Krasnopevtsev (Massachusetts Inst. of Technology (US))
    
    AMS-Be-Isotopes_Krasnopevtsev.pdf
  - 18:00
    
    Confinement of Cosmic rays near the accelerators 15m
    
    Recent cosmic-ray (CR) measurements have revealed unexpected anomalies in secondary CRs, namely deviations from the predictions of the so-called standard Galactic CR paradigm regarding the composition and energy spectra of the products of interactions of primary (accelerated) CRs with interstellar gas: (i) antiparticles (positrons and antiprotons), (ii) light elements of the (Li, Be, B) group, and (iii) diffuse gamma-rays. We argue that the new measurements can still be explained within the standard CR paradigm but with an additional assumption that CRs spend a significant part of their lifetime near their formation sites. The latter can be realized if CRs propagate more slowly in these localized regions than in the interstellar medium.
    
    Ponente: Ruizhi Yang (USTC)
    
    CR_confinement.pdf
  - 18:15
    
    Every Nearby Pulsar is Surrounded by Inhibited Diffusion 15m
    
    The electron + positron cosmic-ray flux recently released by the H.E.S.S. telescope shows a remarkable behaviour: It breaks at around 1 TeV and falls off quickly, following a smooth powerlaw. This is in tension with simple pulsar models, which predict a much harder electron spectrum at tens of TeV. However, in two-zone diffusion models, propagation of high-energy electrons is inhibited in a region around the pulsar (consistent with pulsar wind nebulae and TeV halos), causing the spectral hardening to soften the high-energy spectrum in agreement with observations. We find that there are a tens of known pulsars that would individually overproduce the H.E.S.S. TeV flux, allowing us to conclude that every nearby pulsar must be surrounded by a zone of inhibited diffusion.
    
    Ponente: Isabelle John (University of Turin)
    
    TeVPA_Valencia_2025.pdf
- 16:45 → 18:30
  Cosmology Salón de Grados (ADEIT)
  
  Salón de Grados
  
  ADEIT
  
  Moderador: Hidde Jense
  - 16:45
    
    Invited Talk: Updated Cosmological Constraints with the South Pole Telescope Data 15m
    
    Recently, the South Pole Telescope (SPT) released its measurements of temperature (T) and E-mode polarization power spectra of the cosmic microwave background (CMB). These measurements, made by two years of observation of 4% of the sky, are the most precise in EE and TE spectra for the multipole ranges 1800-4000 and 2200-4000, respectively. When combined with ACT-DR6 and Planck data, these three represent the most precise CMB data combination to date. In this talk, constraints on a variety of models coming from SPT data alone and in combination with ACT-DR6 and Planck are presented. The considered models include ΛCDM, a few of its extensions and Hubble tension solutions, such as modified recombination, the varying electron mass in non-flat geometry and early dark energy. The results underline the constraining power of ground-based CMB experiments, which now reaches the precision of Planck. Moreover, constraints resulting from the combination of these CMB data sets with baryon acoustic oscillations (BAO) data from DESI-DR2 are also presented. The projection of the discrepancy between CMB data and DESI-DR2 in ΛCDM on these models is also highlighted in the talk.
    
    Ponente: Ali Rida Khalife (Institut d'Astrophysique de Paris, Sorbonne University and CNRS)
    
    Updated Cosmological Constraints with SPT
  - 17:00
    
    Cosmic Tensions and Neutrino cosmology 15m
    
    Tensions between independent cosmological probes continue to challenge the $\Lambda$CDM framework. The persistent ~5$\sigma$ discrepancy between early- and late-time determinations of the Hubble parameter remains unresolved, while recent DESI BAO measurements, when interpreted within $\Lambda$CDM, yield constraints on the sum of neutrino masses that increasingly conflict with lower bounds from particle physics. Dynamical dark energy models offer a possible route to relax the neutrino mass tension by introducing additional background-level degrees of freedom. In some cases, these models are even favored over a cosmological constant at more than ~4$\sigma$. However, such late-time extensions generally fail to resolve the Hubble tension and can, in fact, worsen it. Conversely, models that appear promising in raising $H_0$ tend to push the inferred neutrino mass bounds toward unrealistically small values, deepening the disagreement with oscillation experiments. This leaves us questioning whether a consistent resolution is still within reach, or whether we are instead confronted with an unavoidable trade-off. To address this, in this talk I will further explore the three-way interplay between dark sector physics, neutrino cosmology, and cosmic tensions, reviewing what a resolution could require in terms of new physics, and analyzing the role of potential unaccounted-for observational systematics in the data.
    
    Ponente: William Giare (University of Sheffield)
    
    Giare_TEVPA.pdf
  - 17:15
    
    Current constraints on cosmological scenarios with very low reheating temperatures 15m
    
    We present a comprehensive analysis of the effects of models with very low reheating scenarios ($T_\text{RH} \sim \mathcal{O}(\text{MeV})$) on the cosmological observables and derive corresponding bounds on the reheating temperature. With respect to previous work, our study includes a more precise computation of neutrino distribution functions, leveraging the latest datasets from cosmological surveys.
    We perform a joint analysis that combines constraints from Big Bang Nucleosynthesis, the Cosmic Microwave Background, and galaxy surveys, alongside separate investigations of these datasets, carefully assessing the impact of different choices of priors.
    At the $95\%$ confidence level, we establish a lower bound on the reheating temperature of $T_\text{RH} > 5.96 \; \text{MeV} $, representing the most stringent constraint to date.
    
    Ponente: Nicola Barbieri (INFN Ferrara)
    
    talk_TeVPA2025.pdf
  - 17:30
    
    Baryogenesis in the Axiverse 15m
    
    Axiogenesis links the baryon asymmetry and dark matter abundance through the dynamics of the QCD axion, but its minimal form overproduces dark matter and can exacerbate the QCD axion quality problem. In this talk, I’ll show how these issues are naturally resolved in an axiverse framework, where the QCD axion arises from multiple interacting axions. This setup generates large axion velocities without spoiling the Strong CP solution and introduces new friction channels that reduce the relic abundance. The resulting theory makes imminently testable predictions for haloscopes and the CMB.
    
    Ponente: David Cyncynates (ICTP Trieste)
    
    TeVPA.pdf
  - 17:45
    
    Reionization and the Hubble Constant: Correlations in the Cosmic Microwave Background 15m
    
    Recently, the James Webb Space Telescope (JWST) has found early galaxies producing photons from more efficient ionization than previously assumed. This may suggest a reionization process with a larger reionization optical depth, $\tau_{reio}$, in some mild disagreement with that inferred from measurements of cosmic microwave background (CMB). Intriguingly, the CMB would prefer larger values of $\tau_{reio}$, more consistent with the recent JWST hint, if the large-scale measurements (i.e. $\ell <30$) of E-mode polarization are removed. In addition, $\tau_{reio}$ has an indirect correlation with today's Hubble constant $H_0$ in $\Lambda$CDM. Motivated by these interesting observations, we investigate and reveal the underlying mechanism for this correlation, using the CMB dataset without the low-$\ell$ polarization data as a proxy for a potential cosmology with a larger $\tau_{reio}$. We further explore how this correlation may impact the Hubble tension between early and late universe measurements of $H_0$, in $\Lambda$CDM as well as two proposals to alleviate the Hubble tension: the dark radiation (DR) and early dark energy (EDE) models. We find that the Hubble tension gets further reduced mildly for almost all cases due to the larger $\tau_{reio}$ and its positive correlation with $H_0$, with either the Baryon Acoustic Oscillations (BAO) data before those from the Dark Energy Spectroscopic Instrument (DESI) or the DESI data.
    
    Ponente: Praniti Singh (Brown University)
    
    TeVpa_Praniti_Singh.pdf
  - 18:00
    
    Baryonic Imprints on Dark Matter Halos and Substructure in the Mochima Simulations 15m
    
    We use the Mochima suite of cosmological zoom-in simulations (arXiv:2004.06008) to examine how different star formation and feedback models shape the dark matter distribution in a Milky Way–mass galaxy and its satellites (arXiv:2301.06189). All runs share identical initial conditions, allowing controlled comparisons across subgrid prescriptions. In every hydrodynamical case, the host halo develops a steeper inner dark matter profile than the dark matter–only control, with inner slopes ranging from γ∼1.3−1.8 depending on early stellar bulge mass and feedback strength. Despite bursty star formation in some runs, no fully cored profiles emerge, underscoring the tension between contraction and feedback. The solar neighborhood phase-space distribution of dark matter is also modified: although broadly consistent with standard expectations, the speed distribution at the solar circle shifts due to baryonic contraction.
    Satellite survival correlates with host halo concentration and stellar content. Simulations with extended discs and deep central potentials show enhanced tidal disruption of low-mass subhalos, while subhalos with significant stellar mass exhibit greater resilience. The resulting spread in subhalo inner slopes matches the observed cusp–core diversity and is tied to star formation history. These results emphasize the importance of baryonic physics in dark matter modeling, with implications for structure formation, (in)direct detection, and the interpretation of future surveys.
    
    Ponente: Arturo Núñez-Castiñeyra (Institut d'Astrophysique de Paris)
    
    AnunezCasTeVPA2025.pdf
  - 18:15
    
    Cosmology in an extended parameter space: new constraints on dark energy and neutrino masses with DESI BAO 15m
    
    Based on arXiv: 2409.13022 and arXiv: 2504.15340 (both published in ApJ Letters) We update constraints on cosmological parameters in a 12-parameter model, which extends the standard 6-parameter ΛCDM to include dynamical dark energy and massive neutrinos, along with other new parameters. We use the latest Planck PR4 (2020) likelihoods, DESI DR1 & DR2 BAO, and the latest uncalibrated type Ia Supernovae (SNe) datasets. In this talk, I will discuss the implications for dynamical dark energy in such an extended model, and at the same time, provide robust bounds on neutrino masses which will be useful for the astro- and particle physics communities. I will also discuss the current status of the weak lensing tension and the Hubble tension in this extended cosmology.
    
    Ponente: Shouvik Roy Choudhury (Academia Sinica Institute of Astronomy and Astrophysics)
    
    Talk_TeVPA_Shouvik_Roy_Choudhury.pdf
- 16:45 → 18:30
  Dark Matter: Direct Detection Room 3.1+3.2 (ADEIT)
  
  Room 3.1+3.2
  
  ADEIT
  
  Moderador: Karoline Schäffner (Max-Planck Institute for Physics)
  - 16:45
    
    Composite dark matter disassembly in the Earth 15m
    
    Composite dark matter models, where dark matter exists in bound states formed in the early universe, have long been a source of scientific interest. I will focus on loosely bound dark matter composite states, where the binding energy per constituent is small compared to the constituent’s bare mass. If this binding energy is sufficiently small, scattering with Standard Model nuclei will disassemble composites as they pass through the Earth. I will present results from modelling composite disassembly in the Earth prior to their arrival in direct detection experiments, and begin exploring the expected detection signatures from these disassembled composites.
    
    Ponente: Yilda Boukhtouchen (Queen's University)
    
    Boukhtouchen-TEVPANov2025-V2.pdf BoukhtouchenYilda-TEVPANov2025.pdf
  - 17:00
    
    Neutrino Fog and Dark Matter Direct Detection:Generalized Mediator Approach with XENONnT and PandaX-4T 15m
    
    The recent observation of coherent elastic neutrino-nucleus scattering (CE$\nu$NS) from solar $^8$B neutrinos by the XENONnT and PandaX-4T collaborations marks the onset of the neutrino fog in direct dark matter detection experiments. This opens up new possibilities to explore the interplay between CE$\nu$NS and WIMP-nucleus scattering within a common theoretical framework. In this work, we study scenarios where a single new mediator—introduced alongside the Standard Model—simultaneously mediates both CE$\nu$NS and dark matter–nucleus interactions. We consider a set of generalized interactions including scalar, vector, pseudoscalar, and axial-vector mediators, encompassing both spin-independent and spin-dependent couplings. Using recent nuclear recoil data from XENONnT and PandaX-4T, we derive constraints on the zero momentum transfer WIMP-nucleon scattering cross section and the WIMP mass. Additionally, we compute the neutrino fog within the same interaction framework, demonstrating how the dark matter sensitivity approaches this background limit in the mass range of approximately $3$–$10$ GeV, where the neutrino signal becomes indistinguishable from that of light WIMPs. We also highlight that this representation of direct detection constraints on WIMPs—expressed as limits on the zero momentum transfer WIMP-nucleon cross section and WIMP mass—is applicable when a heavy mediator is involved. For scenarios with light mediators, we instead provide limits in the plane of coupling strength versus mediator mass. These results contribute to a more unified and comprehensive interpretation of current and future direct detection data in the presence of neutrino backgrounds.
    
    Ponente: Anirban Majumdar (Indian Institute of Science Education and Research - Bhopal)
    
    TeVPA_2025.pdf
  - 17:15
    
    Inelastic dark matter boosted by terrestrial collisions 15m
    
    Inelastic dark matter (IDM) models feature an energy threshold for scattering with Standard Model particles, which enables their consistency with the increasingly stringent limits placed by direct detection experiments. In a typical construction, elastic scattering is absent at tree level, and a lighter dark matter state must upscatter into a heavier state in order to interact with the nuclei in a detector. We model the excitation of IDM in the Earth followed by its downscattering inside a detector, and we show that considering this process markedly enhances the sensitivity of existing detectors. In particular, current limits based on XENON100 and XENON1T data can be extended to significantly larger mass splittings.
    
    Ponente: Christopher Cappiello
    
    TeVPA 2025 Inelastic Dark Matter.pdf
  - 17:30
    
    Dark matter pair detection via atomic spectroscopy 15m
    
    Atomic transitions are among the most studied and precisely measured phenomena in physics, making them an attractive probe for new physics. If dark matter (DM) interacts with electrons, it could trigger electronic transitions via the absorption or scattering of DM with the atom's electrons. The selection rules for these transitions depend on the Lorentz structure of the DM interaction. An interesting case is that of DM interacting via scalar and axial-vector vertices, which induce transitions that are heavily suppressed for photons, resulting in a background-free channel for DM discovery. In this talk we will lay out the fundamentals of these concepts in the case of absorption and scattering of DM pairs.
    
    Ponente: Javier Pérez Soler (IFIC, CSIC-UV)
    
    Dark matter pair absorption TeVPA.pdf
  - 17:45
    
    Sub-GeV Dark Matter Under Pressure from Direct Detection 15m
    
    The DAMIC-M collaboration recently reported impressive bounds on sub-GeV dark matter, robustly testing both thermal and non-thermal models for the very first time. In this work, we derive novel bounds from the recent PandaX-4T ionization S2-only search for Coherent Elastic Neutrino Nucleus Scattering (CEνNS). We find that the PandaX-4T S2-only data is able to compete with the DAMIC-M results, providing the best constraints for scalar and asymmetric thermal dark matter models for masses between 20 to 200 MeV. We further discuss the implications of recent direct detection results for several other sub-GeV dark matter models, highlighting their complementarity with astrophysical, cosmological, and laboratory probes.
    
    Ponente: Pablo Figueroa (IFIC, CSIC-UV)
    
    TeVPA_2025_Pablo_FF.pdf
  - 18:00
    
    Linear response theory for light dark matter-electron scattering in materials 15m
    
    I combine the non-relativistic effective theory of dark matter (DM) - electron interactions with linear response theory to obtain a formalism that fully accounts for screening and collective excitations in DM-induced electronic transition rate calculations for general DM-electron interactions. In the same way that the response of a dielectric material to an external electric field in electrodynamics is described by the dielectric function, so in our formalism the response of a detector material to a DM perturbation is described by a set of generalised susceptibilities which can be directly related to densities and currents arising from the non-relativistic expansion of the Dirac Hamiltonian. I apply our formalism to assess the sensitivity of non-spin-polarised detectors, and find that in-medium effects significantly affect the experimental sensitivity if DM couples to the detector's electron density, while being decoupled from other densities and currents. Our formalism can be straightforwardly extended to the case of spin-polarised materials.
    
    Ponente: Riccardo Catena (Chalmers University of Technology)
    
    catena.pdf
  - 18:15
    
    Searching For Heavy Dark Matter with LMC Modeling 15m
    
    As the search for dark matter progresses, it is useful to refine past and future searches for heavy dark matter, including for dark matter masses well above a TeV. We show the importance of properly modeling the local dark matter velocity distribution, beyond the standard Maxwellian halo model, and in particular how accurate modeling of the Large Magellanic Cloud and Milky Way impact heavy dark matter searches. As a specific example, we examine the effect of the LMC on heavy dark matter bounds obtained from experiments searching for cosmic rays and magnetic monopoles using plastic etch detectors at the Ohya Mine and aboard the Skylab Space Station.
    
    Ponente: Andrew Buchanan (Queen's University)
    
    LMC TeVPA.pdf LMC TeVPA.pptx
- 16:45 → 18:30
  Gamma Rays: Galactic Salón de Actos (ADEIT)
  
  Salón de Actos
  
  ADEIT
  
  Moderador: Paula Kornecki (IAA-CSIC)
  - 16:45
    
    Pulsars in the very-high-energy gamma-ray domain 15m
    
    Space-based gamma-ray observations have established sharp cutoffs at a few GeV as a common feature of pulsar emission, with the Crab pulsar until recently the only source detected above 100 GeV. Observations with imaging atmospheric Cherenkov telescopes (IACTs), such as H.E.S.S., now reveal pulsar spectra extending up to tens of TeV. For the Vela pulsar, we detect a distinct radiation component reaching at least 20 TeV, providing clear evidence that pulsars can accelerate particles to Lorentz factors above 4 × 10^7. I will present the latest VHE pulsar results and discuss their implications for models of particle acceleration and emission in pulsar magnetospheres.
    
    Ponente: Emma de Oña Wilhelmi (Deutsches Elektronen-Synchrotron DESY)
    
    PulsarsVHE_TeVPA_deOnaWilhelmi2025.pdf PulsarsVHE_TeVPA_deOnaWilhelmi2025.pdf
  - 17:00
    
    Phase-dependent spectra of the Crab pulsar with the MAGIC telescopes 15m
    
    Over the past two decades, the discovery of pulsed very-high-energy (VHE) emission of the Crab pulsar, along with the expansion of the gamma-ray pulsar catalogue driven by the Fermi-LAT satellite, has led to a paradigm shift in the understanding of the gamma-ray emission of pulsars. Once believed to originate near the neutron star’s surface, particle acceleration and radiative processes are now suspected to result from complex magnetopsheric dynamics close to or beyond the pulsar’s light-cylinder. Several theoretical models have been proposed to explain the VHE emission of pulsars, however, distinguishing between them based on observational data has proven challenging.
    
    As one of the youngest known pulsars (~1ka), the Crab hosts extreme electromagnetic processes and its pulsed VHE emission is known to extend up to the TeV range. We present the results of a thorough study of the VHE emission of the Crab pulsar, based on observations from the Fermi-LAT satellite and the MAGIC gamma-ray telescopes. MAGIC is a system of two imaging atmospheric Cherenkov telescopes (IACTs) designed to detect gamma-ray-induced extensive atmospheric showers in the energy range between 20 GeV and 100 TeV. It has been operating since 2004 at the Roque de los Muchachos observatory, on the Canary island of La Palma, Spain. The observations on the Crab pulsar were conducted as part of the commissioning of the Sum-Trigger-II low-energy trigger system and resulted in over 100 hours of good quality data, with a detection of the pulsed emission exceeding the statistical significance of 20σ.
    
    The high-statistics dataset enables a novel phase-resolved spectral analysis, highlighting the evolution of the VHE emission in both energy and time domains. The combined Fermi-LAT and MAGIC observations successfully bridge a statistics gap between 10 GeV and 100 GeV, providing strong evidence for a single inverse-Compton component as the source of the VHE emission. A joint modeling of the spectrum across the entire phase range also imposes stringent constraints on relative energy scale systematics between MAGIC and Fermi-LAT, providing an excellent confirmation of the capabilities of IACTs for gamma-ray pulsar studies. These results constitute a benchmark dataset to test theoretical models of pulsed emission.
    
    Ponente: Dr. Giovanni Ceribella (Max Planck Institut for Physics)
    
    GCeribella_TeVPA2025__20251104.pdf
  - 17:15
    
    Multiwavelength modeling including the first hard X-ray observations of the PeVatron Candidate Pulsar Wind Nebula in G0.9+0.1 15m
    
    Pulsar wind nebulae (PWNe) are bubbles of relativistic particle outflows, primarily composed of electrons and positrons, which are continuously injected from pulsars and often exhibit broadband non-thermal radiation originating from synchrotron and inverse Compton scattering emission. Recently, LHAASO and HAWC observations have detected Ultra-High-Energy (UHE, E>100 TeV) gamma-ray sources associated with PWNe, making them the prime candidates for Galactic leptonic “PeVatrons”, sources capable of accelerating leptons to PeV energies inside our Galaxy.
    X-ray synchrotron radiation from TeV-PeV electrons plays a crucial role in constraining the maximum particle energies and new X-ray studies of TeV PWNe suggest that some of them can accelerate particles up to PeV energies. As such, multi-wavelength observations and broadband spectral energy distributions (SED) modelling of PWNe are the key tools for both localizing and probing the properties of the relativistic particle populations.
    We present a new study of the second brightest TeV source in the Galactic Center region: the PWN powered by the energetic pulsar PSR J1747−2809 and located inside the composite-type supernova remnant G0.9+0.1. The characteristics observed from X-ray to TeV gamma-rays, including a nearby UHE source observed by HAWC, indicate that G0.9+0.1 is a PeVatron candidate. For the first time NuSTAR has detected hard X-ray emission up to 30 keV, revealing the synchrotron burn-off signature of the relativistic electrons. New insights on the source are provided through multiwavelength SED modeling incorporating radio to TeV data. Preliminary results suggest that the PWN in G0.9-0.1 has not yet interacted with the reverse SNR shock, offering a valuable case study for future observatories such as CTAO, AXIS, and NewAthena.
    
    Ponente: Giulia Brunelli (University and INAF-OAS Bologna)
    
    G09_01_TeVPA2025.pdf
  - 17:30
    
    Gamma-ray emission from Pulsar Wind Nebulae in the inner Galactic center 15m
    
    A point-like gamma-ray source (HESS J1745–290) has been detected in the inner Galactic Center, spatially coincident with Sagittarius A (Sgr A). However, the currently quiescent state of Sgr A challenges its interpretation as the origin of the emission. An alternative explanation is that a single pulsar wind nebula (PWN) accounts for the observed signal. However, X-ray observations have identified dozens of PWN candidates within the angular resolution of the gamma-ray instrument. Our goal is to determine whether the point-like gamma-ray emission observed toward Sgr A can be attributed to a population of PWNe. We develop a PWN evolutionary model that is consistent with the observed properties of pulsars in the Galaxy and with interstellar medium conditions representative of the Galactic Center. We compute the cumulative gamma-ray emission from $\sim 10^{35}$ synthetic PWN populations and compare the results with current observations. Although the observed spectrum can be reproduced by several hundred different PWN populations, the rapid evolution of all PWNe in the GC environment prevents their simultaneous presence. At most, two PWNe can coexist within the central 30 pc, in contrast with X-ray observations. In conclusion, the observed gamma-ray spectrum could be explained by one or two PWNe embedded in an intense ambient photon field. The remaining X-ray sources are likely bow shocks from pulsars, with negligible gamma-ray emission.
    
    Ponente: Andrés Scherer (Universidad de Santiago de Chile)
    
    AS-TeVPA.pdf
  - 17:45
    
    Impact of interstellar magnetic field parameters on the asymmetry of pulsar halos 15m
    
    There has been ongoing debate about the potential unconfirmed asymmetric structure of the diffuse $\gamma$-ray emission of the Geminga halo. In this work, we adhere to first principles, injecting and propagating individual cosmic ray (CR) electrons in 3D realizations of turbulent magnetic fields characterized by Kolmogorov turbulence and Bohm turbulence. The particle motion is governed by the Lorentz force, and their energy losses are accounted for through synchrotron and inverse Compton scattering. Furthermore, we consider potential regular magnetic field and the inclination angle between the line of sight (LOS) and the magnetic field lines (MFLs) direction, calculating the resulting gamma-ray emission, comparing it with the HAWC surface brightness measurements. We confirmed that the coherence length $L_{\rm c}$ could be constrained around several pc, the $\chi^2$/d.o.f. fitting findings using the HAWC data suggest that the presence of a regular magnetic field. The Bohm turbulence corresponds to the cosmic-ray-driven instability scenario, which is characterized by more tangled magnetic field lines and a more isotropic distribution of cosmic rays around the injection site, performs worse than Kolmogorov turbulence in reproducing the observed morphology. This results suggest the possibility of potential filamentary structure inside the Geminga halo, while limited by the resolution of very-high-energy (VHE) detectors, the inner asymmetry structure may be invisible. In an extreme case where a large coherence length $L_{\rm c}$ is combined with a strong regular magnetic field, and the line of sight happens to align with the direction of the MFLs, the projected morphology of the pulsar halo appears nearly isotropic. Nevertheless, our results indicate that the underlying filamentary structures remain preserved and are not erased by this projection effect.
    
    Ponente: Yuan Li (Tsung-Dao Lee Institute)
    
    tevpa.pdf
  - 18:00
    
    Geminga and LHAASO J0621+3755: Pushing the Boundaries of X-ray and TeV Observations of Pulsar Halos 15m
    
    Pulsar halos—extended regions of relativistic electrons surrounding middle-aged pulsars—offer critical insight into cosmic-ray acceleration and transport in the interstellar medium. These sources are often bright in the TeV gamma-ray band due to inverse Compton scattering by the most energetic electrons, which are also expected to emit synchrotron radiation in the X-ray band. A multiwavelength approach in the X-ray and TeV bands is therefore essential for probing the highest-energy electron populations. However, current-generation X-ray telescopes and imaging atmospheric Cherenkov telescopes face major challenges in detecting such faint, extended emission due to their limited fields of view.
    To overcome these limitations, we employ novel analysis techniques and present the most detailed multiwavelength investigation to date of two systems: the archetypal Geminga halo and the unidentified gamma-ray source LHAASO J0621+3755. For Geminga, Manconi et al. exploit NuSTAR's stray light to probe diffuse X-ray emission over several degrees. For LHAASO J0621+3755, a candidate pulsar halo spatially coincident with the gamma-ray pulsar PSR J0622+3749, the VERITAS collaboration et al. analyze 40 hours of VERITAS data to look for extended TeV emission using a new technique that accurately models the background across the entire field of view. For both sources, we apply our theoretical model for the spatial and spectral distribution of pulsar halo emission to interpret our multiwavelength observations. These comparisons allow us to place stringent constraints on the magnetic field strength and the nature of cosmic-ray diffusion around the sources. We also report the first detection of X-ray emission and pulsation from PSR J0622+3749 using XMM-Newton. Finally, we discuss the prospects for future observations with the wide fields of view and high sensitivity of SRG/ART-XC, AXIS, and CTAO, which will play a key role in advancing our understanding of particle propagation near cosmic-ray accelerators.
    
    Ponente: Jooyun Woo (Columbia University)
    
    Geminga_LHAASOJ0621_TeVPA2025.pdf
  - 18:15
    
    CTAO Forecasting for the TeV Halos of Geminga and Monogem 15m
    
    TeV “halos” discovered around Geminga and Monogem by HAWC expose pockets of severely quenched particle diffusion close to middle-aged pulsars. Resolving the properties of these slow-diffusion zones, such as the size of the slow-diffusion zone, and local magnetic field strength, is pivotal for modelling lepton transport and for assessing the pulsars’ contribution to the local positron excess. The Cherenkov Telescope Array Observatory (CTAO), spanning ~30 GeV to beyond 100 TeV with arc-minute imaging, can sharpen those measurements decisively. We present end-to-end forecasts that couple two-zone GALPROP simulations to CTAO instrument response functions and realistic diffuse-background models. For both Geminga and Monogem, CTAO should pin down halo radii to ≲20%, and the injection spectral index to \Delta Gamma ≲ 0.2. Such precision will convert TeV-halo studies into a laboratory for cosmic-ray diffusion physics.
    
    Ponente: Youyou Li (GRAPPA, University of Amsterdam)
    
    Youyou_nov04_tevpa25-tevhalo-ctao.pdf
- 16:45 → 18:30
  Neutrinos: Galactic neutrinos Room 1.1+1.2 (ADEIT)
  
  Room 1.1+1.2
  
  ADEIT
  
  Moderador: Xavier Rodrigues (APC, Paris)
  - 16:45
    
    IceCube searches for steady-state sub-TeV neutrino emission from galactic and extragalactic source candidates 15m
    
    The IceCube Neutrino Observatory is a cubic kilometer neutrino telescope located at the South Pole instrumented within deep Antarctic ice. Recently, IceCube has reported evidence of TeV-scale neutrino emission from NGC 1068, a nearby Seyfert II galaxy, suggesting that active galactic nuclei could be potential sources of astrophysical neutrinos. Searches for time-dependent 10 GeV to 1 TeV astrophysical neutrino emission have been conducted. Naturally, an analysis focusing on lower energy steady-state neutrino emission from NGC 1068 is in order. Such a study is further motivated by the soft spectral index of NGC 1068; an extrapolation of the power-law spectrum reveals that most of its neutrino emission may fall within an energy range sensitive to a low-energy analysis. Another motivation stems from evidence of neutrino emission from the Galactic Plane. Although this emission is assumed to be diffuse, a fraction of the observed neutrinos could stem from a collection of yet unresolved point sources. To wit, Galactic Plane pion bump sources observed by Fermi-LAT demonstrate a low-energy soft gamma-ray spectrum, potentially capable of producing similarly soft and low-energy neutrino spectra. In this presentation, we present our search for emitters of steady-state sub-TeV neutrinos. The search is performed with a sample of intrinsic X-ray bright Seyfert Galaxies selected from the BASS survey, as well as Fermi-LAT detected galactic pion bump sources.
    
    Ponente: Andrew Wang (Georgia Institute of Technology)
    
    awang_tevpa2025_parallel.pdf
  - 17:00
    
    Measuring the Astrophysical Galactic Plane Neutrino Flux using the IceCube Multi-Flavor Astrophysical Neutrino Sample 15m
    
    The IceCube Neutrino Observatory has provided new insights into the high-energy universe, unveiling neutrinos from the galactic plane to extragalactic supermassive black holes. In this work, we present a 12.3-year, full-sky, all-flavor dataset, the IceCube Multi-Flavor Astrophysics Neutrino sample (ICEMAN). ICEMAN is the combination of three largely independent neutrino samples of different event morphologies. It builds upon the previous work of the DNN-based cascade sample, Enhanced Starting Track Event Selection, and the Northern Track sample. Recent improvements in ice modeling and detector calibration are also incorporated into the cascade reconstruction. This dataset was used in an unbinned maximum likelihood to carry out a template-based measurement of the diffuse galactic neutrino flux across four distinct model hypotheses. We will present preliminary results addressing the different model assumptions.
    
    Ponente: Matthias Thiesmeyer (University of Wisconsin-Madison)
    
    2025-11-020-TeVPA-2025-Thiesmeyer.pdf
  - 17:15
    
    Measurement of the Neutrino Flux in Segments along the Galactic Plane with IceCube 15m
    
    Gamma-ray emission from the plane of the Milky Way is understood as partly originating from the interaction of cosmic rays with the interstellar medium. The same interaction is expected to produce a corresponding flux of neutrinos. In 2023, IceCube reported the first observation of this galactic neutrino flux at 4.5𝜎 confidence level. The analysis relied on neutrino flux predictions — based on gamma ray observations — to model the expected neutrino emission from the galactic plane. Three signal hypotheses describing different possible spatial and energy distributions were tested, where the single free parameter in each test was the normalization of the neutrino flux.
    We present first results of an analysis that can improve the characterization of Galactic neutrino emission by dividing the galactic plane into segments in galactic longitude. An unbinned maximum-likelihood analysis is used that can fit the spectral index and the flux normalization separately in each segment. While gamma ray emission from the Galactic Plane could be partly of leptonic origin, the neutrino flux must come from hadronic processes. Measuring a spectral index could further help to understand the contribution of unresolved neutrino sources inside the galactic plane. This work uses a full-sky cascade dataset and provides model-independent insight into the variation of the neutrino flux and energy distribution from different regions of the galactic plane.
    
    Ponente: Ludwig Neste (Stockholm University / Oscar Klein Centre)
    
    2025-11-04-TeVPA.pdf
  - 17:30
    
    Joint KM3NeT and HAWC Analysis of Galactic Sources 15m
    
    Galactic sources are key to understanding cosmic-ray acceleration and the extreme astrophysics environment in the Milky Way. Some of these sources are expected to emit both gamma rays and neutrinos: while gamma rays trace high-energy particle interactions, neutrinos provide a direct probe of hadronic acceleration processes. To study these phenomena, observatories with broad energy coverage and high-duty cycles, such as KM3NeT and HAWC, are particularly well-suited. Both instruments are optimized for time-integrated observations and can also support follow-up studies of transient events. In this work, we present first estimations of the capabilities of a joint KM3NeT and HAWC analysis to constrain the hadronic contribution to the emission processes of selected Galactic sources, using KM3NeT Monte Carlo simulations and HAWC observational data. The analysis is performed within the Gammapy framework, enabling a unified treatment of gamma-ray and neutrino data with consistent modeling and likelihood fitting.
    
    Ponente: Sara Coutiño De León (IFIC, CSIC-UV)
    
    Joint_KM3NeT_HAWC_TeVPA2025.pdf
  - 17:45
    
    The very-high-energy neutrino (and gamma-ray) flux from the Galactic Plane 15m
    
    We present updated predictions for the very-high-energy neutrino and gamma-ray flux from the Galactic Plane. Our calculations account for both the diffuse emission generated by cosmic-ray interactions with interstellar gas and the cumulative flux from sources too faint to be resolved by current neutrino or gamma-ray telescopes. The diffuse flux estimates incorporate various assumptions regarding the interstellar gas distribution, the spatial and spectral distribution of cosmic rays (including the possibility of spectral hardening in the inner Galaxy), and the latest local cosmic-ray measurements at PeV energies reported by LHAASO. We validate our predictions against recent gamma-ray observations and compare them with the latest results from neutrino telescopes.
    
    Ponente: Francesco Villante (University of L’Aquila and INFN-LNGS)
    
    Villante_TeVPA_2025.pdf
  - 18:00
    
    Estimating the Galactic Neutrino Flux 15m
    
    The Milky Way hosts astrophysical accelerators capable of producing high-energy cosmic rays. These cosmic rays can interact with the interstellar medium across the Galaxy to produce neutrinos and gamma rays (propagation component), while their interactions with ambient material at their acceleration sites, such as supernova remnants, can give rise to source component of the gamma-ray and neutrino flux. In this work, we estimate the neutrino flux originating from Galactic sources in the energy range of 1-100 TeV. Using simulated populations of Galactic TeV gamma-ray sources, we exploit the correlation between gamma rays and neutrinos to provide a range for the source contribution to the Galactic neutrino flux. For the upper limit, we used the full Galactic simulated gamma-ray source populations, whereas the lower limit was estimated using the hadronic component of the Galactic supernova remnant population. Finally, we compare our results with the Galactic neutrino emission measured by ANTARES and IceCube, and with the predicted propagation component of the neutrino flux.
    
    Ponente: Mohadeseh Ozlati Moghadam (University of Potsdam)
    
    TevPa.pdf
  - 18:15
    
    Young massive star clusters and their contribution to galactic neutrino and diffuse gamma-ray emission 15m
    
    Young massive stellar clusters (YMSCs) have emerged as energetic non-thermal sources, after the recent observation of extended gamma-ray emission by a dozen YMSCs. The large size of their gamma-ray halos, of the order of the excavated bubble from the collective wind, makes the detection of individual YMSCs rather challenging because of the low surface brightness. As a result, the emission from most of the Galactic YMSCs could be unresolved, thus contributing to the diffuse gamma-ray and neutrino radiation observed along the Galactic Plane. In this study, we estimate that possible contribution of the population of YMSCs to the Galactic diffuse radiative emissions, by simulating synthetic samples of these sources resembling the observed properties of local clusters. We compute the resulting secondary emission from hadronic interactions occurring in each cluster by particles accelerated at the cluster’s collective wind termination shock and at the supernovae exploded in the core, and compare them with diffuse gamma-ray and neutrino observations by different experiments, including Fermi-LAT, LHAASO, and IceCube.
    
    Ponente: Stefano Menchiari (Instituto de Astrofísica de Andalucía - CSIC)
    
    DiffuseGamma-NeutrinoYMSC_SM.pdf
miércoles, 5 noviembre
- 9:00 → 10:30
  Plenary Session: V Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Simona Toscano (IIHE - ULB)
  - 9:00
    
    Gamma-Ray Astrophysics from Space 30m
    
    Space-based gamma-ray observatories provide continuous, all-sky coverage from a few hundred keV to hundreds of GeV, bridging the hard X-ray and very-high-energy domains accessible from the ground. Instruments such as Swift-BAT, INTEGRAL, Fermi-GBM, and Fermi-LAT, among others, have enabled precision studies of non-thermal processes in astrophysical sources, cosmological measurements through the extragalactic background light and large-scale structure correlations, and time-domain discoveries of transient phenomena. In this talk, I will review key achievements and recent highlights of gamma-ray astrophysics from space, and discuss upcoming missions designed to close the MeV sensitivity gap and expand discovery space in polarization, timing, and broadband spectroscopy—advancing our understanding of the high-energy Universe.
    
    Ponente: Michela Negro (Louisiana State University)
    
    TeVPA_gammaSpace.pdf
  - 9:30
    
    Recent Advances in Cosmic Ray Physics from Hybrid Air Shower Arrays 30m
    
    The origin and nature of cosmic rays remain some of the most intriguing questions in astroparticle physics. This talk will review the latest developments in CR physics, focusing on findings from major air shower arrays operating in hybrid mode. Key results on the CR energy spectrum, composition, and arrival directions will be presented. The talk will also highlight the future prospects for CR research, and the potential for new discoveries in the field.
    
    Ponente: Jaime Álvarez-Muñiz (Universidad de Santiago de Compostela)
    
    TeVPA2025-Alvarez-Muniz.pdf
  - 10:00
    
    Advances in neutrino astrophysics 30m
    
    Neutrinos herald the dawn of multi-messenger astronomy, carrying signatures of the yet mysterious physics governing the most energetic sources in our universe. Recent developments on the role of neutrinos in cosmic sources will be reviewed together with the most exciting multi-messenger detection prospects.
    
    Ponente: Irene Tamborra (Niels Bohr Institute)
    
    TeVPA2025_Tamborra.pdf
- 10:30 → 11:00
  
  Coffee Break 30m Dome (Fundación Bancaja)
  
  Dome
  
  Fundación Bancaja
- 11:00 → 12:30
  Plenary Session: VI Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Valentina De Romeri (IFIC UV/CSIC)
  - 11:00
    
    Gravitational Waves: Experiments 30m
    
    The direct detection of gravitational waves has opened a new observational window onto the Universe, transforming both fundamental physics and astrophysics. A global network of ground-based interferometers — including the Advanced LIGO, Advanced Virgo, and KAGRA detectors — is now operating at unprecedented sensitivities, routinely detecting signals from compact binary coalescences. I will review the current status of these observatories, highlighting the most recent observing run (O4), its achievements, and the challenges encountered. The talk will also outline the technological upgrades planned for the upcoming observing runs and the path toward next-generation detectors such as the Einstein Telescope and Cosmic Explorer.
    At lower frequencies, space-based detectors like LISA will open a complementary window, targeting sources from massive black hole mergers to stochastic backgrounds, and bridging gravitational-wave astronomy with cosmology and particle physics. I will discuss the experimental landscape across these frequency bands, emphasizing synergies among current and future facilities and their role in enabling multi-messenger and fundamental physics discoveries in the coming decade.
    
    Ponente: Alicia M. Sintes (Universitat de les Illes Balears)
    
    25.11.05_Sintes_TeVPA.pptx
  - 11:30
    
    Non-WIMP and Non-Cold dark matter 30m
    
    In my talk I will briefly introduce dark matter scenarios beyond the vanilla WIMP (and cold) dark matter models. I will then move to feebly interacting to non-interacting dark matter scenarios which can be challenging to probe. Yet they may leave specific imprint in cosmology observables. I will in particular focus on Non-Cold dark matter signatures that can be expected when the dark matter production mechanism give rise to non-negligible velocity dispersion at the time of structure formation.
    
    Ponente: Laura Lopez-Honorez (ULB)
    
    25-TeVpa-LLH.pdf
  - 12:00
    
    Tensions in Modern Cosmology 30m
    
    Modern Cosmology has become a precise discipline thanks to immense improvements in Cosmic Microwave Background (CMB) and Large Scale Structure (LSS) observations, in addition to an ameliorated theoretical description of cosmological models. However, this precision uncovered tensions between datasets that challenge the standard model of Cosmology, ΛCDM. In this talk, I present a brief overview of past and existing tensions, focusing mainly on the Hubble Tension and the rising potential tension between CMB and Baryon Acoustic Oscillations measurements from the Dark Energy Spectroscopic Instrument (DESI). In addition to showing the most up-to-date status of these tensions, I describe a few of the models presented to address these tensions.
    
    Ponente: Ali Rida Khalife (IAP-CNRS and Sorbonne University)
    
    Tensions in Cosmology
- 12:30 → 14:30
  
  Lunch Break 2h ADEIT
  
  ADEIT
- 14:30 → 16:15
  Cosmic Rays Room 2.1+2.2 (ADEIT)
  
  Room 2.1+2.2
  
  ADEIT
  
  Moderador: Ioana Maris (Université Libre de Bruxelles)
  - 14:30
    
    Overview of Cosmic Ray Measurements with the Telescope Array 15m
    
    The origin and nature of cosmic rays remain one of the most intriguing unsolved problems in modern astrophysics, even more than a century after their discovery.
    The Telescope Array (TA) is the largest cosmic ray observatory in the northern hemisphere, continuously observing ultra-high energy cosmic rays (E$>10^{18}\,$eV) with a hybrid detector composed of fluorescence detectors (FD) and a surface detector (SD) array.
    To further enhance observational exposure above $10^{19}\,$eV, we have been extending the SD array by a factor of four since 2019 as part of the TAx4 project, aiming to provide higher statistics for the highest-energy cosmic rays and enabling detailed studies on the energy spectrum, anisotropy, and mass composition.
    
    In addition to ultra-high energy observations, TA has constructed high-elevation FDs and dense SD arrays (the TA Low Energy Extension, TALE) to lower the energy threshold and probe the cosmic ray spectrum, mass composition, and anisotropy in the crucial transition region from galactic to extragalactic cosmic rays ($10^{15}$–$10^{18}\,$eV).
    Recent upgrades, including an infill SD array, further enhance our sensitivity in the lower energy range, allowing for more precise studies of this transition.
    
    In this contribution, we present an overview of recent results covering five orders of magnitude in energy, and briefly discuss observations in the low-energy region relevant to the transition from galactic to extragalactic cosmic rays.
    
    Ponente: Keitaro Fujita (Institute for Cosmic Ray Research, The University of Tokyo)
    
    tevpa2025_telescopeArray.pdf
  - 14:45
    
    New full-sky studies of the distribution of ultra-high-energy cosmic-ray arrival directions 15m
    
    Ground-based full-sky studies of the angular distribution of arrival directions of ultra-high-energy cosmic rays require combining data from different observatories, such as the Pierre Auger Observatory and the Telescope Array, because no single array can cover all declinations. A working group comprising members from both the Pierre Auger and Telescope Array collaborations has been tasked with performing such studies for over a decade and has found several indications of anisotropies. Here, in addition to an overview of previous results, we also apply for the first time new analysis techniques to the data that had previously only been used on simulations.
    
    Ponente: Federico Urban (CEICO, FZU Prague)
    
    urban_tevpa2025.pdf
  - 15:00
    
    Large and intermediate scale anisotropies of ultra-high-energy cosmic rays with the Pierre Auger Observatory 15m
    
    The origin of ultra-high-energy cosmic rays (UHECRs) remains one of the most compelling open questions in astroparticle physics. The Pierre Auger Observatory, the world’s largest facility for cosmic ray detection, has provided unprecedented data to investigate anisotropies in UHECR arrival directions. At large angular scales, a significant dipolar modulation in right ascension has been observed above 8 EeV, reaching a $6.9\sigma$ significance and pointing away from the Galactic Center, strongly supporting an extragalactic origin. At intermediate angular scales, a blind search analysis revealed a localised excess around the Centaurus region within a $27^\circ$ search window radius. Additionally, a likelihood-based analysis framework has identified correlations between events above 32 EeV and several astrophysical source catalogs. The most significant result corresponds to starburst galaxies, showing a correlation at approximately $3.8\sigma$ significance.
    Similarly, a complementary approach has recently focused on the UHECRs flux along the supergalactic plane, which traces the large-scale distribution of matter in the local Universe. The most significant indication, with a post-trial significance of $3.1\sigma$, is again found in the direction of the Centaurus region, extending previous findings to lower energies. No other significant excesses were observed along other regions of the supergalactic plane, where the data are consistent with isotropy.
    
    Ponente: Luca Deval (Universita' degli studi di Torino (UniTo))
    
    TeVPA_Luca_Deval.pdf
  - 15:15
    
    Constraints on local extragalactic magnetic fields from ultra-high-energy cosmic rays 15m
    
    Ultra-high-energy cosmic rays (UHECRs) get deflected by extragalactic magnetic fields (EGMFs) when they propagate from their sources to Earth. The spread of UHECRs around their source position provides a measure of the strength of the turbulent EGMFs between the UHECR sources and Earth. Recent results from the Pierre Auger Observatory suggest correlations between the arrival directions of UHECRs with $E > 32$ EeV and catalogues of starburst galaxies (SGBs) and jetted active galactic nuclei (AGNs) [1]. We re-interpret these observations using the same methodology but taking EGMF deflections into account [2]. Including EGMF deflections allows us to obtain upper limits on the strength of turbulent EGMFs between nearby UHECR sources and the Milky Way (not necessarily EGMFs in voids) under the conservative assumption of negligible deflections in the Galactic magnetic field. When including EGMF deflections for the corresponding source distances, the expected anisotropies in arrival directions of jetted AGN are dominated by Centaurus A only, contrary to Auger's analysis, where Mrk 421 and NGC 1275 contribute significantly as well. For SBGs, the same sources as in Auger's analysis dominate the correlations. Using our framework, we derive 90% CL upper limits for the turbulent EGMF strength (including its coherence length) between the dominant UHECR sources and the Milky Way of about 4 nG Mpc$^{1/2}$ for SBGs and 7 nG Mpc$^{1/2}$ for AGNs. These limits are significantly stronger than were found in a previous work using similar assumptions but different methods [3].
    
    [1] Pierre Auger Collaboration, 2022, ApJ, 935, 170.
    
    [2] AL-Zetoun A., Van Vliet A., Taylor A. M. and Winter W., 2025, arXiv:2506.16169.
    
    [3] Van Vliet A., Palladino A., Taylor A. M. and Winter W., 2021, MNRAS, 510, 1289.
    
    Ponente: Arjen van Vliet (Khalifa University)
    
    VanVliet_ConstraintsOnMagneticFieldsFromUHECRs.pdf
  - 15:30
    
    The UHECR Mass Composition Measurements at the Pierre Auger Observatory 15m
    
    One of the major challenges in astrophysics is the estimation of the mass composition of ultra-high-energy cosmic rays (UHECRs), ions with energies exceeding $1\,\text{EeV}$ of extraterrestrial origin. Due to the low flux of UHECRs, the direct detection of the particles is infeasible, which poses several challenges for estimating their mass. When a UHECR enters Earth's atmosphere, it will eventually interact with an air molecule, inducing a cascade of secondary particles, referred to as an extensive air shower (EAS). The mass information of the UHECR is encoded stochastically in the development of the shower, in particular, the shower depth of the shower maximum, $X_\mathrm{max}$. The Pierre Auger Observatory is the largest detector for measuring UHECRs in the southern hemisphere with an area of $3000\,\mathrm{km}^2$. The Observatory employs multiple sub-detectors to measure different components of the EAS, arranged into two main parts, the Surface Detector (SD) and the Fluorescence Detector (FD). The SD consists of $1\,600$ water-Cherenkov detectors with $1.5\,\mathrm{km}$ spacing. The FD, composed of 27 fluorescence telescopes, overlooks the area above the SD. The highly sensitive FD measures $X_\mathrm{max}$ directly, while having a duty cycle about 10\% as it operates only during moonless nights. The SD, having a significantly larger duty cycle, allows for reconstructing $X_\mathrm{max}$ from the EAS footprint using machine learning techniques. Using data recorded over 20 years, we present an analysis of the $X_\text{max}$ measurements by the SD and FD. In particular, we show that the UHECR mass composition evolution excludes a large proton abundance.
    
    Ponente: Berenika Čermáková (Karlsruhe Institute of Technology)
    
    TeVPA_05_11_2025.pdf
  - 15:45
    
    The CORSIKA 8 cascade simulation framework 15m
    
    CORSIKA 8 is a modern Monte-Carlo simulation framework for particle showers in air and dense media. It is designed as a modular and modern C++ framework, providing the flexibility that is needed for current and future astroparticle physics experiments. In addition to the standard hadronic interaction models for air showers, it also includes the next generation models EPOS-LHC-R and QGSJetIII as well as the well-known high-energy physics model Pythia 8. One particular highlight is the capability of the code to simulate showers in inhomogeneous environments. This also extends to the calculation of radio emission and propagation through complex media that cannot be properly treated with other methods. In this contribution, we will discuss the design principles and give an overview of the models, assumptions and algorithms that are employed. We will also briefly review radio emission and propagation algorithms implemented in the code, including the "endpoint" formalism, numerical raytracing, and a new Green's function-based approach for a full-electrodynamics signal calculation provided by the "Eisvogel" package.
    
    Ponente: Philipp Windischhofer (University of Chicago)
    
    2025_11_05_C8.pdf
  - 16:00
    
    Bayesian Hierarchical Model for cross calibration of hybrid air shower detectors 15m
    
    Energy calibration in indirect air shower detection presents a challenging problem due to the impossibility of controlled laboratory validation. Traditionally, hybrid measurements combining fluorescence detectors (FD) and surface detectors (SD) have relied on calibrating the SD using FD data, assuming that fluorescence measurements closely reflect the calorimetric principle. However, SD energy estimations depend on approximate empirical relationships or Monte Carlo simulations, both of which require reliable extrapolation beyond the limited energy range covered by high-statistics FD observations. Crucially, systematic uncertainties in fluorescence yield, invisible energy fraction, atmospheric conditions, detection efficiency, mass composition dependence, and proxy variable reconstruction are often overlooked or oversimplified, potentially introducing biases into calibration results and subsequent analyses. In this work, we introduce an unbinned Bayesian Hierarchical Model capable of integrating detection uncertainties event-by-event, ensuring unbiased calibration and systematic error propagation. Using toy simulations, we illustrate how common simplifications lead to biased outcomes and quantify the impact of detection and systematic uncertainties on energy calibration accuracy at ultra-high energies.
    
    Ponente: Anton Prosekin (Institute of Physics, Academia Sinica, Taiwan)
    
    TeVPA2025_prosekin.pdf
- 14:30 → 16:15
  Dark Matter: Indirect Detection: Indirect messengers Room 3.1+3.2 (ADEIT)
  
  Room 3.1+3.2
  
  ADEIT
  
  Moderador: Christopher Dessert (Flatiron Institute)
  - 14:30
    
    Invited: Searches for Dark Matter with KM3NeT 15m
    
    This contribution presents the latest searches for dark matter with the KM3NeT neutrino telescope. Indirect searches for neutrinos from dark matter annihilations primarily probe weakly interacting massive particles (WIMPs). The largest flux is expected from WIMP annihilations in celestial objects with a large density of dark matter, such as the Galactic Centre and the Sun. In this work, searches for annihilations in the Galactic Centre are performed in the 50 GeV/c2−100 TeV/c2 mass range, for a representative set of annihilation channels. The low energy detector, KM3NeT/ORCA, is used to probe WIMP annihilations in the mass range up to 1 TeV/c2, while the higher energy detector, KM3NeT/ARCA, probes heavier masses. The ORCA data consists of data sets recorded with 6, 10, and 11 detection lines, totaling around 750 days of livetime. The ARCA data set consists of data recorded with 19 and 21 detection units, totalling around 350 days of livetime. No significant excess was observed in any data set, resulting in constraints on the WIMP pair-annihilation cross section across the probed mass range.
    
    Ponente: Adrian Šaina (IFIC, CSIC-UV)
    
    Saina_TeVPa_talk.pdf
  - 14:45
    
    CosmiXs: Cosmic messenger spectra for indirect dark matter searches 15m
    
    Antimatter cosmic rays and gamma rays are powerful probes for indirect dark matter (DM) detection. In this talk, I will present the CosmiXs framework, which provides state-of-the-art predictions for the energy spectra of cosmic messengers—antiprotons, positrons, gamma rays, neutrinos, and antideuterons—produced from DM annihilation or decay. The spectra are calculated using the state-of-the-art Vincia shower algorithm implemented in Pythia, incorporating QED and QCD radiation, as well as full electroweak corrections with spin correlations and off-shell effects. In particular, CosmiXs implements a novel Wigner-based coalescence model for antideuterons using the Argonne v18 wavefunction, validated against ALEPH data at the Z pole. This approach eliminates free parameters associated with coalescence and demonstrates that coalescence-related uncertainties are no longer the dominant limitation in theoretical predictions for the antideuterons spectrum. All results are tabulated for DM masses from 5 GeV to 100 TeV and a broad set of final states, enabling precise flux predictions for upcoming cosmic-ray experiments.
    
    Ponente: Mattia Di Mauro (INFN Torino)
    
    TeVPa Cosmixs Di Mauro.pdf
  - 15:00
    
    Richer Cosmic Ray Spectra from Expanding the Dark Matter Theoretical Landscape 15m
    
    The study of cosmic rays with indirect detection searches provides a powerful tool to test the properties of dark matter (DM), especially through their potential imprints on the injection spectra. Adopting a model-independent approach, we systematically explore the characteristics of cosmic ray injection spectra arising from DM scenarios exhibiting a richer phenomenology. Our analysis goes beyond conventional direct annihilation signals by incorporating additional processes, namely one-step cascade mechanisms such as one-step annihilation and one-step semi-annihilation. We examine in detail the unique spectral features associated with each channel and consider the impact of scenarios involving weighted combinations of these contributions. This general framework allows us to quantify how effective parameters such as DM and mediator masses, as well as the relative contributions of different channels, shape the resulting injection spectra. It also provides a foundation to reinterpret existing constraints from indirect detection experiments on direct annihilation within an extended parameter space that includes one-step processes. To support and motivate our analysis, we present a concrete model in which a scalar DM candidate is stabilized by a non-Abelian symmetry and interacts with the visible sector through an axion-like particle. This setup naturally accommodates the coexistence of all three types of interactions.emphasized text
    
    Ponente: Tommaso Sassi (University of Padova, INFN Padova)
    
    Sassi_Richer_cosmic_ray_spectra.pdf
  - 15:15
    
    Cosmic ray antihelium in the Galaxy 15m
    
    The creation of anti-nuclei in the Galaxy has been discussed as a possible signal of exotic production mechanisms such as primordial black hole evaporation or dark matter decay/annihilation in addition to the more conventional production from cosmic-ray interactions. Tentative observations of cosmic-ray andideuteron and antihelium by the AMS-02 collaboration have re-energized the quest to use antinuclei to search for physics beyond the standard model.
    
    In this talk, we show state-of-art predictions of the antinuclei flux from both cosmic-ray interactions with the interstellar medium and standard dark matter annihilation models from combined fits to high-precision antiproton data as well as cosmic-ray nuclei measurements. Astrophysical mechanisms can explain the amount of antideuteron events detected by AMS-02, while their antihelium production lies far below the sensitivity of this experiment. In turn, standard dark matter models could potentially produce the detected antideuteron and antihelium-3 events, but the production of any detectable antihelium-4 flux would require exotic physics. We also present prospects for detection of these antinuclei by future detectors, such as GAPs and ALADInO.
    
    Ponente: Pedro De la Torre Luque (Universidad Autónoma de Madrid & Institute of theoretical physics (IFT-UAM))
    
    TeVPA_Antinuclei_DelaTorreLuque.pdf
  - 15:30
    
    Antinuclei production from dark matter via weakly decaying b-hadrons 15m
    
    In this talk, we present a tuning of PYTHIA and a coalescence model that leads to realistic predictions of antinuclei production. This tuning is validated against LEP data including the fragmentation function of $b$-quarks into into $b$-hadrons, which is crucial for determining the $\bar{\Lambda}_b^0$ multiplicity. The coalescence model is tuned to ALICE data for the $\overline{\text{D}}$ and ${}^3\overline{\text{He}}$ spectra. We obtain a branching ratio for the production of ${}^3\overline{\text{He}}$ from $\bar{\Lambda}_b^0$ decays that is consistent with the recent upper limit measured by LHCb. In the end, we find that the contributions of $\overline{\text{D}}$ and ${}^3\overline{\text{He}}$ from dark matter via $\bar{\Lambda}_b^0$ decays are negligible compared to prompt production, challenging previous claims in the literarure.
    
    Ponente: Jordan Koechler (INFN Turin)
    
    2025_Antinuclei_TeVPA.pdf
  - 15:45
    
    Cosmic antinuclei from primordial black holes 15m
    
    In this talk, we present our recent work on cosmic antimatter signatures from primordial black holes (PBHs). Light primordial black holes may have formed in the early Universe, and could contribute to the dark matter content of our Galaxy. Their Hawking evaporation into particles could lead to the production of antinuclei, which propagate and arrive at Earth as cosmic rays with a flux peaked at GeV energies. We revisit here the antiproton and antideuteron signatures from PBH evaporation, relying on a lognormal PBH mass distribution, state-of-the-art propagation models, and an improved coalescence model for fusion into antideuterons. Our predictions are then compared with AMS-02 data on the antiproton flux. We find that the AMS-02 antiproton data severely constrain the Galactic PBH density, setting bounds that depend significantly on the parameters of the lognormal mass distribution, and that are comparable to or slightly stronger than bounds set from diverse messengers. We also discuss prospects for future detection of antideuterons. Given the bounds from AMS-02 antiproton data, we predict that if antideuterons were to be measured by AMS-02 or GAPS, since the secondary contribution is subdominant, they would clearly be a signal of new physics, only part of which could, however, be explained by PBH evaporation.
    
    Ponente: Lorenzo Stefanuto (Università di Torino)
    
    TeVPA_Stefanuto_25f.pdf
  - 16:00
    
    Cosmic-ray cooling by dark matter in astrophysical jets 15m
    
    Astrophysical jets from powerful active galactic nuclei (AGN) have recently been proposed as promising probes of dark matter (DM) in the sub-GeV mass range. These jets accelerate cosmic rays (CRs) to very high energies, which can then interact with their environments to produce multiwavelength (MW) emission ranging from radio frequencies to TeV $\gamma$ rays. If DM consists of light particles, their interactions with CRs could introduce an additional cooling mechanism, altering the expected MW emission.
    In this talk, I will discuss an analysis of the MW spectrum of Markarian 421—a well-studied AGN—using a multizone leptonic jet model that includes interactions between CR electrons and DM particles. I will describe the uncertainties in the astrophysical jet dynamics, which have previously been neglected when constraining the CR–DM interactions. I will demonstrate a strong degeneracy between the particle acceleration efficiency in the jets and the DM–electron cross-section $\sigma_\text{DM-e}$, where lower acceleration efficiencies yield tighter constraints on $\sigma_\text{DM-e}$. Assuming a maximal efficiency of 10%, I will present 5$\sigma$ upper limits on $\sigma_\text{DM-e}$ for various DM masses, and compare these limits with previous estimates based on a fiducial AGN emission model.
    
    Ponente: Marco Chianese (Scuola Superiore Meridionale & INFN)
    
    TeVPA25_Chianese.pdf
- 14:30 → 16:15
  Gamma Rays: Extragalactic Salón de Actos (ADEIT)
  
  Salón de Actos
  
  ADEIT
  
  Moderador: Lea Heckmann (APC Paris CNRS)
  - 14:30
    
    The VERITAS TeV AGN Catalog 15m
    
    VERITAS is one of the world’s most sensitive very-high-energy (VHE; E > 100 GeV) gamma-ray observatories. Around half of its good-weather observations were targeted on active galactic nuclei (AGN). We present the recent efforts to reprocess the historical archive of VERITAS and produce a standardized, first VERITAS TeV AGN Catalog, and announce several new detections by VERITAS of AGNs at TeV energies.
    
    Ponente: Juan Escudero Pedrosa (Harvard-Smithsonian Center for Astrophysics)
    
    veritas_tev_agn_catalog_tevpa2025_jescudero.pdf
  - 14:45
    
    Spectro-Polarimetric Observations of TeV sources (SPOTS) 15m
    
    Blazars are a subclass of active galactic nuclei in which the relativistic jet-component aligns closely with the observer’s line of sight. Due to this viewing geometry, the observed emission is dominated by the highly Doppler boosted non-thermal jet emission which originates from the jet. At optical/UV wavelengths the emission is produced by leptonic synchrotron emission from relativistic electrons in the jet, with an underlying thermal contribution to the emission arising from the accretion disc, broad-line region, dust torus, and host galaxy itself. Polarization measurements at optical wavelengths provide an important diagnostic by which to disentangle the polarized non-thermal emission from the thermal (unpolarized) contribution, placing better constraints on the underlying non-thermal population. In 2023 November a long-term monitoring campaign was launched to perform Spectro-Polarimetric Observations of TeV sources (SPOTS), using the Southern African Large Telescope (SALT). The current sample consists of 12 HBLs and 2 FSRQs. The SPOTS project aims to find trends in the spectropolarimetric behaviour of TeV blazars, and how it connects to the high energy emission. During the observing period none of the blazars showed significant flaring at gamma-ray energies and we present here the results from the first two years of observations, considering the sources in the quiescent state. This will be used to investigate the nature and evolution of their jets, modelling their polarization and SEDs, and will be compared to previous surveys.
    
    Ponente: Brian van Soelen (University of the Free State)
    
    vanSoelen_TevPA.pdf
  - 15:00
    
    High energy emission of cosmic messengers from galaxy clusters 15m
    
    We explore the high-energy emission of cosmic messengers from galaxy clusters hosting active galactic nuclei (AGNs) such as Perseus. The main objective is to distinguish the emission from the central source, such as NGC $1275$, from the diffuse emission. Due to high magnetic field and large size of clusters, CRs with energy $\leq 10^{18}$ eV can be confined within these structures over cosmological time scales, and generate secondaries, including neutrinos and gamma-rays, through interactions with the background gas and photons. We employ three-dimensional cosmological magnetohydrodynamical simulations of structure formation to model the turbulent intracluster medium (ICM). To study the propagation of CRs in intracluster medium (ICM) and intergalactic medium, multi-dimensional Monte Carlo simulations are conducted, considering all relevant photohadronic, photonuclear, and hadronuclear interactions. By comparing our results with the existing upper limits from IceCube and LHAASO as well as the sensitivity of CTA, we predict that these observatories could potentially establish a new class of astrophysical sources capable of emitting high-energy multi-messenger signals. In addition, we computed the contribution from clusters across redshifts to the diffuse neutrino and gamma-ray background.
    
    Ponente: Saqib Hussain (University of Nova Gorica)
    
    TeVPA-2025_Saqib.pdf
  - 15:15
    
    Time-Dependent Leptonic Modeling of the High-Redshift Blazar 4C +01.02 Using Multiwavelength Observations 15m
    
    Active galactic nuclei (AGNs) are powered by accretion onto supermassive black holes (SMBHs), yet the mechanisms governing their energy output and the growth of SMBHs, particularly at high redshift, remain incompletely understood. Blazars, a subclass of AGNs with relativistic jets oriented close to our line of sight, are detectable across the electromagnetic spectrum, from radio to gamma rays, even at cosmological distances due to Doppler boosting. The blazar 4C +01.02 is located at a high redshift z=2.107 and it is a flat spectrum radio quasar (FSRQ). In this work, we investigate a detailed long-term spectral and temporal analysis of 4C +01.02 using multiwavelength observations from Fermi-LAT, Swift-XRT, and Swift-UVOT, interpreted within the framework of a time-dependent one-zone leptonic model. Our analysis aims to characterize the variability behavior of the source in both flaring (Dec 2014-Sep 2017 & May 2020-Sep 2023) and quiescent states (Aug 2008-Dec 2014 & Sep 2017-May 2020) and to constrain key physical parameters of the emission region. We first model the time-averaged spectral energy distributions (SEDs) by solving the time-dependent Fokker–Planck equation for the electron population under steady-state conditions. Subsequently, we introduce perturbations in parameters such as the magnetic field strength, electron injection luminosity, and electron spectral index to simulate transitions between quiescent and flaring states. These variations allow us to compute time-dependent SEDs and multi-band light curves (optical, X-ray, and gamma-ray), facilitating a comparison with observational data. A black hole mass of approximately $M_{\mathrm{BH}} = 5 \times 10^{9}\ M_\odot$ and a magnetic field strength of B ≈ 0.15 G, are used to successfully reproduce the broadband spectral energy distributions (SEDs) consistent with the multiwavelength observational data. Furthermore, the model derives the characteristics of the relativistic electron energy distributions and magnetic field strength. Thus, the modeling of detailed broadband spectral energy distributions (SEDs) during different flaring and quiescent states reveals the physics of particle acceleration processes and radiative mechanisms in relativistic AGN jets.
    
    Ponente: Shruti Mukherjee (The University of Free State)
    
    Time dependent modeling of FSRQ 4C+01.02.pdf
  - 15:30
    
    A Systematic Search for Blazar QPOs: Connecting Jet Variability to Gravitational Wave Sources 15m
    
    Blazars show variability across the entire electromagnetic spectrum and over a wide range of timescales. In some cases, characteristic emission patterns have been observed, such as the multi-year modulation detected in PG 1553+113. Quasi-periodic oscillations (QPOs) can arise from various astrophysical mechanisms, including jet precession, accretion disk instabilities, and supermassive binary black holes (SMBBHs). While the latter is a particularly compelling possibility, potentially linking galaxy mergers and gravitational wave progenitors to jet physics, the other scenarios also offer valuable information about the physical processes governing blazar variability, which remain poorly understood. In this work, we apply Singular Spectrum Analysis (SSA) to a large sample of Fermi-LAT blazars to systematically search for QPOs. SSA decomposes the signal into trend, oscillatory, and noise components, allowing robust detection of periodic features and construction of forecasting models. We identify 46 QPO candidates, including 25 previously unreported, representing the largest sample to date and enabling the first steps toward population-level statistical analyses of these phenomena. By identifying promising candidates and exploring their relevance within the broader context of multi-messenger astrophysics, this study establishes a foundation for future investigations into the physical origins of blazar variability and the potential connection to gravitational wave sources.
    
    Ponente: Alberto Domínguez (UCM & IPARCOS)
    
    TeVPA 2025- A Systematic Search for Quasi-Periodic Oscillations in Gamma-Ray Blazars using Singular Spectrum Analysis (1).pdf
  - 15:45
    
    Multi-wavelenght view of 3C 279 during the 2017-2018 EHT campaigns including an unprecedented gamma-ray flare 15m
    
    Spinning super-massive black holes at the centers of galaxies can launch powerful magnetized jets. 3C 279 is an archetypal blazar with a prominent radio jet that undergoes broadband emission variability. In April 2017 and April 2018, the Event Horizon Telescope (EHT) observed 3C 279 with an unprecedented angular resolution of 20 micro-arcseconds. In parallel, an extensive quasi-simultaneous multi-wavelength (MWL) campaign was conducted using both ground- and space-based observatories, covering frequencies from radio wavelengths to the TeV energy range. Here, we present preliminary results from the first two EHT-MWL observational campaigns, including the detection of a record-breaking gamma-ray flaring episode. Additionally, we provide initial interpretations based on the modeling of 3C 279's time-variable broadband emission and polarization using the Turbulent Extreme Multi-Zone numerical framework.
    
    Ponente: Giacomo Principe (INFN Trieste - University of Trieste)
    
    EHT_MWL_3C279_TevPa2025.pdf
  - 16:00
    
    Investigating the morphology and polarisation of kiloparsec-scale AGN jets with hybrid relativistic magnetohydrodynamic simulations 15m
    
    Radio-loud Active Galactic Nuclei (AGN) produce relativistic jets that are among the most energetic structures in the universe. These jets emit radiation across most of the electromagnetic spectrum, with their Spectral Energy Distribution (SED) typically exhibiting a double hump structure. The lower energy part of the SED is dominated by synchrotron emission from non-thermal electrons in the jet. Observations of AGN jets have also revealed complex, time-dependent morphologies that span vast length scales. To understand the morphology, dynamics, and evolution of these jets, it is essential to model their physical properties, such as density, energy and magnetic field. This study uses the PLUTO code to perform 3D relativistic magnetohydrodynamic (RMHD) simulations of kiloparsec-scale jet morphologies. The resulting morphology is investigated for three different jet velocities: a relativistic, mildly relativistic, and non-relativistic case. The synchrotron emission is modelled for each simulation using Lagrangian particles that represent the non-thermal electron population. The electron spectrum is evolved over time, accounting for effects such as diffusive shock acceleration and radiative cooling. A post-processing ray-tracing code is used to generate intensity maps and polarisation vectors by integrating the emission coefficients of each simulation cell along arbitrary lines of sight. The code accounts for both relativistic effects as well as light travel time. The results reveal emission features corresponding to recollimation shocks within the jet beam, which in some cases produce multiple bright components along the jet axis. Additionally, it is shown that magnetic filaments in the jet cocoon can reproduce filamentary emission similar to that observed in the lobes of FR II-type radio galaxies.
    
    Ponente: Izak van der Westhuizen (University of the Free State)
    
    TEVPA2025_VDWESTHUIZENIP.pdf TEVPA2025_VDWESTHUIZENIP.pptx
- 14:30 → 16:15
  Gamma Rays: Galactic Salón de Grados (ADEIT)
  
  Salón de Grados
  
  ADEIT
  
  Moderador: Emma de Oña Wilhelmi (Deutsches Elektronen-Synchrotron DESY)
  - 14:30
    
    Results of the long-term campaign on Cygnus X-3 with the MAGIC telescopes 15m
    
    Cygnus X-3 is a microquasar consisting of a compact object of unknown nature and a Wolf-Rayet star, which orbit each other with a very short period of 4.8 hours. The compact object launches powerful jets that are an excellent site for particle acceleration up to relativistic energies. The presence of these relativistic particles, combined with the proximity to the star and its high luminosity, makes the conditions in the source very favorable for inverse Compton scattering of stellar photons by the jet electrons, resulting in gamma-ray emission. Cygnus X-3 has been detected in a broad frequency range, from radio to gamma rays above 100 MeV, although it has never been confirmed as a very-high-energy (VHE; above 100 GeV) gamma-ray emitter. Studies of microquasars in gamma rays have recently become a hot topic in the community after the LHAASO detection of four microquasars above 100 TeV, establishing these sources as potential contributors to the Galactic cosmic-ray spectrum at energies above the PeV.
    Due to the scientific interest of the source, the MAGIC telescopes have observed Cygnus X-3 in the VHE band for more than a decade. In this contribution, we present a long-term analysis of 130 h collected by MAGIC between 2013 and 2024. This represents the largest available dataset (in both exposure and time coverage) at VHE to date, resulting in the strongest VHE upper limits of the source between 100 GeV and a few TeV. Both the temporal and spectral constraints of Cygnus X-3 during this 11-year period will be interpreted within the multi-wavelength context, providing meaningful constraints on the source properties based on its (lack of) emission in gamma rays at different energies.
    
    Ponente: Luis Barrios-Jiménez (Instituto de Astrofísica de Canarias)
    
    Cyg_X-3_TeVPA2025.pdf
  - 14:45
    
    Study on Gamma ray-binaries with the LHAASO data 15m
    
    Gamma-ray binaries are rare stellar systems where a compact object interacts with a massive companion star, producing high-energy emission in the MeV–TeV range. Leveraging the sensitivity of LHAASO’s WCDA and KM2A detectors, we analyze multiple key systems, including HESS J0632+057, PSR J2032+4127, GRS 1915+105, SS 433, LS 5039, and LS I +61 303. These sources display diverse behaviors such as orbital-phase-dependent variability, relativistic jets, and wind-driven interactions.
    In total, six binary candidates have been identified in the LHAASO northern sky map. The morphology and energy spectra of all these sources have been systematically modeled. Notably, flaring activity has been observed during the orbital phases of LS I +61° 303 and HESS J0632+057, highlighting dynamic particle acceleration processes in these systems.
    Our study demonstrates LHAASO’s capability to resolve both spectral and temporal features with high significance, offering deeper insight into the mechanisms driving gamma-ray emission in compact binary environments.
    
    Ponente: Mariam Hasan (IHEP)
  - 15:00
    
    Orbital Modulation of Gamma Rays up to 100 TeV from LS 5039 15m
    
    Gamma-ray binaries are among the most extreme accelerators in the Galaxy, capable of producing photons at TeV energies. LS 5039, a well-studied high-mass X-ray binary, is one of the few systems known to emit modulated TeV gamma rays. We report the detection of orbital modulation in gamma rays from LS 5039 up to 100 TeV using over 2800 days of observations with the High-Altitude Water Cherenkov (HAWC) Observatory. The emission extends beyond 200 TeV during inferior conjunction, with no evidence of a spectral cutoff, and shows a significant flux difference between superior and inferior conjunction phases. We also find a hint of modulation above 100 TeV. These observations suggest that particle acceleration occurs deep within the binary system, where absorption from stellar photons is expected. While a leptonic origin would require extremely efficient acceleration of electrons to ~200 TeV under low magnetic fields, a hadronic scenario involving PeV protons interacting with dense stellar wind material or X-ray radiation fields provides a more natural explanation. Our results position LS 5039 as a candidate Galactic PeVatron and motivate future multi-messenger searches, including high-energy neutrinos.
    
    Ponente: Miguel Mostafa (Temple University)
    
    mostafa-HAWC-TeVPA2025.pdf
  - 15:15
    
    Detection of very-high-energy gamma-ray emission from Eta Carinae during its 2020 periastron passage 15m
    
    The binary system Eta Carinae is a unique laboratory to study particle acceleration processes under a wide range of conditions. Particles are thought to be accelerated at shocks forming in the wind collision region. Eta Carinae has been firmly established as a source of high-energy (HE) and very-high-energy (VHE) gamma-rays in Fermi-LAT and H.E.S.S. data in the last decade. With its highly eccentric orbit lasting 5.5 years, the periastron passage of the two stars is extremely close, making it an intriguing time interval to probe the underlying acceleration processes within the system.
    The 2020 periastron was the first periastron passage visible for the full 5-telescope H.E.S.S. array and was therefore monitored with an extensive observation campaign spanning the phase range from 0.97 to 1.05. This led to the detection of VHE emission above 130 GeV close to and during the periastron passage ( H.E.S.S. Collaboration, 2025).
    We report on the spectral and temporal characteristics of this signal. Together with previous and follow-up observations, a VHE light curve sampling one full orbit is presented. Modelling the combined VHE and HE spectrum, we can constrain the gamma-ray emission region and the emission can be assigned to the acceleration of protons up to energies of at least several TeV inside the system.
    
    Ponente: Simon Steinmassl (Max Planck Institut für Kernphysik)
    
    etacar_pres_tevpa.pdf
  - 15:30
    
    A new orbital solution for HESS J0632+057 and modelling the effect of the Be discs on the emission from gamma-ray binaries 15m
    
    Gamma-ray binaries produce the majority of their multi-wavelength non-thermal emission at energies >1 MeV. These systems consist of an O/Be star and a compact object, which has been detected as a neutron star in 3 of the 9 systems. It is largely understood, then, that the VHE non-thermal emission in these systems originates in a stand-off shock that is produced when the stellar wind and/or disc of the O/Be companion collides with the relativistic pulsar wind from the young neutron star.
    The Be gamma-ray binary HESS J0632+057 has a ~317.3 d orbital period and displays a double-peaked profile in both the X-ray and TeV lightcurves, which is believed to be due to the pulsar crossing/interacting with the circumstellar disc, similar to what is observed in the other Be gamma-ray binary systems. We report on the new orbital solution for this system, obtained from optical spectroscopic data obtained with SALT which will allow for a simpler interpretation of the two peaks in the non-thermal emission. Furthermore, we investigate the impact of the disc on the optical as well as high energy emission with the implementation of a toy-model of the circumstellar disc in these systems.
    
    Ponente: Natalie Matchett (University of the Free State)
    
    Matchett_TEVPA2025.pdf
  - 15:45
    
    Discovery of TeV emission from the PWN of PSR J0855-4644 15m
    
    At the edge of the Galactic supernova remnant (SNR) Vela Junior lies the pulsar PSR J0855-4644. Pulsars are among the most efficient particle accelerators in our Galaxy, making the study of this region of interest. PSR J0855-4644 has remarkable X-ray and radio features, revealing a pulsar wind nebula (PWN) structure along with a bow shock nebula. PSR J0855–4644 stands out as one of the highest Ė/d$^{2}$ pulsars from which no GeV gamma-ray pulsations have been detected, despite its proximity (<900 pc), high spin-down luminosity (>10$^{36}$ erg/s), and jet-like structures. It lies in a complex environment near the SNR shock, offering a unique opportunity to study the evolution of the PWN and particle acceleration physics.
    In this contribution, we present a full forward-folding analysis of data from the H.E.S.S. gamma-ray telescopes to announce the discovery of a TeV gamma-ray counterpart of the PWN of PSR J0855-4644. This is possible from the substantial on-source livetime combined with advanced 3D analysis and modeling techniques, allowing the emission in the Vela Junior region to be resolved into distinct components. For the first time, we are able to disentangle the emission from the PWN from the supernova remnant emission in part due to its significantly different gamma-ray spectrum (power law index <2) extending up to tens of TeV. We present the PWN very-high-energy spectrum and morphology and discuss the object multi-wavelength characteristics in the landscape of PWN.
    
    Ponente: Kirsty Feijen (Astroparticule et Cosmologie Laboratoire)
    
    TeVPA_Discovery_VelaJrPWN_v2.pdf
  - 16:00
    
    Variability of non-thermal emission from supernova remnants induced by reflected shocks 15m
    
    Majority of supernova remnants expand into a complex environment of the stellar wind bubble blown up either by their progenitor or their companion star, where forward shock might interact with various density inhomogeneities. Such interactions would cause formation of fast reflected shocks propagating back and forth between the forward shock, the contact discontinuity in the interior of the remnant and the reverse shock. Current investigations of particle acceleration at supernova remnant shocks usually ignore the complexity of the hydrodynamic picture. On the other hand, rapidly improving observational facilities allow now for precise spatially and temporally resolved measurements that do not always agree with simplified modelling. It is intuitive that many irregularities as compared to the classical view of non-thermal emission from supernova remnants could be connected to the particulars of the environment. This work investigates the impact of the interaction of a reflected shock with a forward shock of an SNR on the particle acceleration in the source and examines observational signatures that could potentially arise from such interactions. We demonstrate that such interaction could lead to significant variability of the X-ray and gamma-ray flux on yearly time scale accompanied with the change of the spectral shape.
    
    Ponente: Iurii Sushch (CIEMAT, Spain)
    
    snr_FSRS_tevpa2025_sushch.pdf
- 14:30 → 16:15
  Neutrinos: Future detectors Room 1.1+1.2 (ADEIT)
  
  Room 1.1+1.2
  
  ADEIT
  
  Moderador: Claire Guépin Detrigne (CNRS, LUPM)
  - 14:30
    
    The IceCube Upgrade and IceCube-Gen2: Next Steps in Neutrino Astrophysics 15m
    
    The IceCube Neutrino Observatory at the geographic South Pole has achieved key milestones in neutrino astrophysics, including the discovery of a high-energy astrophysical neutrino flux and the correlation of neutrinos with flaring blazars and Seyfert galaxies. Building on this success, the IceCube Upgrade is scheduled for completion during the 2025/26 Antarctic summer season. It will add seven new strings of densely packed optical sensors, primarily near the bottom of the detector, significantly improving event reconstruction and the selection efficiency of atmospheric neutrinos down to a few GeV. This will provide a unique opportunity to access neutrino oscillations and high-precision measurements of tau neutrino appearance. The Upgrade’s extensive associated calibration program will enhance our understanding of the glacial ice’s optical properties and detector response, thereby improving the angular resolution of neutrino events. These improvements will further benefit IceCube’s archival data once they are retroactively applied. In addition to its immediate scientific goals, the Upgrade lays critical groundwork for IceCube-Gen2 by expanding our knowledge of glacial ice and enabling in situ studies of over ten Gen2 optical module prototypes. IceCube-Gen2 aims to increase the instrumented volume to approximately 8 cubic kilometers of optical array, while also incorporating an expanded surface detector array and radio antennas.
    This contribution will present the status of the IceCube Upgrade ahead of the upcoming construction season, with a special focus on the calibration program and its foundational role in the Gen2 effort. Updates on IceCube-Gen2 will also be provided, highlighting the design and performance of the optical module arrays that will drive the next generation of discoveries in neutrino astrophysics.
    
    Ponente: Aya Ishihara (ICEHAP, Chiba University)
    
    Gen2_Upgrade_TeVPa2025_v2.pdf
  - 14:45
    
    The Radio Neutrino Observatory in Greenland (RNO-G) 15m
    
    The Radio Neutrino Observatory in Greenland (RNO-G) will be, upon completion, the largest cosmic neutrino telescope that uses the in-ice radio detection mechanism. RNO-G is also the first radio detector of its kind, with each station having a combination of antennas deployed at different depths, the so-called shallow and deep components. With this approach, it is expected that RNO-G will be able to uniquely identify the radio signals from Ultra-High-Energy (UHE) neutrinos in ice, separating them from a large background of man-made radio emission or similar radio emission from cosmic-ray air showers.
    
    This presentation will provide an overview of the RNO-G experiment, from the science case to the latest results from the collaboration.
    
    Ponente: Enrique Huesca Santiago (Deutsches Elektronen-Synchrotron (DESY))
    
    2025_TeVPA-RNOG_Overview.pdf
  - 15:00
    
    Status of the Radar Echo Telescope for Cosmic Rays 15m
    
    Situated near Summit Station, Greenland in 2023 and 2024, the Radar Echo Telescope for Cosmic Rays (RET-CR) experiment searched for radar echoes produced by reflections from in-ice cosmic-ray (CR) cascades. These secondary cascades are generated by energetic CR air showers impacting a high altitude ice sheet and depositing a portion of their energy into the ice. They can be detected with radar by illuminating the ice volume with a radio-frequency transmitter, and using receivers to record the radio signals scattered by the ionisation trails left in the wake of the cascades. A successful detection of an in-ice CR cascade will demonstrate the feasibility of the radar method, allowing it to be applied towards the detection of UHE cosmic neutrinos; the main goal of the Radar Echo Telescope (RET) collaboration. In this way, RET-CR is acting as a pathfinder experiment for the RET-N neutrino telescope, an experiment targeting PeV-EeV neutrinos to help provide insight into the highest energy astrophysical processes. In this work, we will discuss the radar detection method and the RET-CR experiment, focusing on the expected signal features and first data.
    
    Ponente: Isha Loudon (Université Libre de Bruxelles)
    
    StatusRET-CR_TeVPA_Iloudon.pdf
  - 15:15
    
    Prospects for UHE neutrino flavor measurements with PUEO 15m
    
    The Payload for Ultrahigh Energy Observations (PUEO) is a balloon-borne radio detector for neutrinos at energies above 1EeV, scheduled to fly over Antarctica in the austral summer of 2025/2026. Through the observation of radio signals from neutrino interactions in the Antarctic ice sheet, PUEO can achieve an effective detection volume that is unparalleled by other experiments.
    Charged leptons produced in these neutrino interactions can cause particle showers that emit distinct secondary radio signals. In this presentation we will show that PUEO is sensitive to these secondary signals and explore how they could be used to constrain the flavor of detected neutrinos.
    
    Ponente: Christoph Welling (University of Chicago/Pennsylvania State University)
    
    TevPA2025.pdf
  - 15:30
    
    The Pacific Ocean Neutrino Experiment 15m
    
    The IceCube Neutrino Observatory has discovered an extragalactic neutrino flux and observed neutrinos from the Milky Way. Even though two active galaxies, NGC 1068 and TXS 0506+056, are candidate neutrino sources, the classes of objects responsible for the extragalactic flux are not known. And the Milky Way flux should be a combination of yet to be identified individual sources as well as a diffuse flux due to cosmic ray propagation in the Galaxy. Understanding the galactic and extragalactic fluxes requires a new generation detector focused on precision measurements that provide significant improvements in angular resolution. In this talk, I will discuss the status and prospects of the Pacific Ocean Neutrino Experiment (P-ONE), located in the Cascadia basin off the west coast of Canada. By leveraging modern instrumentation and longer scattering length in seawater compared to Antarctic ice, a kilometer-scale P-ONE can increase the number of extragalactic sources by an order of magnitude and can probe realistic models for Galactic sources.
    
    Ponente: Ignacio Taboada (Georgia Institute of Technology)
    
    TeVPA_PONE_Taboada.pdf
  - 15:45
    
    Tracing Out the Neutrino Sky with TAMBO 15m
    
    The detection of high-energy astrophysical neutrinos by IceCube has opened a new window on our Universe. While IceCube has measured the flux of these neutrinos at energies up to several PeV, much remains to be discovered regarding their origin and nature. Currently, the discovery of point sources of neutrinos is hindered by atmospheric neutrino backgrounds; likewise, astrophysical neutrino flavor ratio measurements are limited by the difficulty of discriminating between electron and tau neutrinos.
    
    TAMBO is a next-generation neutrino telescope specifically designed to detect tau neutrinos in the 100 TeV to 1 EeV energy range at a fraction of the cost of traditional neutrino telescopes. The tau neutrino specificity enables the low-background identification of astrophysical neutrino sources, as well as tests of the flavor ratio of astrophysical neutrinos. Additionally, the high-energy reach of TAMBO will allow us to probe models of cosmogenic neutrino production. TAMBO will comprise an array of water Cherenkov and plastic scintillator detectors deployed on the face of a deep valley, with its unique geometry facilitating the high-purity measurement of astrophysical tau neutrinos. In this talk, I will present the particle physics and astrophysics that TAMBO will study in the context of next-generation neutrino observatories. I will also provide an update on the status of detector construction.
    
    Ponente: Will Thompson (Harvard University)
    
    TAMBO TeVPA 2025.pdf
  - 16:00
    
    RES-NOVA: an observatory for supernova neutrinos and astroparticle physics 15m
    
    Core-collapse Supernovae (SN) release nearly all their binding energy as a burst of neutrinos of all three flavours. RES-NOVA addresses a major challenge in astroparticle physics by introducing a novel detection technique based on low-temperature calorimeters operated at the milliKelvin scale, exploiting Coherent Elastic Neutrino-Nucleus Scattering (CE$\nu$NS) as detection channel.
    CE$\nu$NS offers the major advantages of being equally sensitive to all $\nu$ flavours, with a cross-section $\sim10^4$ times higher than conventional neutrino detection channels.
    
    RES-NOVA aims to deploy the first ton-scale array of low-temperature calorimeters made from ultra-pure archaeological lead, which maximizes the CE$\nu$NS cross-section and enables the suppression of radioactive background. As a result, a compact (30 cm)$^3$ detector array features exceptional sensitivity, capable of surveying $\sim$90$\%$ of galactic SN and enabling precise SN neutrino measurements, independently of flavour oscillation uncertainties.
    
    Beyond supernova neutrino detection, RES-NOVA technology offers promising applications in solar neutrino physics, Dark Matter searches, and axion detection. We will present recent experimental progress, including first prototype results and updated sensitivity projections.
    
    Ponente: Simone Quitadamo (Università di Milano-Bicocca)
    
    TeVPA2025_ResNova.pdf
- 16:15 → 16:45
  
  Coffee Break 30m ADEIT
  
  ADEIT
- 16:45 → 18:30
  Cosmic Rays Room 2.1+2.2 (ADEIT)
  
  Room 2.1+2.2
  
  ADEIT
  
  Moderador: Arjen van Vliet (DESY Zeuthen)
  - 16:45
    
    Measurement of the Cosmic-Ray Proton Spectrum with MAGIC 15m
    
    Recent high-precision measurements of cosmic rays have revealed spectral features that are not justified by a simple power-law behavior. These deviations provide valuable insights into cosmic ray acceleration, propagation, and injection mechanisms, including possible contributions from nearby sources. Among the various cosmic ray species, protons—being the most abundant and least charged nuclei—serve as a key probe for testing these theoretical scenarios due to the reduced complexity in modeling their acceleration and propagation. In this study, we present a measurement of the cosmic-ray proton spectrum in the 1–500 TeV energy range, derived from archival MAGIC data originally collected for gamma-ray observations. The analysis is based on neural networks for both energy reconstruction and event classification. Notably, this represents the first measurement of the proton spectrum in this wide energy range using the ground-based imaging atmospheric Cherenkov technique. The results provide a complementary perspective to space-based experiments and contribute to a more complete understanding of cosmic-ray spectra at the highest energies accessible with current instrumentation.
    
    Ponente: Miguel Molero (IAC)
    
    ProtonFlux_TeVPa2025_MMolero.pdf
  - 17:00
    
    Discriminating Heavy Cosmic Rays at TeV Energies with MAGIC via Direct Cherenkov Emission 15m
    
    Iron nuclei are the most abundant heavy component of cosmic rays and provide critical insight into their astrophysical origin and propagation. Ground-based IACT telescopes have demonstrated the effectiveness of using the direct Cherenkov light emission of heavy atomic nuclei high-up in the atmosphere for measuring the iron spectrum in the multi-TeV energy range. Building on previous results from H.E.S.S. and VERITAS, we present a measurement of the cosmic-ray iron spectrum above 10 TeV using the MAGIC telescopes. By detecting early Cherenkov emission prior to shower development from primary iron nuclei, we achieve effective separation from lighter elements. Our results are consistent with existing measurements.
    
    Ponente: Salvatore Mangano (CIEMAT)
    
    MAGICCRironfinal.pdf
  - 17:15
    
    Cosmic-Ray Anisotropy at PeV Energies with IceTop 15m
    
    We present preliminary results from a study of the anisotropy in cosmic-ray arrival directions as observed by IceTop, the surface array component of the IceCube Neutrino Observatory. IceTop is primarily sensitive to cosmic rays in the PeV energy range, providing complementary data to and extending beyond recently published results from IceCube’s in-ice component. This work uses 10 years of data collected between 2011 and 2022 to study the structure of cosmic-ray anisotropy in the Southern Hemisphere for four energy bins, with median energies from 300 TeV to 6.9 PeV.
    
    Ponente: Frank McNally (Mercer University)
    
    2025-11-007-TeVPA-2025-McNally.pdf
  - 17:30
    
    Energy-dependent Orbital Compton-Getting Dipole with IceCube Cosmic-Ray Muons 15m
    
    The Compton-Getting effect — an apparent dipolar anisotropy of cosmic rays generated by Earth's orbital motion around the Sun — serves as a known calibration source for cosmic-ray anisotropy studies. The amplitude of the Compton-Getting dipole depends on both the orbital speed and the mean spectral index of the cosmic-ray flux. It therefore provides an indirect method for studying the energy spectrum of cosmic rays. This work will report on a study of the spectral index of cosmic-ray induced muons as a function of energy using data collected over 12 years by IceCube in the 10 TeV to 100 TeV range.
    
    Ponente: Juan Carlos Díaz Vélez (University of Wisconsin-Madison)
    
    2025-11-006-TeVPA-2025-Díaz-Vélez.pdf
  - 17:45
    
    Comparison of the atmospheric muon flux in KM3NeT data with simulations using the data-driven Daemonflux model 15m
    
    Muons, created by the interactions of cosmic rays with the Earth's atmosphere, form the main component of the cosmic ray air showers which reach underwater or in-ice detectors such as KM3NeT and IceCube. Precise measurements of such muons can provide key insights into the properties of cosmic rays, and their interactions. The KM3NeT research infrastructure consists of two telescopes in the Mediterranean Sea, KM3NeT/ORCA, deployed at a depth of 2450 m off the coast of Toulon, France, and KM3NeT/ARCA, deployed at a depth of 3500 m offshore Capo Passero, Italy. This design provides a unique opportunity to measure the flux of atmospheric muons at two depths and locations. Exploiting this feature, the KM3NeT collaboration recently reported a comparison of the atmospheric muon flux between the data collected using six lines of KM3NeT/ORCA and six lines of KM3NeT/ARCA and simulations performed using CORSIKA. These Monte Carlo simulations are found to be significantly underestimating the event rates with respect to data, thus contributing to the phenomenon called the Muon Puzzle. In an attempt to resolve the global Muon Puzzle, a data-driven model has been developed to describe the atmospheric muon flux at sea level. In this study, the Daemonflux model is incorporated into the KM3NeT simulations. A significant improvement has been observed in the comparison between these simulations and the data collected using 21 lines of KM3NeT/ARCA and 13 lines of KM3NeT/ORCA. Furthermore, we also show a significant reduction in the systematic uncertainties on the simulations.
    
    Ponente: Venugopal Ellajosyula (INFN Genova)
    
    KM3NeT_TeVPA_Daemonflux.pdf
  - 18:00
    
    Ultra-High-Energy Photon Searches with the Pierre Auger Observatory: Constraints, Multi-messenger Synergies, and Future Prospects 15m
    
    The Pierre Auger Observatory, the largest air-shower detector in the world, provides unmatched exposure to photons with energies above 5 × 10¹⁶ eV. Its hybrid detection system - combining a surface detector array and fluorescence telescopes - enables the most stringent upper limits on the diffuse Ultra-High-Energy photon flux, achieved through advanced discrimination of photon-induced air showers and hadron-induced air showers. These limits, derived from nearly two decades of data, challenge theoretical models of cosmic-ray origins, including top-down scenarios and extreme astrophysical accelerators, and also highlight the significant capabilities of the Pierre Auger Observatory in the framework of multi-messenger astronomy at the highest energies. In this contribution, we present the latest Auger Observatory results on photon searches and review prior follow-up investigations of photons associated with gravitational wave events that LIGO/Virgo detected. Finally, we discuss the impact of AugerPrime, the upgrade of the Pierre Auger Observatory, on photon searches by further increasing the sensitivity, thus continuing to play a key role in gaining new insights on the most extreme phenomena in the Universe.
    
    Ponente: Chaitanya Priyadarshi (Instytut Fizyki Jadrowej PAN, Kraków)
    
    Auger_UHE_photons_Priyadarshi.pdf
  - 18:15
    
    Probing AGN jet structure with RMHD simulations: implications for VHE emission 15m
    
    The internal structure and dynamics of relativistic jets in active galactic nuclei (AGN) are central to understanding where and how particles are accelerated to very high energies. In particular, recollimation shocks and the turbulent regions they generate downstream can serve as natural sites for localized energy dissipation and non-thermal particle energization. Using high-resolution 2D and 3D relativistic magnetohydrodynamic (RMHD) simulations with the PLUTO code, we explore how the jet’s macroscopic structure—shaped by external confinement, pressure gradients between the jet and its environment, and the structure of the magnetic field—governs the development of time-dependent features that can efficiently accelerate particles. Our results provide a physically grounded framework connecting the large-scale dynamics of AGN jets to their spectral, polarization, and variability signatures in the very-high-energy (VHE) regime. This work offers new insights into the emission of high-energy-peaked blazars, highlighting the importance of global jet modeling for interpreting VHE observations.
    
    Ponente: Stella Boula (INAF-OAB)
    
    Boula_Valencia.pptx
- 16:45 → 18:30
  Dark Matter: Indirect Detection: Photons I Room 3.1+3.2 (ADEIT)
  
  Room 3.1+3.2
  
  ADEIT
  
  Moderador: Nirmal Raj (Indian Institute of Science)
  - 16:45
    
    Invited: Was there a 3.5 keV line? 15m
    
    The 3.5 keV line is a purported emission line observed in galaxies, galaxy clusters, and the Milky Way whose origin is inconsistent with known atomic transitions and has previously been suggested to arise from dark matter (DM) decay. I show why the line cannot arise from DM decay, and then describe work in which collaborators and I reanalyzed the datasets providing the bulk of the evidence for the 3.5 keV line. Surprisingly, we found a line in only one of those datasets; in the rest we found no evidence for a line, possibly due to the use of local optimization in earlier works. In the remaining dataset we present evidence for mismodeling that suggests the line is spurious. We conclude that there is no robust evidence for the existence of the 3.5 keV line. I finally discuss prospects for detecting X-ray lines with XRISM, a recently-launched telescope with 20 times better energy resolution than that of previous telescopes.
    
    Ponente: Christopher Dessert (Flatiron Institute)
    
    TeVPA_11052025.key TeVPA_11052025.pdf
  - 17:00
    
    20 GeV halo-like excess of the Galactic diffuse emission and implications for dark matter annihilation 15m
    
    Fifteen years of the Fermi Large Area Telescope (LAT) data in the halo region of the Milky Way (MW) are analyzed to search for gamma rays from dark matter annihilation. Gamma-ray maps within the region of interest (|l| < 60 deg, 10 < |b| < 60 deg) are modeled using point sources, the GALPROP models of cosmic-ray interactions, isotropic background, and templates of Loop I and the Fermi bubbles, and then the presence of a halo-like component is further examined. A statistically significant halo-like excess is found with a sharp peak around 20 GeV, while its flux is consistent with zero below 2 GeV and above 200 GeV. Examination of the fit residual maps indicates that a spherically symmetric halo component fits the map data well. The radial profile agrees with annihilation by the smooth NFW density profile, and may be slightly shallower than this, especially in the central region. Various systematic uncertainties are investigated, but the 20 GeV peak remains significant. In particular, the halo excess with a similar spectrum is detected even relative to the LAT standard background model, which does not depend on GALPROP or other model templates. The halo excess can be fitted by the annihilation spectrum with a mass m ∼ 0.5-0.8 TeV and annihilation cross section < sigma v > ~ (5-8)×10^{-25} cm^3s^-1 for the bb channel. This cross section is larger than the upper limits from dwarf galaxies and the canonical thermal relic value, but considering various uncertainties, especially the density profile of the MW halo, the dark matter interpretation of the 20 GeV ``Fermi halo'' remains feasible. The prospects for verification through future observations are briefly discussed.
    
    Ponente: Tomonori Totani (Univ. of Tokyo)
    
    totani_TeVPA2025.pdf
  - 17:15
    
    Prospects of MeV telescopes in probing weak-scale Dark Matter 15m
    
    Weak-scale Dark Matter (DM) particles annihilating into lepton-rich channels in the Galaxy not only produce $\gamma$-rays via prompt radiation, but also generate abundant energetic $e^\pm$, which subsequently emit through inverse Compton scattering or bremsstrahlung (collectively called `secondary-radiation photons'). While the prompt $\gamma$-rays concentrate at high-energy, the secondary emission falls in the MeV range, which a number of upcoming experiments (e.g., AMEGO, E-ASTROGAM and MAST) will be able to probe. I shall discuss the sensitivity of these future telescopes for weak-scale DM, focusing for definiteness on observations of the galactic center. I shall show that they have the potential of probing a wide region of the DM parameter space which is currently unconstrained, precisely thanks to the significant leverage provided by their sensitivity to secondary emissions. I shall also comment on astrophysical and methodological uncertainties, and compare with the reach of future high-energy gamma ray experiments.
    
    Ponente: Arpan Kar (LPTHE, CNRS, Sorbonne University)
    
    AKar_TeVPA_2025.pdf
  - 17:30
    
    A novel method for Forecasting and Recasting Dark Matter Annihilation Limits from Gamma-Ray Observations 15m
    
    We present a novel algorithm for both forecasting and recasting upper limits (ULs) on dark matter (DM) annihilation cross sections. The forecasting method relies solely on the instrument response functions (IRFs) to predict ULs for a given observational setup. The recasting procedure uses published ULs to reinterpret results for alternative DM models or channels, without requiring access to raw data or full analysis pipelines. We demonstrate its utility across a range of annihilation channels and apply it to several major gamma-ray experiments, including MAGIC, Fermi-LAT, and CTAO. Notably, we develop a recasting approach that remains effective even when the IRF is unavailable by extracting generalized IRF-dependent coefficients from benchmark channels. Through Monte Carlo simulations and comparison with published results, we validate the robustness and accuracy of our approach, achieving good agreement within statistical uncertainties. Our framework offers a powerful tool for reinterpreting existing gamma-ray limits and efficiently exploring the DM parameter space in current and future indirect detection experiments.
    
    Ponente: Giacomo D'Amico (Institut de Física d'Altes Energies (IFAE))
    
    Cast_DM_TeVPA.pdf
  - 17:45
    
    Indirect detection probes for Minimal Dark Matter 5plet 15m
    
    We critically reassess the Minimal Dark Matter model and propose novel indirect detection signatures. Specifically, we compute the photon flux associated with the originally proposed accidentally stable SU(2) 5-plet, arising from Dark Matter bound state formation and Sommerfeld-enhanced annihilations. Our analysis reveals several distinctive spectral features that constitute promising targets for gamma-ray searches. We then examine the constraints on the 5-plet from current FERMI-LAT observations of the Galactic diffuse emission, and evaluate the projected sensitivity of the upcoming Cherenkov Telescope Array (CTA) in observations of Dwarf Spheroidal Galaxies.
    
    Ponente: Giulio Marino (Università di Pisa & INFN Pisa)
    
    TeVPA.pdf
  - 18:00
    
    Looking for Dark Matter in the Unresolved Gamma-Ray Background through Cross-Correlations with Gravitational Tracers 15m
    
    Our understanding of the $\gamma$-ray sky has improved dramatically in the past decade, however, the unresolved $\gamma$-ray background (UGRB) still has a potential wealth of information about the faintest $\gamma$-ray sources pervading the Universe. Statistical cross-correlations with tracers of cosmic structure can indirectly identify the populations that most characterize the $\gamma$-ray background. In this study, we analyze the angular correlation between the $\gamma$-ray background and the matter distribution in the Universe as traced by gravitational lensing and galaxy clustering analyses, leveraging more than a decade of observations from the $\textit{Fermi}$-Large Area Telescope (LAT) and 3 years of data from the Dark Energy Survey (DES). We provide results obtained so far from both the lensing and galaxy clustering analyses, and discuss the potential composition of the UGRB, and what it could imply for WIMP DM searches. We also comment on the astrophysical nature of the UGRB through phenomenological and physical modelling. Using a 2-halo model approach, we find that in both cases (i.e, lensing and galaxy clustering), the cross-correlations are stronger for the 2-halo component, implying a stronger presence of the large-scale structure in the signal compared to point-like objects.
    
    Ponente: Bhashin Thakore (University of Turin and University of Amsterdam)
    
    TeVPA_2025_Bhashin_Thakore.pdf
  - 18:15
    
    Searching for Axion Dark Matter with Radio Telescopes 15m
    
    The QCD axion, originally proposed to resolve the strong CP problem, is also a compelling dark matter (DM) candidate. In strong magnetic fields, such as those surrounding neutron stars, axions can convert into photons, potentially generating detectable radio signals. This axion-photon coupling offers a unique avenue for experimental searches in a well-defined mass range. In this seminar, I will present an observational study using the Green Bank Telescope (GBT) to search for transient radio signals from axion-photon conversion. Focusing on the core of Andromeda, we employ the VErsatile GBT Astronomical Spectrometer (VEGAS) and the X-band receiver (8–10 GHz) to probe axions with masses between 33 and 42 μeV, achieving a mass resolution of 3.8 × 10^-4 μeV. We describe our observational strategy and analysis techniques, which reach an instrumental sensitivity of 2 mJy per spectral channel. While no candidate signals exceeding the 5σ threshold were detected, I will discuss future improvements, including expanding the search to additional frequency bands and refining theoretical models, to strengthen constraints on axion DM scenarios. Based on 2407.13060, 2011.05378, 2011.05377, and ongoing work.
    
    Ponente: Luca Visinelli (Università degli Studi di Salerno, Italy)
    
    TeVPA2025.pdf
- 16:45 → 18:30
  Gamma Rays: Extragalactic Salón de Actos (ADEIT)
  
  Salón de Actos
  
  ADEIT
  
  Moderador: Alberto Domínguez (UCM & IPARCOS)
  - 16:45
    
    Twelve Years of Multiwavelength Monitoring of PG 1553+113: Evidence for a Two-Zone SSC Emission 15m
    
    PG 1553+113 is a BL Lac object located at redshift z = 0.433. It is one of the most luminous extragalactic sources in the very-high-energy (VHE, E > 100 GeV) gamma-ray band, and it has been detected by all currently operating Imaging Air Cherenkov Telescopes (IACTs). A key feature of this source is the evidence of quasi-periodic modulation in high-energy (HE, E > 100 MeV) gamma rays detected by Fermi-LAT, with a period of about 2.2 years. Optical data also confirm a similar modulation pattern.
    In this contribution, we present a comprehensive dataset spanning over a decade of MAGIC observations, complemented by simultaneous multiwavelength data from instruments operating in other energy bands. Detailed analysis of intra-band correlations, complemented by a search for periodic emission, suggest that the emission mechanism may be described by using a two-zone synchrotron-self compton (SSC) model, with two distinct electron populations. The low-energy population is responsible for the emission in optical, UV and HE gamma-ray photons, while X-ray and VHE gamma rays are produced by an additional high-energy population. Very remarkably, in April 2019, PG 1553+113 exhibited its highest VHE flux ever recorded. To interpret the observed spectral energy distribution, we tested, for the first time, a two-zone SSC model. We will demonstrate how our model aligns with recent observational results and the resulting intra-band correlations.recent observational results and the resulting intra-band correlations.
    
    Ponente: Giuseppe Silvestri (University and INFN of Padova)
    
    GiuseppeSilvestri_TEVPA_PG1553.pdf
  - 17:00
    
    Search for VHE Short-Timescale Variability in PG 1553+113 15m
    
    PG 1553+113 is a high-frequency peaked BL Lac object with a redshift of 0.433, detected by the current generation of Imaging Atmospheric Cherenkov Telescopes up to approximately 1 TeV. Interestingly, the continuous gamma-ray light curve recorded by Fermi-LAT since 2008 has shown a periodic modulation of 2.18 ± 0.08 years at energies above 100 MeV and 1 GeV. Additionally, the source shows clear variability on a daily timescale across all bands. Recent XMM-Newton data revealed rapid variability in the X-ray band down to approximately 40 minutes. Periodicity and intra-day variability have not yet been detected at very high energies (VHE), i.e. above 100 GeV.
    
    Short-timescale (sub-hour) variabilities are key observables to probe the small spatial structures of the jet and provide important constraints to the size of the photon-emitting region in the jet. The first Large-Sized Telescope (LST-1) of the Cherenkov Telescope Array Observatory (CTAO), located at the Roque de los Muchachos in La Palma, Spain, provides a unique opportunity to study such phenomena due to its high sensitivity at low energies and its low energy threshold (down to about 20 GeV). In April 2023, a very bright flare from PG 1553+113 triggered LST-1 and multi-wavelength observation campaigns. In this study, we present the results of these observations, with a focus on the search for short-timescale variability in the VHE range. We characterized the variations in the observed flux of PG 1553+113 during a 4-hour observation conducted by LST-1, using different time variability significance estimators applied to the light curve.
    
    Ponente: Helena Luciani (University and INFN Trieste)
    
    PG1553_TeVPA_Valencia_2025.pdf
  - 17:15
    
    The Littlest Galaxies Shine All Too Softly: A Gamma-Ray Look at Dwarf AGN 15m
    
    We present the first gamma-ray study of X-ray selected AGN in dwarf galaxies, using 15 years of Fermi-LAT data. These low-mass systems likely host intermediate-mass black holes and offer a unique view into accretion and feedback in the faintest galactic nuclei, as well as a new window into the properties of dark matter. While no individual source is detected, a joint likelihood analysis of 74 eROSITA-selected dwarfs reveals an indication of a soft-spectrum excess. This marginal signal may point to low-efficiency jet or corona-driven gamma-ray emission, distinct from processes observed in their more massive AGN counterparts. We also consider dark matter annihilation in density spikes as a speculative but intriguing contributor to the soft gamma-ray signal. These results suggest that dwarf AGN, the littlest gamma-ray galaxies, may host new windows into both high-energy astrophysics and beyond-standard-model physics.
    
    Ponente: Milena Crnogorcevic (Stockholm University/OKC)
    
    tevpa2025.pdf tevpa2025.pptx
  - 17:30
    
    Investigation of the extreme activity of Mrk 501 in 2014 and of its intriguing TeV feature 15m
    
    Markarian 501 is a well know close by (redshift = 0.034) BL Lac object. It is categorized as a high-synchrotron peaked blazar (HSP; νpeak> 10^{16} Hz) with temporarily extremely high-synchrotron peaked behavior (EHSP; νpeak> 10^{17} Hz). The proximity of the source allows for the observations in the Very High Energy range (VHE; E> 100 GeV) by IACTs, such as the MAGIC telescopes. In 2014, the MAGIC collaboration organized a multiwavelength campaign, during which several flares in VHE and X-ray frequencies were observed. The source presented a similar extreme activity in 1997. Furthermore, a feature was located at ~3 TeV in the spectral energy distribution, and its origin is still discussed to this day. This study seeks to provide an alternative theoretical interpretation of the multiwavelength behaviour in 2014, investigating the appearance of this unique TeV feature in the same year.
    
    Ponente: João Gabriel Giesbrecht Formiga Paiva (Centro Brasileiro de Pesquisas Físicas)
    
    tevpa_conference_joao_paiva.pdf
  - 17:45
    
    Gamma rays from M87* 15m
    
    M87* is a particularly well-studied black-hole system, thanks to the wealth of spectral data and the ability to image its central region using VLBI techniques. We present a model of the broadband emission of this object, in which radiation from the millimetre to TeV range is explained by leptonic emission from the innermost accretion flow. The model is based on GRMHD simulations and takes into account the hybrid (thermal and non-thermal) electron energy distribution. After calibrating the model to reproduce mm-range measurements — in particular, the Event Horizon Telescope images — we determined the electron acceleration parameters capable of explaining the high-energy and very high-energy emission from the source.
    
    Ponente: Andrzej Niedzwiecki (Łodz ́ University)
    
    NiedzwieckiTEVPA.pdf
  - 18:00
    
    Search for cosmic-ray induced gamma-ray emission from local galaxy clusters using Fermi-LAT data 15m
    
    Galaxy clusters are the most massive gravitationally bound structures in the Universe. Even if clusters are nearly virialized structures, they undergo merging processes, creating merging shocks, and suffer from feedback from galaxies and AGNs; causing complex turbulent motions and amplifying their magnetic fields. These processes act as acceleration mechanisms for the plasma of the intracluster medium (ICM), originating a population of cosmic rays (CRs). Leptonic CRs have been long detected, but we should also expect a CR hadronic population that, through interactions with the ICM, should produce neutral pions that decay into gamma-rays. The detection of diffuse gamma-ray emission from galaxy clusters is one of the long-awaited milestones for the high-energy astroparticle physics community. Still, no unambiguous detection has been yet obtained.
    In this talk, we will present the results of a combined cluster analysis searching for CR-induced gamma-ray signals, using 16 years of Fermi-LAT data. In our previous work (di Mauro et al. 2023) we obtained from the combined analysis of 49 local galaxy clusters (12 years of data) a hint of signal between 2.5-3 sigmas, depending on the DM model considered. These results are aligned with the most recent works on searches for gamma-ray emission from clusters on Fermi-LAT data, which consistently find a non-vanishing hint of signal around the detection threshold. In this new work, we use a sample of near, well-known galaxy clusters and develop CR-induced emission templates using well-established X-ray measurements for calibration, assuming self-similarity for the members of our sample. To strengthen the robustness of our analysis, we define benchmark models to encapsulate the uncertainties in the spectral and spatial profiles for the CR-induced emission and perform the standard template-fitting analysis using the likelihood ratio test.
    
    Ponente: Judit Pérez-Romero (Center for Astrophysics and Cosmology/ University of Nova Gorica)
    
    JuditPerezRomero_FermiClusters_TeVPA25.pdf
  - 18:15
    
    Studies of low-luminosity AGN: NGC 4278 15m
    
    NGC 4278 is a low-luminosity active galactic nucleus (AGN) in the local Universe. The detection of very-high-energy (VHE) gamma rays from NGC 4278 by the Large High Altitude Air Shower Observatory (LHAASO) has identified it as a newly discovered extragalactic TeV gamma-ray source. However, the physical origin of the VHE gamma-ray emission from NGC 4278 remains unclear.
    In this study, we perform a comprehensive analysis of multi-wavelength and multi-messenger observations of NGC 4278 spanning a period up to 2024--2025. From the analysis of X-ray data obtained with Swift-XRT, we measure a flux of $1.17_{-0.10}^{+0.11} \times 10^{-12}~\mathrm{erg~cm^{-2}~s^{-1}}$ with a spectral index of $2.11_{-0.17}^{+0.17}$ in 2024--2025. We analyze Fermi-LAT data at the radio position of NGC 4278 from MJD 59274 to 60796, obtaining a test statistic (TS) value of 20.62. Additionally, we examine 10 years of public IceCube data to search for neutrino emission, but find no significant excess. We place upper limits on the neutrino flux from NGC 4278.
    We employ the leptohadronic code AMES to model the multi-wavelength emission from a relativistic jet, fitting both flaring and quiescent states to constrain the physical parameters. Furthermore, we investigate the potential contribution of high-energy gamma rays from large-scale outflows driven by the accretion disk.
    
    Ponente: Shilong Chen (Key Laboratory of Particle Astrophysics and Experimental Physics Division and Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences, 100049 Beijing, China)
    
    Talk_TeVPA2025_Multi-wavelength and multi-messengers from low-luminosity AGN NGC 4278.pdf
- 16:45 → 18:30
  Gamma Rays: Galactic Salón de Grados (ADEIT)
  
  Salón de Grados
  
  ADEIT
  
  Moderador: Stefano Menchiari (Instituto de Astrofísica de Andalucía - CSIC)
  - 16:45
    
    MeV radiation from a relativistic tidal disruption event 15m
    
    On 2 July 2025, the Gamma-ray Burst Monitor (GBM) onboard the Fermi Gamma-ray Space Telescope detected three short-duration MeV transients with overlapping sky locations. These events, named GRB 250702D/B/E (DBE), were triggered within approximately 1-2 hours of one another. Follow-up observations of this unusually long MeV transient (lasting longer than 3 hours) by the Neil Gehrels Swift Observatory and the Nuclear Spectroscopic Telescope Array over a period of 10 days revealed a steep temporal decline in the soft X-rays. These characteristics suggest that DBE may originate from a relativistic jet launched during the tidal disruption of a star by a compact object. We performed a time resolved spectral analysis of DBE during the prompt phase. The spectra are best described by a single power-law, extending from 10 keV to 40 MeV with a possible break at > 50 MeV. From standard MeV gamma-ray transparency arguments, we derive a lower limit on the jet bulk Lorentz factor (Gamma > 10). These constraints place DBE in agreement with four previously reported relativistic tidal disruption events in terms of outburst luminosity and energetics. The MeV spectra disfavor inverse Compton scattering of disk photons, while synchrotron radiation from sub-TeV electrons naturally accounts for the observed emission. Detection of relativistic tidal disruption events in the MeV gamma-rays open new windows for the characterization of their jet properties.
    
    Ponente: Gor Oganesyan (Gran Sasso Science Institue)
    
    Gor_Oganesyan_TeVPA2025.pdf
  - 17:00
    
    Supernova-origin of ultra-high energy gamma-rays in the Cygnus star-forming complex 15m
    
    Cygnus is a vast star-forming complex harbouring a population of powerful objects, including massive star clusters and associations, Wolf-Rayet stars, pulsars, and supernova remnants. The multi-wavelength picture is far from understood, in particular the recent LHAASO detection of multi-degree scale diffuse γ-ray emission up to PeV energies. In this talk, I demonstrate that hadronic emission from protons accelerated at a tens-of-kiloyears old, powerful supernova can account for the gamma-ray spectrum at 10 TeV-PeV. Furthermore, the energy dependent morphology is recovered using a 3D molecular cloud model. The supernova maximum energy in the hot, turbulent superbubble environment is estimated from published hydrodynamical simulations of Cygnus OB2 (Vieu et al. 2024). The transport equation is solved to determine the radial distribution of non-thermal particles, which is then used to infer the gamma-ray flux generated in molecular clouds and the neutral medium. To complement the very-high energy model, Fermi-LAT data at GeV-TeV is modelled with inverse-Compton emission of electrons accelerated at the termination shocks of Wolf-Rayet winds in Cygnus OB2. I discuss these results in the context of background from Galactic diffuse emission and other source candidates. I highlight in particular the role of multi-wavelength data to constrain the 3D distribution of molecular clouds.
    
    Ponente: Lucia Haerer (MPIK, Heidelberg, Germany)
    
    haerer_tevpa_25.pdf
  - 17:15
    
    Exploring the potential hadronic gamma-ray emission from a protostellar jet 15m
    
    Massive young stellar objects (MYSOs) can drive high-speed, collimated outflows capable of propagating at hundreds of kilometers per second through the circumstellar medium. The strong shocks produced in the internal regions of these jets, as well as the powerful termination shocks, can create favorable conditions for particle acceleration. In this study, that has been published in the beginning of 2025, we analyzed 15 years of data from the Fermi LAT instrument to investigate gamma-ray emission in the vicinity of IRAS 18162-2048, a ~20 M$_\odot$ MYSO that powers the longest and one of the most energetic jets known in the Galaxy.
    
    Previous radio observations of this object have revealed linearly polarized emission, indicating the presence of ~GeV electrons radiating synchrotron emission along the inner regions of the jet. Our analysis identifies the protostellar jet as the most likely source of the observed gamma-ray emission, suggesting an extension of the relativistic particle population to at least tens of GeV. Furthermore, given the jet’s energetics and ambient conditions, we cannot rule out a hadronic origin for the gamma rays. These findings position MYSOs as potential contributors to the hadronic cosmic-ray acceleration in star-forming regions and provide compelling evidence that protostellar jets can indeed radiate in gamma rays.
    
    Ponente: Javier Méndez-Gallego (IAA-CSIC)
    
    tevpa_slides.pdf
  - 17:30
    
    Understanding TeV gamma-ray emission from star clusters through global MHD simulations 15m
    
    In recent years, massive star cluster environments have emerged as a new class of gamma-ray sources capable of accelerating particles to very-high energies, to such extent that they could complement the supernova model for the origin of galactic cosmic rays. The environment sculpted by the interaction of powerful stellar winds is complex, highly structured from small (pc) to large (100 pc) scales, and presents a priori a number of plausible particle acceleration sites. Theoretical modelling is key to pinpoint the origin of the emission and constrain acceleration scenarios which could be probed with the next generation of gamma-ray instruments.
    The feedback of massive stars onto their environment is driven by non-trivial wind interactions which are inherently three-dimensional, making simple analytic models unable to fully capture the shock dynamics or to predict the properties of the magnetic fields. Understanding non-thermal phenomena in star-forming environments therefore requires detailed large-scale magnetohydrodynamic simulations. In this talk I present a novel method to simulate massive star cluster winds of arbitrary age in a variety of configurations. I will highlight the conditions required to generate a large-scale wind termination shock which could efficiently accelerate particles above hundreds of TeV. It is found that only compact clusters hosting a large number of powerful stars can become ultra-high energy (>100 TeV) sources after several million years of evolution. This result supports the wind termination shock scenario for Westerlund 1, but disproves this possibility in the case of the Cygnus region.
    
    Ponente: Thibault Vieu (Max-Planck-Institut für Kernphysik)
    
    TeVPa_2025.pdf
  - 17:45
    
    Star-Forming Galaxies as TeV γ-ray Sources: Prospects for Detection 15m
    
    Star-forming galaxies (SFGs) provide a unique laboratory to investigate cosmic-ray (CR) acceleration and transport in environments shaped by massive stellar populations. Their non-thermal emission, including γ-rays, is primarily associated with star formation rather than active galactic nuclei, as evidenced by the well-established correlation between star formation rate (SFR) and both radio and γ-ray luminosities.
    γ rays in SFGs are mainly produced through interactions between hadronic CRs and the interstellar medium (ISM), while CRs themselves are accelerated at supernova remnants (SNRs) and possibly in additional sites such as young massive star clusters. These acceleration regions, abundant in SFGs, may contribute significantly to the γ-ray output, particularly in systems with elevated SFR. While GeV γ-ray emission from SFGs has been firmly detected, their very-high-energy (VHE) counterparts remain largely unexplored due to observational limitations.
    In this work, we compiled a sample of GeV-detected SFGs and additional candidates identified from near-infrared surveys in the Local Volume. Employing empirical models constrained by multi-wavelength observations, we predicted their TeV spectra and assessed their detectability with current and next-generation ground-based γ-ray observatories. Our results indicate that the upcoming Cherenkov Telescope Array Observatory (CTAO) has the potential to detect nearly a dozen SFGs, significantly expanding the population of extragalactic VHE emitters. Such detections would not only establish SFGs as a new class of TeV sources, but also provide valuable constraints on CR acceleration mechanisms and the interplay between star formation and high-energy processes in galaxies.
    
    Ponente: Paula Kornecki (IAA-CSIC)
    
    kornecki_TeVPA.pdf
  - 18:00
    
    Exploring PeVatrons with associated molecular clouds in the era of CTAO and ASTRI Mini-Array 15m
    
    LHAASO has recently detected ultra-high-energy (UHE, >100 TeV) γ-rays from various Galactic sources, including supernova remnants, pulsar wind nebulae, microquasars, and young massive clusters. The presence of these UHE γ-rays indicates the potential acceleration of cosmic rays to PeV energies. A leading explanation for this emission involves CRs from sources interacting with nearby molecular clouds, generating γ-rays via neutral pion decay. This has sparked interest in galactic particle accelerators with associated molecular clouds.
    
    In this contribution, I will discuss whether galactic accelerators like supernova remnants, illuminating/interacting with molecular clouds can explain the UHE γ-ray emission detected by LHAASO. As a case study, I will mainly focus on the W51 Complex with different active acceleration sites especially supernova remnant W51C and analyze source-molecular cloud interactions contributing to the observed UHE emission. Two theoretical frameworks will be discussed: one involving direct remnant shock and cloud interaction, where the clouds are crushed and a second scenario in which cosmic rays from an earlier supernova remnant phase or neighboring sources illuminate nearby clouds. We will also present simulations for Cherenkov Telescope Array Observatory (CTAO) and ASTRI Mini-Array, highlighting their potential role in spatially resolving the UHE emission region.
    
    Ponente: Alan Sunny (INAF-IAPS & University of Rome Tor Vergata, Italy)
    
    PeVatron_MC-Sunny.pdf
  - 18:15
    
    Prospects on detection of the Fermi Bubbles with CTAO 15m
    
    In 2010, the Fermi Gamma-ray Space Telescope observed two gamma-ray emitting structures, the Fermi Bubbles (FBs), that extend up to 55° above and below the Galactic plane and that seem to emanate from the Galactic center region. Although the spectrum at latitudes |b| > 10° has a softening or a cutoff around 100 GeV, the one at the base of the FBs, |b| <10°, extends up to about 1 TeV without a significant cutoff in the Fermi LAT data. The mechanism behind the FBs production is currently under debate. More observations of the FBs at different energies are required to improve our understanding of their origin.
    Recently, H.E.S.S. and HAWC Observatory have set upper limits on the FBs. In this work, we assess the sensitivity of the Cherenkov Telescope Array Observatory (CTAO) using the "alpha configuration" to detect the FBs and investigate the optimal strategies for their detection. We will explore detection prospects for low and high latitude FBs. Paying special attention to the transition region. We simulate the observations using the official CTAO science tool, gammapy, considering several benchmark models for the FBs and the interstellar emission, and test different observational strategies that take advantage of the proposed CTAO consortium surveys.
    
    Ponente: Nina Bavdaž (University in Nova Gorica)
    
    TeVPA_Prospects_on_detection_of_the_FBs_with_CTAO.pdf
- 16:45 → 18:30
  Neutrinos: Source modeling Room 1.1+1.2 (ADEIT)
  
  Room 1.1+1.2
  
  ADEIT
  
  Moderador: Denise Boncioli (University of L'Aquila and INFN-LNGS)
  - 16:45
    
    The case for blazars as ultra-high-energy neutrino sources 15m
    
    Blazars are strong neutrino source candidates owing to their high intrinsic power and Doppler boost. However, in the sub-PeV range, where IceCube is most sensitive, blazars are inefficient neutrino emitters, and models seem to require extreme proton luminosities. In this talk, I present a new leptohadronic blazar model that captures the energetics and the extended nature of the relativistic jet. Magnetic turbulence can accelerate EeV protons just outside the broad line region, emitting 100 PeV neutrinos and describing the gamma-ray spectrum. Only a small fraction of the Eddington luminosity is carried by protons. The optical flux originates from a similar number of co-accelerated electrons and extends to the parsec scale. The model can describe both the quiescent emission and the 2017 flare of blazar TXS 0506+056 and the emission from PKS 0605-085, one of the blazars spatially associated with the UHE event KM3-230213A detected by KM3NeT. This suggests that some blazars should emit a hard UHE neutrino spectrum that will be within reach of future experiments.
    
    Ponente: Xavier Rodrigues (APC, Paris)
    
    xavier_rodrigues_tevpa2025.pdf
  - 17:00
    
    Modeling of blazar emission: multiwavelength and multimessenger fit powered by Convolutional Neural Network 15m
    
    Multimessenger observations, combining electromagnetic radiation and neutrinos, offer critical insights into the high-energy processes occurring in astrophysical sources. Recent coincident detections of high-energy neutrinos from the direction of blazars highlight them as ideal candidates for multimessenger modeling, and at the same time underscore the necessity of accurate modeling frameworks to interpret these complex signals. However, conventional hadronic models that explain neutrino emission from blazars are computationally intensive, complicating thorough parameter-space exploration and precise data fitting. In this presentation, I introduce a novel approach based on convolutional neural networks (CNNs), specifically designed to significantly accelerate the modeling of multimessenger blazar emissions. This CNN, trained on outputs from the SOPRANO numerical code, effectively and accurately reproduces the radiative signatures of protons, electrons, and secondary particles, transforming computationally demanding hadronic emission calculations into an efficient tool for rapid exploration and robust statistical fitting of observational data. I demonstrate the application and efficacy of this CNN-based method through fitting multimessenger observational data from blazars TXS 0506+056 and PKS 0735+178, showing the capability of the model to effectively constrain physical parameters and interpret multimessenger emission from blazar jets. This innovative methodology advances our understanding of blazar physics and provides a powerful analytical framework for future multimessenger astrophysics studies.
    
    Ponente: Narek Sahakyan (ICRANet Armenia IO)
    
    Sahakyan_TeVPA.pdf
  - 17:15
    
    Can the Neutrinos from TXS 0506+056 Have a Coronal Origin? 15m
    
    The recent detection of high-energy neutrinos from NGC 1068 supports the idea that AGN coronae—magnetized, compact regions around supermassive black holes—can accelerate protons and produce neutrinos via photohadronic interactions with X-ray photons. I present a plasma-informed framework for this coronal scenario, grounded in particle-in-cell simulations of magnetic reconnection and turbulence. Motivated by the NGC 1068 signal, I also examine whether similar coronal processes could contribute to neutrino production in blazars—AGN with a powerful jet pointing toward Earth. This is an exciting possibility in view of the neutrino association with a gamma-ray flare from the blazar TXS 0506+056. However, I show that a coronal origin is strongly disfavored in this case, reinforcing the interpretation of jet-based emission for blazars.
    
    Ponente: Damiano Fiorillo (DESY (Zeuthen))
    
    SlidesTXS0506TeVPa.pdf
  - 17:30
    
    Multimessenger-Informed Characterization of High-Energy Neutrino Emission from Bright Seyfert Galaxies 15m
    
    Observation of high-energy neutrinos from the direction of the nearby active galaxy, NGC 1068, was a major step in identifying the origin of high-energy neutrinos. This observation revealed that high-energy neutrinos originated at the heart of active galaxies, which are opaque to very-high-energy gamma-ray emission. This realization is further reinforced by the multimessenger picture for the observed all-sky neutrino flux in IceCube as well as the recently identified excess of neutrinos in the direction of NGC 4151, another nearby AGN. Modeling neutrino emission from the core of AGN relies on the multi-wavelength observations of the inner parts of the active galaxy and is challenging due to the uncertainties associated with the absorption of emission in these dense environments. Here, we employ the measured neutrino spectra together with the sub-GeV gamma-ray emission measured by the Fermi satellite to break the degeneracy and narrow down the parameter space of neutrino emission from the coronae of AGN. Our result will help estimate the prospects for identifying additional sources and guide future targeted analyses.
    
    Ponente: Jose Carpio (University of Nevada Las Vegas)
    
    TeVPA2025_Carpio.pdf
  - 17:45
    
    Universal properties of electromagnetic cascades initiated by hadronic interactions 15m
    
    The interactions of high-energy cosmic rays produce neutrinos and gamma rays. However, while neutrinos travel unimpeded, the accompanying gamma rays can trigger electromagnetic cascades via pair production on ambient photons, reprocessing their energy to lower frequencies. For intergalactic cascades produced in the propagation through extragalactic radiation, the resulting photons have a universal spectral shape, first described by Berezinsky in the 1970s. For internal cascades, developed within the astrophysical sources where the gamma rays are produced, the assumptions behind this result often break down due to dominant synchrotron losses. I will discuss a generalized theory of electromagnetic cascades, encompassing synchrotron-dominated cases, and determine the conditions under which a universal cascade spectrum can be obtained. I will focus on cascades triggered by gamma rays of hadronic origin and show how the universal spectrum emerges among a variety of high-energy astrophysical sources. These results are particularly relevant for predicting the electromagnetic counterpart of gamma-ray opaque sources, such as the coronae of active galactic nuclei, which are likely the dominant sources of the diffuse neutrino flux observed by the IceCube telescope.
    
    Ponente: Federico Testagrossa (DESY Zeuthen)
    
    TeVPa_Testagrossa.pdf
  - 18:00
    
    Cosmic-Ray Interactions in Pulsar Magnetospheres 15m
    
    Gamma-ray observations have established that pulsar magnetospheres are efficient accelerators of electrons and positrons. Analytical models and numerical simulations further suggest that a fraction of a pulsar’s rotational energy can be converted into the acceleration of cosmic rays, positioning pulsars as potential contributors to the Galactic cosmic-ray population. However, direct observational evidence of hadronic acceleration within these environments remains elusive. In this talk, we present recent advances toward a self-consistent modeling of the radiation fields in pulsar magnetospheres, with the goal of predicting secondary signals arising from the interactions of accelerated cosmic rays with these fields. We focus in particular on the production of high-energy neutrinos, which are especially compelling in light of recent IceCube observations indicating a high-energy neutrino signal from the Galactic plane. We assess the detectability of these signals with current and upcoming neutrino observatories, highlighting the potential of KM3NeT.
    
    Ponente: Claire Guépin Detrigne (CNRS, LUPM)
    
    CGuepin_Pulsars_Nov2025.pdf
  - 18:15
    
    Constraints on High Energy Neutrino density from Large Scale Structure 15m
    
    Despite growing statistics, the sources of most high energy neutrinos remain unknown. Here we present a tomographic approach that makes use of the angular, harmonic cross-correlation between IceCube data and galaxy surveys. If neutrino sources follow the Large Scale Structure (LSS), this cross-correlation will be non-zero and, if detected, it will determine how neutrino sources correlate with the LSS via the linear bias and measure now the neutrino emissivity evolves with redshift, thereby allowing to exclude certain neutrino source models. In this proceedings we introduce our method and apply it to the 10-year IceCube data in combination with four galaxy catalogues covering redshifts up to z~3.
    
    Ponente: Alberto Gálvez Ureña (Institute of Physics of the Czech Academy of Sciences)
    
    TevPA Valencia Presentation.pdf
jueves, 6 noviembre
- 9:00 → 10:30
  Plenary Session: VII Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Aart Heijboer (nikhef)
  - 9:00
    
    Gamma-ray astrophysics from the ground 30m
    
    The field of ground-based gamma-ray astronomy is in the midst of a transformative era, with the current generation of instruments revealing a rich and intricate view of non-thermal astrophysics in the TeV–PeV energy range. At the same time, a new generation of observatories is being planned or built, promising a major step forward in our understanding of numerous astrophysical systems, as well as offering new ways to probe fundamental physics.
    In this talk, I will briefly review the current status of these instruments and highlight selected recent discoveries. I will also discuss the progress and discovery potential of the upcoming Cherenkov Telescope Array Observatory (CTAO).
    
    Ponente: Gabrijela Zaharijas (Center for Astrophysics and Cosmology, University of Nova Gorica)
    
    2025-TeVPA-Zaharijas-v1.pdf
  - 9:30
    
    Cosmic-ray acceleration in Galactic Sources 30m
    
    Recent VHE and UHE observations of Galactic sources are at last identifying the key extreme Galactic particle accelerators. This suggests that we may soon be able to address the physics underpinning the origin of the locally measured knee feature in the cosmic-ray spectrum. I will review some of these findings, and discuss their implications.
    
    Ponente: Brian Reville (MPIK)
    
    TeVPa_2025.pdf
  - 10:00
    
    Chasing the Rarest Particles in the Universe: Prospects for Ultra-High-Energy Neutrino Detection 30m
    
    After more than a decade since the advent of neutrino astronomy, the origin of most of the diffuse astrophysical neutrino flux observed by IceCube remains unresolved. Notably, while IceCube has yet to detect any neutrino events above 10 PeV, the KM3NeT collaboration has recently reported the observation of the highest-energy neutrino ever detected. Ultra-high-energy (UHE) neutrinos (E > 10 PeV) are expected to originate either directly from astrophysical sources or as cosmogenic neutrinos produced during the propagation of ultra-high-energy cosmic rays interacting with cosmic photon fields. Because of their extremely low flux, detecting such particles requires detectors covering surfaces of the order of hundreds of square kilometers. In this talk, I will discuss the scientific importance of UHE neutrino detection, together with an overview of current and future experimental efforts aiming to unveil these elusive messengers.
    
    Ponente: Simona Toscano (IIHE - ULB)
    
    Toscano_TeVPA2025.pdf
- 10:30 → 11:00
  
  Coffee Break 30m Dome (Fundación Bancaja)
  
  Dome
  
  Fundación Bancaja
- 11:00 → 12:30
  Plenary Session: VIII Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Marco Taoso (INFN Torino)
  - 11:00
    
    Strong gravitational lensing at gamma rays 30m
    
    Strong gravitational lensing at gamma rays is mostly unexplored, with only two confirmed strong lenses emitting at these energies. Despite their rarity, these two objects offer a unique window into high-energy astrophysical sources at high redshifts. The paucity of lenses at gamma rays is primarily due to challenges in detecting and confirming them using standard methods, as the angular resolution to identify multiple images is limited at high energies. Nevertheless, strong lenses display characteristic time delays between multiple images, making time-domain analyses a viable alternative route to investigate these systems and discover new ones.
    
    In this talk, we review the current status of strong gravitational lensing at gamma rays, including the properties of known systems. We highlight recent advances in time-domain techniques and discuss the prospects for future discoveries with current and upcoming gamma-ray observatories, which can potentially open a novel channel for cosmological studies at the highest precision.
    
    Ponente: Cristiana Spingola (INAF Institute for Radioastronomy)
    
    TevPA2025_Spingola_Plenary.pptx
  - 11:30
    
    Axion-like Particles 30m
    
    Axion-like particles are hypothetical low-mass weakly coupled particles that appear naturally in many extensions of the standard model and can have a surprising number of potentially detectable effects in astrophysics and cosmology. In this talk we will review and update the theoretical motivation for their existence, the abundant astrophysical probes at our disposal and the recent boom in experimental techniques to find these elusive particles and pinpoint new physics at amazingly large energy scales.
    
    Ponente: Javier Redondo (Zaragoza U)
    
    redondo-tevpa.pptx
  - 12:00
    
    The 21cm signal from the Cosmic Dawn 30m
    
    The 21-cm hyperfine line of HI is set to revolutionize studies of the first billion years, spanning the cosmic dawn of the first stars and eventual reionization of our Universe. I will discuss the potential of this probe in learning about the unknown astrophysics of the first galaxies as well as physical cosmology. Preliminary claims of a detection of the mean (sky-averaged) 21cm signal showcased its potential in constraining exotic dark matter-baryon interactions in the early Universe, although recent robust interpretation points against new physics. The true potential of the cosmic 21cm signal is in mapping out the first half of our observable Universe through HI fluctuations. Current upper limits on the 21-cm power spectrum already provide new insights into the heating of the intergalactic medium, likely caused by a new population of high mass X-ray binaries. Future detections will allow us to set the strongest available constraints on exotic heating mechanisms through dark matter decay and annihilation.
    
    Ponente: Andrei Mesinger (University of Catania)
    
    Mesinger_2025.pdf
- 12:30 → 14:30
  
  Lunch Break 2h ADEIT
  
  ADEIT
- 14:30 → 16:15
  Connections to Particle Physics Salón de Grados (ADEIT)
  
  Salón de Grados
  
  ADEIT
  
  Moderador: Luca Visinelli (Università degli Studi di Salerno, Italy)
  - 14:30
    
    Probing the Parameter Space of Axion-Like Particles Using Simulation-Based Inference 15m
    
    Axion-like particles (ALPs) appear in various extensions of the Standard Model and can interact with photons, leading to ALP-photon conversions in external magnetic fields. This phenomenon can introduce characteristic energy-dependent “wiggles” in gamma-ray spectra. The Cherenkov Telescope Array Observatory (CTAO) is the next-generation ground-based gamma-ray observatory, designed to provide enhanced sensitivity and energy coverage (20 GeV – 300 TeV) over current Imaging Atmospheric Cherenkov Telescopes (IACTs) and offers an excellent opportunity to study such effects.
    
    In this work, we employ Simulation-Based Inference (SBI) to explore the parameter space of ALPs, targeting the flaring states of blazars, which are among the brightest gamma-ray sources and ideal candidates for probing ALP-induced spectral modulations. Additionally, we investigate whether this inference method can produce accurate ALP exclusion limits comparable to those reported in previous studies that use the classical likelihood-ratio approach. Through this approach, we seek to yield robust constraints on ALP-photon interactions and make substantial advancements in this field.
    
    Ponente: Pooja Bhattacharjee (University of Nova Gorica)
    
    TeVPA_Pooja_Bhattacharjee.pdf
  - 14:45
    
    Sensitivity of CTAO to axion-like particles from blazars: a machine learning approach 15m
    
    Blazars are a class of active galactic nuclei, supermassive black holes located at the centres of distant galaxies characterised by strong emission across the entire electromagnetic spectrum, from radio waves to gamma rays. Their relativistic jets, closely aligned to the line of sight from Earth, are a rich and complex environment, characterised by the presence of strong magnetic fields over parsec-scale lengths. Owing to their cosmological distance from Earth, these sources serve as ideal targets to probe non-standard gamma-ray propagation. In particular, axion-like particles (ALPs) could be detected through their coupling to photons, which enables ALP-photon conversions in external magnetic fields, leading to distinct signatures in the blazars’ gamma-ray spectra. The Cherenkov Telescope Array Observatory (CTAO), with its enhanced energy resolution and point-source sensitivity with respect to present ground-based gamma-ray telescopes, will be a next-generation instrument very well fit to probe such features. In this contribution, we explore an approach based on the use of machine learning (ML) classifiers and compare it to the standard method of likelihood-ratio test, previously applied in CTAO sensitivity studies for ALP signatures. Our preliminary $2\sigma$ exclusion regions on the ALP parameter space suggest that both techniques yield consistent results, with the ML-based method offering broader coverage and potentially extending the CTAO sensitivity beyond existing constraints.
    
    Ponente: Francesco Schiavone (Università degli Studi di Bari & INFN Bari)
    
    Schiavone_TeVPA25.pdf
  - 15:00
    
    Producing Light Dark Matter at Fixed Target Experiments 15m
    
    Sub-GeV, or light, dark matter (DM) has emerged as a compelling candidate for the observed DM in the universe. Unlike the canonical WIMP, light DM can account for the thermal relic abundance while evading nuclear recoil direct detection constraints, due to its limited momentum transfer. This motivates alternative search strategies, such as electron recoil direct detection and accelerator based experiments.
    Upcoming experiments such as the Light Dark Matter eXperiment (LDMX) and the Search for Hidden Particles (SHiP), are projected to probe a broad range of dark matter scenarios, significantly extending the sensitivity frontier for light DM theories.
    In this talk, we explore three main aspects in the context of DM at fixed target experiments: the methods for simulating expected signals, the vast theory landscape, and the implications of a potential DM signal.
    
    Ponente: Taylor Gray (Chalmers University)
    
    TeVPA_TaylorGray.pdf
  - 15:15
    
    Time-delayed gamma-ray signatures of heavy axions from core-collapse supernovae 15m
    
    Heavy axions that couple to both quantum electrodynamics and quantum chromodynamics with masses on the order of MeV–GeV and high-scale decay constants in excess of $10^{8}$ GeV may arise generically in, e.g., axiverse constructions. In this work we provide the most sensitive search to date for the existence of such heavy axions using Fermi-LAT data toward four recent supernovae (SN): Cassiopea A, SN1987A, SN2023ixf, and SN2024ggi. We account for heavy axion production in the proto-neutron-star cores through nuclear and electromagnetic processes and then the subsequent decay of the axions into photons. While previous works have searched for gamma rays from SN1987A using the Solar Maximum Mission that observed SN1987A during the SN itself, we show that using Fermi Large Area Telescope data provides an approximately 5 orders of magnitude improvement in flux sensitivity for axions with lifetimes larger than around 10 yrs. We find no evidence for heavy axions and exclude large regions of previously unexplored parameter space.
    
    Ponente: Yujin Park (UC Berkeley)
    
    TeVPA2025_Yujin.pdf
  - 15:30
    
    Can Axions Put Out Gamma-ray Bursts? 15m
    
    Short gamma-ray bursts (GRBs) are some of the brightest transients in the universe. We show that heavy axion-like particles (ALPs) can be produced in the hot plasma of GRB fireballs. When produced in the earliest stages, they escape and decay outside the source. We demonstrate that the resulting prompt photon field arising from ALP decay is too rarefied to re-thermalize, effectively preventing the re-emergence of the fireball, thus dimming or disrupting GRBs. In the later stages of the evolution of the expanding fireball, hadronic interactions become important and radiative transfer from decaying ALPs can lead to a diffuse contribution to various cosmic backgrounds through cascades, among other signatures. Using existing observations of short GRBs, we place competitive bounds reaching ALP-photon couplings of $g_{a \gamma \gamma} \sim 4 x 10^{-12}~\text{GeV}^{-1}$ for ALP masses between 200 MeV and 5 GeV.
    
    Ponente: Oindrila Ghosh (Oskar Klein Centre, Stockholm University)
    
    Oindrila_Ghosh_TeVPA_2025.pdf
  - 15:45
    
    Heating the dark matter halo with dark radiation from supernovae 15m
    
    Supernova explosions are extreme cosmic events that may impact not only ordinary matter but also dark matter (DM) halos. In this talk, I explore the possibility that a fraction of supernova energy is released as dark radiation, which could transform a cuspy DM halo into a cored one, potentially explaining observed cores in some dwarf galaxies. Alternatively, limits on DM core sizes provide constraints on the energy channeled into light particles beyond the Standard Model (SM). Based on evaluation of energetics, one finds that even a small fraction of the total SN energy is sufficient to change the overall shape of the DM halo and transform a cuspy halo into a cored one. We evaluate some well motivated benchmark models, e.g. the dark photon and dark Higgs, to demonstrate that significant supernova emissivity of dark radiation and large DM halo opacity are achievable in realistic particle physics model. Interestingly, couplings consistent with SN1987A observations can still have a measurable impact on dwarf galaxy halos.
    
    Ponente: Stefan Vogl (University of Freiburg)
    
    Vogl_SN_heating_TeVPA.pdf
  - 16:00
    
    Particle Physics Studies at the Pierre Auger Observatory 15m
    
    The Pierre Auger Observatory is the world's largest facility dedicated to the study of ultra-high-energy cosmic rays. By observing extensive air shower cascades produced when cosmic rays interact with the Earth's atmosphere, the Observatory enables indirect measurements of hadron-air collisions at center-of-mass energies that exceed those achievable by the Large Hadron Collider.
    Analyses of global shower observables, such as the depth of shower maximum and the ground-level signals associated to the muonic component have revealed significant discrepancies between experimental data and predictions from current hadronic interaction models. In particular, a persistent muon deficit in simulated showers has sparked a range of new investigations aimed at better understanding hadronic interactions at extreme energies.
    To address these challenges and enhance its sensitivity to the primary mass composition, the Observatory is undergoing a major upgrade known as AugerPrime. This upgrade introduces new detector components capable of disentangling the various constituents of the air shower, opening the door to more detailed studies of its development and the underlying particle physics.
    
    Ponente: Alexandra Fernandes (LIP/UM)
    
    Fernandes_TeVPA2025.pdf
- 14:30 → 16:15
  Cosmic Rays Room 2.1+2.2 (ADEIT)
  
  Room 2.1+2.2
  
  ADEIT
  
  Moderador: Denise Boncioli (University of L'Aquila and INFN-LNGS)
  - 14:30
    
    The galactic cosmic ray knee confronts very-high energy diffuse gamma-ray 15m
    
    Recently, LHAASO has announced the highest-energy measurements of the diffusive gamma-ray flux, offering the possibility of probing the spatial distribution and energy spectrum of the galactic cosmic rays (CRs) up to the all-particle spectrum knee ( PeV). However, a persistent tension between observations by experiments (such as Fermi and LHAASO) and the predictions based on measurements of the local CR flux increase the necessity of a robust model of the CR spectrum. In the present work, we estimate the gamma-ray flux coming from CRs with energies as high as the knee. We developed a phenomenological model of the galactic CR flux using the latest data available by satellite missions and ground-based observatories. In particular, our model identifies the series of spectral breaks found in the proton and helium fluxes in the range of to GeV and corroborates that these breaks are located at the same rigidity for different CR species. In contrast with other models, our analysis also includes the most recent measurements of the proton spectrum by the GRAPES-3 experiment, showing an additional spectral break at TeV. We also include the uncertainty related to the contribution of heavier nuclei in the CR composition. We compare our expected gamma-ray flux with previous models and recent observational data, focusing our discussion on the new spectral features provided by our model.
    
    Ponente: Luis Enrique Espinosa Castro (GSSI)
    
    Pagliaroli_TeVPA2025.pdf
  - 14:45
    
    Cosmic Rays at the Knee: Rethinking the End of the Galactic Spectrum 15m
    
    The cosmic ray knee, observed at around 4 PeV, marks a striking feature in the all-particle cosmic ray spectrum and is widely regarded as the signature of the end of the Galactic component. Recent direct measurements from DAMPE, CALET, and ISS-CREAM are now probing the spectrum with unprecedented precision up to the vicinity of the knee, while LHAASO has provided groundbreaking indirect data on both the all-particle flux and composition in this critical energy range. These advances are challenging the traditional view that the knee reflects either the maximum acceleration energy of Galactic sources or a change in diffusion properties of the Galactic magnetic field. Surprisingly, when considered together, these new observations indicate a breakdown of the standard rigidity paradigm, suggesting either the emergence of a new population of cosmic ray sources at the highest energies or the need for additional physical mechanisms. In this talk, I will discuss recent developments and present novel interpretations of the data, exploring how these results reshape our understanding of the Galactic–extragalactic transition and the origin of the highest energy Galactic cosmic rays.
    
    Ponente: Carmelo Evoli (Gran Sasso Science Institute)
    
    CEvoli_TEVPA2025.pdf
  - 15:00
    
    Assessing the diffusion-drift transition as the origin of the cosmic ray knee 15m
    
    The transition from diffusion to gradient-curvature drift as the dominant mechanism for the Galactic escape of cosmic rays (CRs) is considered a possible origin of the CR “knee". We studied the connection between antisymmetric diffusion and these drifts by performing test-particle simulations of CR propagation in synthetic turbulent magnetic fields using the Monte Carlo code CRPropa 3. We computed the drift escape timescale in realistic Galactic magnetic field configurations as a function of particle rigidity and magnetic turbulence level, and we compared it to the escape timescales by parallel and perpendicular diffusion. We found that for low turbulence levels and large Galactic halo lengths, a "knee"-like spectral feature is predicted, attributed to the onset of drifts over perpendicular diffusion. To evaluate the effectiveness of this model, we estimated the predicted CR grammage at the “knee” energy range under this model and compared it to the grammage inferred from measurements of B/C ratio at TeV energies. We discuss how a energy-independent gramme at high-energies could lead to a good agreement between the model and direct CR observations. Alternatively, we explored how a topology of the regular magnetic field enhancing parallel and perpendicular diffusion could reproduce the observed grammage at low-energies while preserving a diffusion-drift transition at PeV energies.
    
    Ponente: Luis Enrique Espinosa Castro (GSSI)
    
    Espinosa_TeVPA2025.pdf
  - 15:15
    
    Supernova remnants in super bubbles acting as cosmic ray accelerators 15m
    
    Supernova remnants (SNRs) are often considered as the main sites of acceleration of Galactic cosmic rays, up to the knee feature in the cosmic-ray spectrum. However, their ability to accelerate particles to reach PeV energies is questionable and lacks observational evidence. Theoretical predictions suggest that only a small subclass of very young SNRs evolving in dense environments could potentially satisfy the necessary conditions to accelerate particles to PeV energies. Most such theoretical investigations are carried out either in the standard interstellar medium or in the wind of the progenitor. Since most core collapse supernovae occur in star clusters, it is important to extend such investigation to SNRs expanding in super bubbles. In this work we focus on a SNR shock propagating in the collective wind of a compact star cluster, and we study the acceleration process as a function time, with special emphasis on the maximum energy of accelerated particles. Using both analytic and numerical approaches we investigate the spectrum of accelerated particles and maximum achievable energy in the case of pre-existing turbulence in the collective wind and self-generated magnetic perturbations. We find that similar to isolated SNRs, acceleration to PeV energies is plausible only for extreme conditions achievable only in a small subset of SNRs.
    
    Ponente: Iurii Sushch (CIEMAT, Spain)
    
    snr_starcluster_tevpa2025_sushch.pdf
  - 15:30
    
    Microquasar jet-cocoon systems as PeVatrons and the origin of cosmic rays 15m
    
    The origin of Galactic cosmic rays (CRs), particularly around the knee region ($\sim$3 PeV), remains a major unsolved question. Recent observations by LHAAASO suggest that the knee is shaped mainly by protons, with a transition to heavier elements at higher energies.
    Microquasars -- compact jet-emitting sources -- have emerged as possible PeV CR accelerators, especially after detections of ultrahigh-energy gamma rays from these systems. We propose that the observed proton spectrum (hard below a few PeV, steep beyond) arises from the reacceleration of sub-TeV Galactic CRs via shear acceleration in large-scale microquasar jet-cocoon structures.
    Our model also naturally explains the observed spectrum of energies around a few tens of PeV by summing up heavier nuclei contributions. Additionally, similar reacceleration processes in radio galaxies can contribute to ultrahigh-energy CRs, bridging Galactic and extragalactic origins. Combined with low-energy CRs from supernova remnants and galaxy clusters around the second knee region, this scenario could provide a unified explanation for CRs across the entire energy spectrum.
    
    Ponente: Bing Theodore Zhang (Institute of high energy physics, CAS)
    
    TeVPA-microquasar-TeVPA-20251106-v2.pdf
  - 15:45
    
    Interacting SNe: super-PeV CR candidates that explain the nuclear composition trends 15m
    
    The mysterious sources of high energy cosmic rays must be able to explain the power-law flux in energy as well as the nuclear composition changes at spectral breaks. Interacting supernovae may be able to explain these observed features. We build on a self-consistent model of the shock formed between supernova ejecta and the circumstellar medium by accounting for the composition of accelerated nuclei. IIn supernovae, with more massive circumstellar media compared to other types, are able to accelerate nuclei to super-PeV energies. We show that the flux and spectral shape from interacting supernovae agree well with the cosmic rays observed recently by experiments like LHAASO, TA, and IceTop between ~1e16 and ~5e17 eV. We also take into account the result that partially ionized nuclei can be preferentially injected, based on their mass and charge, to show that an initially solar composition before injection can explain the increasing average mass number at these energies. Finally, we discuss connections between cosmic ray acceleration and multi-messenger astrophysics.
    
    Ponente: Nick Ekanger (Tohoku University)
    
    Ekanger_TeVPA25.pdf
  - 16:00
    
    Is SNR G69.7+1.0 a PeVatron? A NuSTAR Hard X-ray Investigation of 1LHAASO J2002+3244u 15m
    
    The study of UHE $\gamma$-ray emission plays a key role in identifying the astrophysical accelerators responsible for producing $\sim$ PeV particles and shaping the Galactic cosmic-ray population. SNR G69.7+1.0 has recently attracted attention due to its association with the LHAASO source 1LHAASO J2002+3244, which emits above 100 TeV. This spatial coincidence provides a unique opportunity to investigate particle acceleration in supernova remnants (SNRs). While young SNRs are efficient cosmic ray accelerators, direct evidence for their role as PeVatrons remains unclear. We present preliminary results from the first NuSTAR observation of SNR G69.7+1.0, aimed at characterizing its hard X-ray emission, constraining its spectral properties, and probing the maximum energies of accelerated particles. These results are complemented by multi-wavelength data to assess the physical conditions under which SNRs may become PeVatrons.
    
    Ponente: Moaz Abdelmaguid (New York University Abu Dhabi)
    
    TeVPA_Conference_2025_moaz.pdf
- 14:30 → 16:15
  Dark Matter: Indirect Detection: Stars and galaxies Room 3.1+3.2 (ADEIT)
  
  Room 3.1+3.2
  
  ADEIT
  
  Moderador: Matthew Baumgart
  - 14:30
    
    Stellar streams as targets for indirect dark matter searches 15m
    
    In this talk, we summarize our research on stellar streams as a new and complementary target for dark matter (DM) searches with gamma rays.
    
    Stellar streams whose progenitor is a dwarf galaxy (dG) are particularly interesting targets for DM searches, since dGs are thought to be highly DM-dominated systems. We expect these streams to have lost most of their DM content during the stretching process, yet a significant amount of DM should remain within their core. If the DM particles are Weakly Interacting Massive Particles (WIMPs), they could annihilate in the streams’ core, producing a detectable gamma-ray signal. In this work, we analyze data from the Large Area Telescope on board the NASA Fermi satellite (Fermi LAT) to look for a potential WIMP annihilation signal from the direction of an optimized sample of streams. In the absence of a signal, we place the first constraints on the WIMP parameter space obtained from these objects for several annihilation channels.
    
    A key challenge in this analysis is the uncertainty in the DM density profile of the streams, which directly impacts the expected gamma-ray flux. To address this issue, we will also present our ongoing work in which we are using the Auriga suite of high-resolution hydrodynamical simulations to model the DM distribution within disrupted dG streams. These simulations provide a more robust framework for interpreting our results and refining future DM searches with stellar streams.
    
    Ponente: Cristina Fernández-Suárez (UAM & IFT)
    
    Streams_DM_Tevpa2025_CFS.pdf
  - 14:45
    
    New insights on low-mass dark matter subhalo tidal tracks via numerical simulations 15m
    
    https://arxiv.org/abs/2506.01152
    A number of studies assert that dark matter (DM) subhaloes without a baryonic counterpart and with an inner cusp always survive no matter the strength of the tidal force they undergo.
    In this work, we perform a suite of numerical simulations specifically designed to analyse the evolution of the circular velocity peaks ($V_\mathrm{max}$, and its radial value $r_\mathrm{max}$) and concentration of low-mass DM subhaloes due to tidal stripping. We employ the improved version of the DASH code, introduced in our previous work AAS+23 to investigate subhalo survival.
    We follow the tidal evolution of a single DM subhalo orbiting a Milky Way (MW)-size halo, the latter modeled with a baryonic disc and a bulge replicating the actual mass distribution of the MW. We also consider the effect of the time-evolving gravitational potential of the MW itself. We simulate subhaloes with unprecedented accuracy, varying their initial concentration, orbital parameters, and inner slope (both NFW and prompt cusps are considered).
    Unlike much of the previous literature, we examine the evolution of subhalo structural parameters --tidal tracks-- not only at orbit apocentres but also at pericentres, finding in the former case both similarities and differences -- particularly pronounced in the case of prompt cusps.
    Overall, $r_\mathrm{max}$ shrinks more than $V_\mathrm{max}$, leading to a continuous rise of subhalo concentration with time. The velocity concentration at present is found to be around two orders of magnitude higher than the one at infall -- about an order of magnitude more compared to the increase found for field haloes -- being comparatively larger for pericentre tidal tracks versus apocentres.
    These findings highlight the dominant role of tidal effects in reshaping low-mass DM subhaloes, providing valuable insights for future research via simulations and observations, such as correctly interpreting data from galaxy satellite populations, subhalo searches with gravitational lensing or stellar stream analyses, and indirect DM searches.
    
    Ponente: Alejandra Aguirre-Santaella (ICC Durham University)
    
    AAguirreSantaella-ttracks.pdf AAguirreSantaella-ttracks.pptx
  - 15:00
    
    Dark Matter-Electron Interactions Change the Spectral Index of M87 15m
    
    The Dark Matter (DM) distribution within a few kpc of the center of galaxies is essential for indirect detection searches and probing the particle nature of DM. Below the kpc scale, we examine external galaxies where adiabatically growing black holes lead to the formation highly dense DM region dubbed the DM spike. These spikes may lie within galaxy radio jets, such as M87, where minimal coupling between DM and the standard model can significantly impact the electron distribution. Observations from the KVN and VERA Array (KaVA) and the Very Long Baseline Array (VLBA) constrain this electron distribution, enabling leading constraints on sub-GeV DM. We further model the effect of DM cooling on the electron distribution and argue that this mechanism offers a compelling explanation for the enigmatic behavior the spectral index in Radio Loud galaxies.
    
    Ponente: Abdelaziz Hussein (MIT)
    
    Hussein_TeVPA_2025.pdf
  - 15:15
    
    Impact of Galactic dark matter on annihilation signals from Sagittarius 15m
    
    A gamma-ray source has been identified at the center of the Sagittarius (Sgr) dwarf spheroidal. It is unclear whether the observed gamma-ray emission is from a millisecond pulsar population or from dark matter annihilation within the Sgr halo. Probing this ambiguity requires accurate knowledge of the Sgr dark matter distribution. However, since Sgr is in the process of tidal disruption, there may be systematic issues in accurately determining the distribution from equilibrium models. Therefore, it is optimal to turn to hydrodynamical simulations. In this talk, I will discuss the expected annihilation signals from Sgr using analogues from the Auriga cosmological simulations. Additionally, I will show that by taking into consideration the presence of Milky Way dark matter particles passing through Sgr, the annihilation rate for velocity-dependent models can be enhanced by several orders of magnitude. Finally, I will discuss the impact of Milky Way dark matter particles on annihilation signals from other known dwarf galaxies.
    
    Ponente: Evan Vienneau (University of Alberta)
    
    TeVPA_2025.pdf
  - 15:30
    
    On the dark matter capture by celestial objects 15m
    
    Dark matter capture by celestial objects is widely studied as one of the methods to indirectly detect dark matter. Celestial objects, such as neutron stars, brown dwarfs, and planets, first gravitationally attract ambient dark matter particles. If dark matter particles are heavy enough, they transfer energy to those objects upon scattering, being gravitationally bound. This process ends up accumulating a large number of dark matter particles inside celestial bodies, producing a detectable signature including the decay products of their annihilation. In this talk, we will examine the underlying assumptions in this scenario and point out that they might be inconsistent with each other in some cases.
    
    Ponente: Takuya Okawa (SISSA)
    
    2025_TeVPA_Okawa.pdf
  - 15:45
    
    Jupiter is a Leptophilic Dark Matter Refrigerator 15m
    
    Jupiter has long been considered a pre-eminent target for dark matter searches, due to its proximity, mass, and low astrophysical backgrounds. However, low-mass dark matter ($\leq$400 MeV) is expected to efficiently evaporate from the Jovian core via interactions with standard model particles, limiting searches for dark matter effects. We show that in the case of leptophilic dark matter, evaporation rates are strongly suppressed due to the fact that most of Jupiter's hydrogen exists in a metallic state where electrons completely fill the Fermi-Dirac particle distribution and thus cannot donate energy to evaporate the dark matter particle. We show that dark matter down to MeV-masses can remain trapped within Jupiter on Gyr timescales. Applying this effect to previous studies of dark matter-induced airglows on the Jovian surface, we find limits that hit theoretically motivated targets for MeV-scale leptophilic dark matter.
    
    Ponente: Thong Nguyen (Stockholm University)
    
    TeVPA2025_ThongNguyen.pdf
  - 16:00
    
    Searching for Dark Matter in Antarctica with the GAPS Experiment 15m
    
    The General Antiparticle Spectrometer (GAPS) is a balloon-borne cosmic-ray experiment designed to search for light antinuclei at kinetic energies below 0.25 GeV/n, a largely unexplored range that may carry distinctive signatures of dark matter.
    The instrument consists of a ten-layer lithium-drifted silicon tracker, cooled by a novel oscillating heat pipe thermal system, and is enclosed on all sides by a plastic scintillator-based time-of-flight (TOF) and trigger system with high-precision timing.
    The experiment employs an innovative exotic-atom-based identification method: incoming antinuclei are slowed and captured in the tracker material, forming exotic atoms. The resulting de-excitation X-rays, along with dE/dx and velocity measurements and the unique annihilation product topology, enable clear identification of the antinucleus species.
    GAPS will measure the antiproton flux with unprecedented statistics in a previously inaccessible energy regime, and it will be the first experiment optimized for the detection of cosmic antideuterons—a potential "smoking gun" for new physics. Additionally, it will provide leading sensitivity to antihelium.
    GAPS is scheduled to launch during the Antarctic summer season 2025/26 and is currently sitting at the Long Duration Balloon facility at McMurdo Station, following an extensive ground calibration campaign completed in the 2024/25 season.
    This talk will present an overview of the GAPS science goals, recent calibration results from Antarctica, and an outlook on the upcoming science flight and its potential impact on the fields of cosmic ray physics and dark matter detection.
    
    Ponente: Elena Vannuccini (INFN Florence)
    
    TeVPA2025-Vannuccini.pdf
- 14:30 → 16:15
  Gamma Rays: Methods Salón de Actos (ADEIT)
  
  Salón de Actos
  
  ADEIT
  
  Moderador: David Green (CTAO)
  - 14:30
    
    Inferring the Source-Count Distributions and Spectra of the Unresolved Gamma-Ray Background with Simulation-Based Inference 15m
    
    The extragalactic background (EGB) observed by Fermi-LAT provides a detailed map of the non-thermal universe. We construct a simulation-based inference framework with the goal of characterizing the full information contained in the EGB. Using a convolutional neural network method, we provide the first simultaneous inference of the energy spectrum and source-count distribution (SCD) for the underlying EGB populations. Our method has the flexibility to account for correlations introduced by the telescope’s point-spread function. Our predicted EGB spectra is consistent with that found by the Fermi calibration, whereas our SCD maintains sensitivity to dimmer sources than in previous works. By simulating blazars and star-forming galaxies, we train the neural network to distinguish between populations based on their spectral shape and infer the relative abundance of each population. Validating this method in the clean high latitude region paves the way towards extending the method towards noisier environments, such as the Galactic center.
    
    Ponente: Eve Schoen (UC Berkeley / LBNL, USA)
    
    tevpa2025.pdf
  - 14:45
    
    Multi-class classification of unassociated Fermi LAT sources with machine learning and the puzzle of soft Galactic unassociated sources 15m
    
    About half of the Fermi-LAT gamma-ray sources within plus or minus 10 degrees in latitude from the Galactic plane are unassociated. Interestingly, the distribution of the Galactic unassociated sources as a function of spectral parameters is different from the distributions of known classes of Galactic sources, such as pulsars, supernova remnants, and pulsar wind nebulae. This difference in distributions is not only puzzling from the point of view of known classes of gamma-ray emitters, it is also a challenge for standard machine learning classification, where it is assumed that the distributions of training and target datasets are the same. In this talk I will discuss how machine learning can be used in modeling Galactic unassociated sources taking into account dataset shifts between training and target distributions and what such models can tell us about the physical nature of low-latitude unassociated sources.
    
    Ponente: Dmitry Malyshev (ECAP, Erlangen, Germany)
    
    2025-11_Malyshev_LAT_unas_PS_ML_TeVPA.pdf
  - 15:00
    
    Recovering population properties of gamma-ray sources in the presence of biased data 15m
    
    Galactic cosmic-ray accelerators are identified efficiently by gamma-ray observations of space-borne and ground-based instruments. The gamma-ray sources observed so far, however, represent only the tip of the iceberg, a highly biased sample of the brightest and closest sources. Studying the population as a whole requires careful evaluation of the available data and their biases, stemming from the detection thresholds of the involved instruments. In this presentation I will outline and quantify the problem based on simulations, present a procedure to derive population properties and give examples for the application to individual source classes and their spatial and acceleration properties.
    
    Ponente: Kathrin Egberts (University of Potsdam)
    
    2025-10-TeVPA.pdf
  - 15:15
    
    An event-type based analysis for LST-1 15m
    
    The analysis generally applied to Imaging Atmospheric Cherenkov Telescopes data optimizes quality selection cuts, selecting a sub-sample of high-quality events, and computes a set of Instrument Response Functions (IRFs) for these events. All surviving events are treated as equal in quality, and are assumed to be well represented by a single set of IRFs, while the rest of the events are discarded. A different approach, already proven successful by experiments such as Fermi-LAT, is an event-type based analysis. It consists of separating the events in subsamples according to their expected reconstruction quality and generating IRFs for each subsample. At the science tools level, these subsamples are analysed jointly and treated as independent observations, each with their own set of IRFs.
    
    In this work we explore the use of machine learning techniques to estimate event reconstruction quality. A model predicts the error on the angular reconstruction of each event. Events are ranked according to their expected angular reconstruction quality, and separated into different partitions. Using simulations of the future Cherenkov Telescope Array Observatory (CTAO), this procedure has already been proven to significantly boost both angular resolution and energy resolution. We present an implementation of this methodology for a set of Crab Nebula data acquired by The Large-Sized Telescope prototype (LST-1) with the goal to test the performance of the event-type based analysis.
    
    Ponente: Silvia García Soto (Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT))
    
    ET_silvia_TEVPA_2025_v2.pdf
  - 15:30
    
    Improving LST-1 Sensitivity on Real Data Using Deep Learning Techniques and CTLearn 15m
    
    The Cherenkov Telescope Array Observatory (CTAO) will be the next generation of very high energy (VHE) gamma-ray observatories, using Imaging Atmospheric Cherenkov Telescopes (IACTs) such as the LST-1 (Large-Sized-Telescope-1). In this contribution, we present a successful application of deep learning techniques for event reconstruction in real LST-1 data, using the CTLearn framework. The model is based on convolutional neural networks (CNNs) applied to calibrated images, allowing the precise estimation of physical event parameters such as energy, direction and gammaness (a score used in the selection of gamma-ray events over background).
    
    The results show a significant improvement in the differential sensitivity of LST-1 in the low energy range up to about 500 GeV, compared to classical methods based on Random Forests. This improvement is particularly reflected in better angular resolution, energy resolution, and improved the gammaness estimation, which directly contributes to the increase in sensitivity. The work demonstrates the potential of deep learning as a robust and effective tool for the analysis of real data in IACT telescopes and reinforces its applicability in operational scientific environments.
    
    Ponente: Cristian Pozo González (IAA - CSIC)
    
    Improvement the sensivility of LST1 CTLearn_pytorch.pdf
  - 15:45
    
    Performance and scientific evaluation of Gammalearn on LST-1 data 15m
    
    The Cherenkov Telescope Array Observatory (CTAO) marks the next generation of Imaging Atmospheric Cherenkov Telescopes (IACTs), offering a sensitivity increase of up to five to ten times over current instruments. Its first prototype, the Large-Sized Telescope (LST-1), is already in operation at the Roque de los Muchachos Observatory in La Palma, Spain. Deep learning methods have shown significant promise in reconstructing key properties of incident particles—such as energy, arrival direction, and type—using simulated data. Unlike traditional approaches that rely on simplified image shape parameters, deep learning can exploit the full temporal and charge information of the recorded events, providing enhanced performance, particularly at low energies (~20 GeV) accessible by LST-1. This capability is especially valuable for observing distant extragalactic sources like Active Galactic Nuclei, which are key to probing fundamental physics and cosmology. In this work, by producing sensitivity curves, we evaluate the performance of GammaLearn, a deep learning framework tailored for IACT data analysis (Vuillaume et al., 2021, ICRC), by comparing it to the standard analysis used with LST-1 and applying it to real observational data from LST-1.
    
    Ponente: Guillaume Grolleron (LAPP (CNRS))
    
    TeVPa2025 - Real data analysis with gammaLearn -8.pdf
  - 16:00
    
    Classifying Waveform MAGIC Telescope Data Using Graph Neural Networks 15m
    
    Graph Neural Networks (GNNs) have emerged as a robust architectural choice for deep learning across scientific disciplines, and are particularly suited for datasets with irregular topology. The MAGIC Telescope, comprising a pair of 17 m Imaging Atmospheric Cherenkov Telescopes (IACTs) located at Roque de Los Muchachos Observatory in La Palma, Spain, is designed to detect gamma rays from around 50 GeV to over 50 TeV. Arrays of IACTs rely on a complex pipeline in which each particle registered by the detectors generates a temporal stereo signal that must be calibrated, flattened into an image, cleaned, parameterized, and ultimately reconstructed by multiple machine learning algorithms. In recent years, Convolutional Neural Networks (CNNs) have shown great promise in performing full event reconstruction.
    
    In contrast, this study leverages the calibrated waveform data, consisting of a 30 ns signal in each pixel of the camera. Due to the unconventional geometry of the MAGIC cameras and asynchronous clocks between pixels, we represent MAGIC data as a point cloud graph and employ GNNs as a classification algorithm for the first time in an IACT. Our preliminary trials indicate that GNNs not only represent a robust method for reconstructing raw MAGIC data, but also show potential for fast online inference or even direct telescope triggering.
    
    Ponente: Jarred Green (Max Planck Institute for Physics)
    
    Green Jarred TeVPA 2025
- 14:30 → 16:15
  Neutrinos: Neutrino alerts & Standard neutrino physics Room 1.1+1.2 (ADEIT)
  
  Room 1.1+1.2
  
  ADEIT
  
  Moderador: Damiano Fiorillo
  - 14:30
    
    IceCat-2: Updated IceCube Event Catalog of Alert Tracks 15m
    
    The moment a neutrino event, likely of astrophysical origin, triggers a light emission in the glacial ice at the South Pole, the IceCube Neutrino Observatory issues a real-time alert to potential observers worldwide. The same filters that select alerts with track-like signatures were applied to the entire IceCube data sample from 2011 to 2023, leading to the public release of the IceCat-1 catalog. Several searches for potential astrophysical neutrino sources have been based on these alerts, with some even reporting evidence of neutrino emission. In 2024, the directional reconstruction used for real-time track alerts was updated, reducing the area of the 50%(90%) error regions by factors of 5(4), while also improving statistical coverage. This update, together with the addition of the latest alerts, motivated the creation of the IceCat-2 catalog. Here, we present preliminary results and correlation studies based on IceCat-2, which may shed new light on the puzzle of the origin of astrophysical neutrinos.
    
    Ponente: Giacomo Sommani (Ruhr-Universität Bochum)
    
    2025-11-014-TeVPA-2025-Sommani.pdf
  - 14:45
    
    The KM3NeT neutrino alert pipeline for multi-messenger astronomy 15m
    
    KM3NeT, a Cherenkov-based neutrino telescope sensitive to energies ranging from MeV to PeV, is currently under construction in the depths of the Mediterranean Sea. It comprises two detectors, KM3NeT/ARCA and KM3NeT/ORCA, already partially deployed and data taking; full completion is anticipated by the end of the decade. Its design provides a large field of view and high duty cycle, enabling it to address various physics goals, such as the search for astrophysical neutrino sources, the detection of very high-energy neutrinos, or a real-time monitoring of the sky, among others.
    
    The rise of time-domain astronomy and multi-messenger studies emphasizes the need for information systems capable of sharing observations in real-time. In these fields, concurrent observations across a broad spectrum are key to identifying new transient sources or validating models about them.
    By identifying interesting neutrino candidates, KM3NeT, thanks to its unique ability to observe the Galactic plane, along with its broad energy sensitivity and online analysis capabilities, could play a crucial role in this global effort.
    
    This contribution will detail the alert system developed by KM3NeT to share significant detections and enable follow-up campaigns within the astronomy community. We will describe the system’s architecture, the analysis strategies used to identify candidate events, the format and content of the alert messages, and the criteria and policy for issuing alerts.
    
    Ponente: Vincent Cecchini (IFIC - CSIC)
    
    talk_TeVPA2025_KM3NeTOnlineAlerts_CecchiniV.pdf
  - 15:00
    
    Advancing Multi-Messenger Astronomy: IceCube's Enhanced Real-Time Neutrino Alert System 15m
    
    The IceCube Neutrino Observatory, situated at the South Pole, plays a pivotal role in multi-messenger astronomy by continuously monitoring the entire sky for high-energy neutrinos. This presentation highlights recent advancements in IceCube's real-time alert system, particularly focusing on the Gamma-ray Follow-Up (GFU) program and the innovative Neutrino FlareWatch platform. These advancements build upon past successes, such as the observation of a multi-wavelength flare from blazar TXS 0506+056, triggered by an IceCube alert.
    
    The GFU program operates in two modes: the "Source List" mode, targeting known high-energy emission sources, and the "All-sky" mode, searching for exceptional neutrino emissions across the sky. Recent improvements include developing methods to report angular uncertainty in "all-sky" alerts. A new, expanded list of target sources now includes X-ray bright AGN and binary systems alongside gamma-ray bright AGN, enhancing search sensitivity and broadening scientific engagement. A significant development is the transition of GFU cluster alerts from private sharing to public accessibility. The new Neutrino FlareWatch platform, a modern web-based interface, will provide real-time, interactive access to GFU alerts. This presentation will introduce the new GFU alert system, the Neutrino FlareWatch platform, and discuss their implications for future multi-messenger astronomy research.
    
    Ponente: Elisa Bernardini (Padova University & INFN)
    
    TeVPa_IceCube_alerts_Bernardini.pdf
  - 15:15
    
    Gamma rays as leptonic portals to energetic neutrinos: a new Monte Carlo approach 15m
    
    High center-of-mass electromagnetic (EM) interactions could produce decaying heavy leptons and hadrons, leading to neutrino generation. These processes might occur in the most extreme astrophysical and cosmological scenarios, potentially altering the expected gamma-ray and neutrino fluxes in both the hadronic and the leptonic pictures. For instance, neutrinos could arise from high-redshift EM cascades, triggered by gamma rays beyond $10^{18} \; \text{eV}$ scattering background photons, from low-radio to ultraviolet energy bands. Such energetic gamma rays are predicted in cosmogenic models and in scenarios involving non-standard physics. On astrophysical scales, leptonic production of neutrinos could take place in active galactic nuclei cores, where several-TeV gamma rays interact with the X-ray photons from the hot corona. We explore these scenarios within the CRPropa Monte Carlo code framework, developing dedicated tools to account for leptonic production and decay of heavy leptons and hadrons. In particular, decays are performed in synergy with the PYTHIA event generator. With these novel tools, we characterise the spectrum and flavour composition of neutrinos emerging from cosmological EM cascades and from leptonic processes in inner core of active galactic nuclei. Finally, we investigate the leptonic production of neutrinos in the context of the IceCube detection of NGC 1068.
    
    Ponente: Gaetano Di Marco (IFT UAM/CSIC)
    
    EMcascadeNeutrino2_TeVPA25_GDiMarco.pdf
  - 15:30
    
    Earth Tomography Results Using High-Energy Atmospheric Neutrinos at IceCube 15m
    
    The IceCube Neutrino Observatory has selected a sample of very pure, primarily atmospheric, predominantly muon neutrino events over 11 years from all directions below the horizon, spanning the energy range 500 GeV to 100 TeV. These neutrinos traverse the earth and are attenuated in varying amounts depending on their energy and traversed column density. By parameterizing the earth as multiple constant-density shells, IceCube can measure the upgoing neutrino flux as a function of the declination, inferring the density of each shell. In this talk, we present the results of a Bayesian analysis using this approach, including measurements of the Earth’s density profile, mass, and moment of inertia. In addition, the analysis procedure, details about the data sample, and systematic effects are also discussed. This analysis represents the latest, weak-force driven, non-gravitational measurement of the earth’s density, mass, and moment of inertia.
    
    Ponente: Alex Wen (Harvard University)
    
    2025_Nov_TeVPA_Parallel_AlexWen.pdf
  - 15:45
    
    Prompt atmospheric leptons and the potential role of intrinsic charm 15m
    
    The all-sky very-high energy ($10^4$ - $10^6$ GeV) atmospheric muon flux, most recently measured by IceCube, shows a spectral hardening in the higher energy range, indicating a prompt component. Since the atmospheric muon neutrino flux at high energy, also measured by IceCube, is dominated by the astrophysical flux, only upper bounds on the prompt atmospheric muon neutrino flux contribution are currently available. We provide a new evaluation of the prompt atmospheric muon flux including for the first time an intrinsic charm component to the colliding nucleons. This increases forward production of $\bar D^0$, $D^-$ and $\Lambda_c$ which decay into final states that can contain muons and muon neutrinos. We show how the increase in the prompt muon flux due to intrinsic charm has an associated increase in the prompt muon neutrino flux. We implement the models of Brodsky-Hoyer-Peterson-Sakai and the Regge ansatz for intrinsic charm in MCEq, used for the calculation of the lepton fluxes. The challenges of obtaining predictions that are simultaneously consistent with IceCube's high energy atmospheric muon flux measurements and their upper bound on the prompt muon neutrino flux are discussed and the discrepancies are quantified.
    
    Ponente: Günter Sigl (University of Hamburg)
    
    atmospheric-leptons-IC.pdf
  - 16:00
    
    Charm Production in IceCube and its Implications for Astrophysical Tau Neutrino Searches 15m
    
    Tau neutrinos, being most likely of astrophysical origin, plays a crucial role in solving cosmic‐ray–related puzzles. In IceCube, iterations of searches for tau neutrinos via their characteristic “double-cascade” / "double pulse” morphology have been conducted. However, this signature is not unique to tau neutrinos: the much less studied charmed production can lead to a similar signature due to the D meson’s similar decay lifetimes with tau leptons. Furthermore, D mesons constitute about 10 % of all deep inelastic scattering (DIS) events. Beyond serving as a background to tau searches, D mesons are interesting in their own right—studying them provides insights into D–nucleon scattering at very high energies and constrains the intrinsic strange content of the nucleon. In this talk, we present a preliminary study of an inclusive search for D mesons and tau neutrinos in IceCube, covering the charm production simulation, an inclusive event selection, and implications for astrophysical tau‐neutrino searches.
    
    Ponente: Miaochen Jin (Harvard University)
    
    Inclusive Search for Taus and Charmed Hadrons in IceCube.pdf
- 16:15 → 16:45
  
  Coffee Break 30m ADEIT
  
  ADEIT
- 16:45 → 18:30
  Connections to Particle Physics Salón de Grados (ADEIT)
  
  Salón de Grados
  
  ADEIT
  
  Moderador: Jordi Salvadó (Universitat de Barcelona)
  - 16:45
    
    Dark Matter in an Evanescent Three-Brane Randall-Sundrum Scenario 15m
    
    Apart from its gravitational interactions, dark matter (DM) has remained so far elusive in laboratory searches. One possible explanation is that the relevant interactions to explain its relic abundance are mainly gravitational. In this work we consider an extra-dimensional Randall-Sundrum scenario with a TeV-PeV IR brane, where the Standard Model is located, and a GeV-TeV deep IR (DIR) one, where the DM lies. When the curvatures of the bulk to the left and right of the IR brane are very similar, the tension of the IR brane is significantly smaller than that of the other two branes, and therefore we term it ``evanescent". In this setup, the relic abundance of DM arises from the freeze-out mechanism, thanks to DM annihilations into radions and gravitons. Focusing on a scalar singlet DM candidate, we compute and apply current and future constraints from direct, indirect and collider-based searches. Our findings demonstrate the viability of this scenario and highlight its potential testability in upcoming experiments. We also discuss the possibility of inferring the number of branes if the radion and several Kaluza-Klein graviton resonances are detected at a future collider.
    
    Ponente: Alejandro Muñoz Ovalle (IFIC, CSIC-UV)
    
    Charla_TeVPA.pdf
  - 17:00
    
    Cosmic Gravitational Waves as Tracers of Leptogenesis 15m
    
    Gravitational Waves (GWs) provide a remarkable perspective into the physics of the early Universe and could serve as an innovative means of investigating high-scale leptogenesis theories. In this presentation, I will examine how GW observations can can shed light on a class of GUT-inspired seesaw models based on the $U(1){B-L}$ gauge symmetry. Within these models, the scalar field $\Phi$, which is responsible for the spontaneous symmetry breaking of $U(1) {B-L}$, generates Majorana masses $M_N$ for right-handed neutrinos. Furthermore, when this scalar field has a weak coupling to the Standard Model Higgs, it naturally gives rise to an epoch of early matter domination that is closely linked to the leptogenesis scale $M_N$. This connection encodes vital information regarding various phases of flavored leptogenesis. In this context, GWs are produced by cosmic strings linked to the $U(1)_{B-L}$ gauge symmetry breaking and by the enhancement of primordial density fluctuations during the early matter-dominated epoch. I will illustrate how the characteristics and spectral features of the resultant GW background are influenced by the underlying leptogenesis scale $M_N$. A prospective detection of GWs across several frequency ranges could thus provide exclusive understanding of the origins of the matter-antimatter imbalance. Even in the absence of a detectable signal, stringent constraints could be imposed on the leptogenesis parameters that are typically unreachable through standard observational methods.
    
    Ponente: Ninetta Saviano (INFN)
    
    gw_lepto_Valencia.pdf
  - 17:15
    
    Primordial black hole probes of heavy neutral leptons 15m
    
    Primordial black holes (PBH), while still constituting a viable dark matter component, are expected to evaporate through Hawking radiation.
    Assuming the semi-classical approximation holds up to near the Planck scale, PBHs are expected to evaporate by the present time, emitting a significant flux of particles in their final moments, if produced in the early Universe with an initial mass of $\sim 10^{15}$ g.
    These ``exploding'' black holes will release a burst of Standard Model particles alongside any additional degrees of freedom, should they exist.
    We explore the possibility that heavy neutral leptons (HNL), mixing with active neutrinos, are emitted in the final evaporation stages.
    We perform a multimessenger analysis. We calculate the expected number of active neutrinos from such an event, including contributions due to the HNL decay for different assumptions on the mixings, that could be visible in IceCube. We also estimate the number of gamma-ray events expected at HAWC. By combining the two signals,
    we infer sensitivities on the active-sterile neutrino mixing and on the sterile neutrino mass. We find that, for instance, for the scenario where $U_{\tau 4}\neq 0$, IceCube and HAWC could improve current constraints by a few orders of magnitude, for HNLs masses between 0.1 - 1 GeV, and a PBH explosion occurring at a distance of $\sim 10^{-4}$ pc from Earth.
    
    Ponente: Agnese Tolino (IFIC, CSIC-UV)
    
    PBH probes of HNLs-TeVPA25-Tolino.pdf
  - 17:30
    
    Revisiting Magnetic Monopole Bounds in Light of New Constraints on the Intergalactic Magnetic Field 15m
    
    The Intergalactic Magnetic Field (IGMF), though significantly weaker than the Galactic Magnetic Field (GMF), is believed to permeate the vast cosmic voids. Recent experimental developments have provided both upper and lower bounds on the IGMF, motivating us to revisit the scenario in which Magnetic Monopoles (MMs) are accelerated by these large-scale fields. In this work, we analyze MM acceleration in the IGMF and GMF, finding that the inclusion of IGMF effects calls for an update of the long-standing Parker bound.
    
    Magnetic Monopoles—predicted in several extensions of the Standard Model—offer a compelling probe of cosmic magnetic fields. By modeling their acceleration mechanisms, we establish a unified framework connecting monopole mass, flux, and velocity at Earth. This approach allows us to reinterpret current experimental constraints, often reported in terms of Lorentz factor, in a more physically comprehensive manner.
    
    Particular emphasis will be placed on the sensitivity of present and future Imaging Atmospheric Cherenkov Telescopes (IACTs), such as the Cherenkov Telescope Array (CTA), in the search for MMs.
    
    Ponente: Michele Doro (University of Padova)
    
    doro_2025_tevpa_monopoles.pdf
  - 17:45
    
    Latest Results from CUORE and Progress towards CUPID 15m
    
    The search for neutrinoless double beta decay (0νββ) is fundamental for investigating lepton-number violation, probing new physics beyond the Standard Model, and determining whether neutrinos are Majorana particles. CUORE, a cryogenic bolometric experiment at LNGS, studies 0νββ in $^130$Te using 988 TeO$_2$ crystals. It is a milestone of cryogenic detector arrays with a tonne-scale detector operated for more than 7 years below 15 mK. Since 2017, CUORE has accumulated over 2.5 tonne-years of exposure, achieving one of the leading 0νββ limits and one of the most precise two-neutrino double beta decay (2νββ) half-life measurements thanks to a detailed background reconstruction across a broad energy range. Building on CUORE's success, CUPID (CUORE Upgrade with Particle IDentification) aims to significantly enhance its 0νββ discovery sensitivity to 10 27 yr in 100 Mo, covering the Inverted Hierarchy of neutrino masses. It will employ 1596 lithium molybdate (Li$_2$MoO$_4$) crystals enriched in 100 Mo, alongside 1710 light detectors with Neganov-Trofimov-Luke amplification, enabling simultaneous heat and light readout for enhanced background rejection, particularly against alpha contamination and 2νββ pileup. CUPID will reuse CUORE's cryostat and infrastructure. Current efforts focus on detector performance validation, sensitivity studies, and finalizing the experimental design to maximize physics reach. This work presents the latest CUORE results and outlines the key milestones toward CUPID's realization.
    
    Ponente: Dounia Helis (INFN-LNGS)
    
    TeVPA_2025_Dounia_Helis_final.pdf
  - 18:00
    
    Floating Into the Unknown: Levitated Sensors for New Physics 15m
    
    Magnetic levitation technology offers force and displacement sensitivities at the quantum frontier, making it an attractive platform for probing the feeble interactions expected of beyond the Standard Model physics. Despite its promise, the case for magnetic levitation in fundamental physics applications is only just being built. In this talk, I will introduce two new experiments based on the Meissner levitation of a ferromagnet within a superconducting trap: POLONAISE (Probing Oscillations using Levitated Objects for Novel Accelerometry In Searches
    of Exotic physics) and MORRIS (Magnetic Oscillatory Resonator for Rare-Interaction Studies). I will show how these experiments will have world-leading sensitivities to three fundamental physics cases: the hunt for ultralight dark matter, ultraheavy dark matter, and a non-Newtonian gravitational fifth force. I will present the results from the first searches for ultralight and ultraheavy dark matter using magnetic levitation technology around the dark matter masses $m \sim 10^{-13}\,\mathrm{eV}/c^2$ and $m\sim 10^{14}\,\mathrm{GeV}/c^2$, respectively. I will also show new constraints on fifth forces at $\mathcal{O}(\mathrm{mm})$ scales - currently the most sensitive in this regime. Our results demonstrate the power of magnetic levitation as a frontier tool for fundamental physics, opening new avenues for precision tests of physics and the hunt for dark matter.
    
    Ponente: Dorian Amaral (IFAE, Barcelona; Rice University, Texas)
    
    dwpa_TeVPA_2025.pdf
  - 18:15
    
    Dark models and bright tools to address the stochastic gravitational waves background observation 15m
    
    The evidence of a Stochastic Gravitational Wave Background (SGWB) in the nHz frequency range is posed to open a new window on the Universe. A preferred explanation relies on a supercooled first order phase transition at the 100 MeV–GeV scale. I will address the feasibility of this solution by discussing viable dark sectors and their constraints, going from the particle physics model to the production of the gravitational waves, by also taking into account the challenges faced by a supercooled first order phase transition explanation.
    I will also present ELENA, a new public software that allows for a fast and precise computation of the first order phase transition dynamics and gravitational waves spectrum, by employing the tunnelling potential formalism instead of the commonly used bounce equations. ELENA allows to compute the SGWB starting from a Lagrangian input, while going beyond several simplifying assumptions often employed in the literature.
    
    Ponente: Michele Lucente (University of Bologna)
    
    Lucente_TeVPA.pdf
- 16:45 → 18:30
  Cosmic Rays Room 2.1+2.2 (ADEIT)
  
  Room 2.1+2.2
  
  ADEIT
  
  Moderador: Maurizio Spurio (University of Bologna (Italy) and INFN)
  - 16:45
    
    From Ground to Space: The JEM-EUSO Program for UHECRs and Astrophysical Neutrinos 15m
    
    Since 2010, the JEM-EUSO (Joint Exploratory Missions for Extreme Universe Space Observatory) collaboration has been developing an ambitious program to observe Ultra-High-Energy Cosmic Rays (UHECRs) and related phenomena from space. These particles, with energies exceeding 10²⁰ eV, carry crucial information about the most extreme astrophysical environments, yet are difficult to study due to their extremely low flux.
    The collaboration’s primary goal is to develop a space-based observatory equipped with an ultra-fast, high-sensitivity UV camera, capable of detecting extensive air showers generated when UHECRs interact with the Earth’s atmosphere. A dedicated Cherenkov camera has also been developed to evaluate the feasibility of the Earth-skimming technique from high altitudes. Fluorescence and Cherenkov detectors can be combined into a hybrid detection system, enhancing observational capabilities. Observing from orbit allows for a significant increase in exposure and near-uniform full-sky coverage, complementing ground-based efforts.
    The JEM-EUSO collaboration follows a multi-platform strategy. Ground-based (EUSO-TA) and balloon-borne missions (EUSO-Balloon, EUSO-SPB1, EUSO-SPB2) have tested key technologies and validated detection techniques, while the space-based Mini-EUSO instrument aboard the ISS has delivered valuable data on UV backgrounds, transient luminous events, meteoroids, and more. These pathfinder missions have laid the groundwork for future large-scale projects, including M-EUSO and POEMMA (Probe Of Extreme Multi-Messenger Astrophysics). The upcoming PBR (POEMMA Balloon with Radio) mission, scheduled for launch in 2027, will add a radio-detection capability to the program.
    This presentation will summarize the scientific and technological milestones of the JEM-EUSO program, highlight updated objectives based on recent findings, and outline the roadmap toward space-based UHECR astronomy and broader multi-messenger exploration—including studies of meteoroids, nuclearites, and strange quark matter.
    
    Ponente: Valentina Scotti (Università di Napoli Federico II - INFN Napoli)
    
    JEM-EUSO_TeVPA_Scotti.pdf
  - 17:00
    
    The Terzina Telescope on board the NUSES mission: A Pathfinder for the Detection of EAS Cherenkov Light from Space 15m
    
    Ultra-high energy cosmic rays (UHECRs) above 100 PeV can be detected from space by looking towards the Earth's limb, where the optical emission from extensive air showers (EAS) can be observed. Space-based experiments can also play a crucial role in the multi-messenger astrophysics era, particularly through the detection of Earth-skimming neutrinos. Validating the observational techniques used to detect such rare UHE events involves precursor missions such as NUSES: a satellite mission designed to operate in a sun-synchronous, quasi-polar low Earth orbit.
    Two payloads will be installed on board the satellite platform, developed by Thales Alenia Space–Italia (TAS-I): Terzina, which is the main focus of this contribution, and ZIRE’, which is dedicated to low-energy cosmic and gamma rays, space weather, and the study of magnetosphere–ionosphere–lithosphere interactions.
    The Terzina telescope is a compact Schmidt-Cassegrain Cherenkov instrument designed to observe the Cherenkov light produced by EASs in the Earth's atmosphere. Its focal plane camera is equipped with an array of Silicon Photomultipliers (SiPMs), enabling precise detection of fast optical signals. The instrument is capable of observing two distinct types of events: when pointing above the Earth's limb, it detects EASs generated by UHECRs; when pointing below the limb, it targets upward-going showers produced by Earth-skimming neutrinos.
    To evaluate Terzina’s performance, a full Monte Carlo simulation chain has been implemented, including Cherenkov signal modeling, trigger logic, and particle interaction simulations. A key component is the optical validation performed in Geant4 using the dedicated OpticsLibSim library, developed to accurately reproduce the telescope’s optical response.
    Studies have focused on the instrument’s aperture and performance, highlighting its effective collection area and angular response — critical parameters for determining sensitivity to UHECRs and neutrinos. These results validate the current design and support the development of future large-scale space-based observatories.
    
    Ponente: Caterina Trimarelli (GSSI - LNGS INFN)
    
    terzina_tevpa.pdf
  - 17:15
    
    The PBR Mission: the balloon-borne precursor of the space-based POEMMA multi-messenger Observatory 15m
    
    The main objective of the international JEM-EUSO (Joint Exploratory Missions for Extreme Universe Space Observatory) Collaboration is to develop a large mission with dedicated instrumentation looking down on the Earth atmosphere from space, both towards nadir and/or towards the limb, to detect the Extensive Air Shower (EAS) and the High Altitude Horizontal Airshowers (HAHA) initiated by Ultra-High-Energy Cosmic Ray (UHECR) and Very-High-Energy Neutrino (VHEN). In the last decade, the JEM-EUSO Program successfully developed five intermediate missions: one ground based (EUSO-TA), three balloon-borne (EUSO-Balloon, EUSO-SPB1, EUSO-SPB2) and one space-based (MINI-EUSO). The new balloon-borne mission PBR (POEMMA-Balloon with Radio) represents a huge leap in the direction of a space-based full-scale mission: the stereo double telescope Probe Of Extreme Multi-Messenger Astrophysics (POEMMA), a multi- messenger observatory to be considered for a NASA Probe Mission in the next decade. Already approved and funded by the USA space agency, the PBR mission is a Ultra-Long Duration Balloon payload scheduled for launch in Spring 2027 from Wanaka, New Zealand over the Southern Ocean for expected 50 days. The PBR mission is a real precursor of the POEMMA observatory, accomodating a multi-hybrid detector (Cherenkov and fluorescence telescopes, Radio and X/Gamma detectors), properly adpated on board, and aspiring to primary scientific goals: observation of EASs and HAHAs induced by UHECRs and search for VHENs. In this contribution, the paylod and its detectors, the corresponding advances in their assembling and completion in view of the pre-flight tests and studies of performances, in addition to the expected scientific results, will be described in detail.
    
    Ponente: Rossella Caruso (Department of Physics and Astronomy "E.Majorana" - University of Catania & INFN-CT)
  - 17:30
    
    GRAND and latest progress of its prototype array 15m
    
    GRAND is a planned large-scale, worldwide radio array designed for autonomous self-triggered detection of ultra-high-energy cosmic rays and neutrinos. GRANDProto300 is one of pioneering prototype array of the GRAND experiment. It consists of 300 radio antennas and will cover an area of (200\, \text{km}^2) in a radio-quiet region of western China. Serving as a test bench for the GRAND experiment, GRANDProto300 aims to achieve autonomous radio detection and reconstruction of highly inclined air showers. It is designed to detect ultra-high-energy cosmic rays in the energy range of (10^{16.5} - 10^{18}\, \text{eV}) at a rate comparable to that of the Auger Observatory. Over the past two years, significant improvements have been made to both the hardware and firmware of GP300. Currently, 65 antenna units have been deployed at the site. We present the current status of detector commissioning, including updates on hardware, calibration results such as GPS timing and antenna positioning. Additionally, we discuss the solar radio bursts associated with solar flares, the galactic radio emissions detected, and preliminary cosmic ray candidates.
    
    Ponente: Pengxiong Ma
    
    TeVPa2025_GRAND_Pengxiong_HR.pdf
  - 17:45
    
    Observation of In-ice Askaryan Radiation from High-Energy Cosmic Rays 15m
    
    We present the first experimental evidence for in-ice radiofrequency emission from cosmic-ray-induced high-energy particle cascades developing in the Antarctic ice sheet. In 208 days of data recorded with the phased-array trigger of the Askaryan Radio Array, we detect 13 events with impulsive radiofrequency pulses originating from below the ice surface. Considering only the arrival angles and timing properties, this rate is inconsistent with the a-posteriori expectation of the combined background from thermal noise events and impulsive on-surface events at the level of 3.5 𝜎, rising to 5.1 𝜎 when additionally considering impulsivity. The observed event geometry, event rate, signal shape, spectral content, and electric field polarization are consistent with Askaryan radiation from cosmic ray air shower cores impacting the ice sheet. For the brightest events, the angular radiation pattern independently favors an extended cascade-like emitter over a pointlike source.
    
    Ponente: Nathaniel Alden (University of Chicago)
    
    TeVPA_2025_CRs.pdf
  - 18:00
    
    Combined radio and radar signal study for the Radar Echo Telescope for Cosmic Rays (RET-CR) 15m
    
    The Radar Echo Telescope for Cosmic Rays (RET-CR) is a pathfinder experiment deployed at the Summit Station in Greenland, with a full data-taking run conducted in the summer of 2024. This experiment utilises the radar technique to search for an in-ice secondary cascade produced when the core of a high-energy cosmic ray air shower propagates into the high-altitude ice sheet.
    Detecting a complementary in-ice cascade from an air shower will help verify the radar technique in nature and contribute to the ultimate goal of establishing the Radar Echo Telescope for Neutrinos (RET-N).
    
    For both RET-CR and RET-N, we would also observe the radio emissions from the particle showers at the receivers.This includes the in-air radio emissions from the cosmic ray air shower as well as the Askaryan emissions from the in-ice secondary cascade. To effectively study the signal at the receivers, it is crucial to understand the radar signal in conjunction with the combined radio background from the particle cascades themselves. This contribution focuses on the combined study of radar and radio emission backgrounds at the Radar Echo Telescope for Cosmic Rays
    (RET-CR).
    
    Ponente: Krishna Nivedita Gopinath (Radboud University, Netherlands)
    
    TeVPA_Krishna.pdf
  - 18:15
    
    Radio Signatures of Cosmic-Ray Particle Showers in Deep In-Ice Antennas 15m
    
    To detect ultra-high-energy neutrinos, experiments such as the Askaryan Radio Array (ARA) and the Radio Neutrino Observatoy in Greenland (RNO-G), target the radio emission induced by these particles as they cascade in the ice, using deep in-ice antennas at the South Pole or in Greenland. In this context, it is essential to first characterize the in-ice radio signature from cosmic-ray-induced particle showers, which constitute a primary background for neutrino detection, and represent the fist in-situ detection of in-ice particle cascades with radio antennas. This characterization will help validate the detection principle and assist in calibration. To achieve this goal, we used FAERIE, the “Framework for the simulation of Air shower Emission of Radio for in-Ice Experiments” that combines CoREAS and GEANT4 to simulate the radio emission of cosmic ray showers deep in the ice. Using this tool, we analyze in-ice radio signatures of cosmic-ray showers, including polarization, timing, and radiation energy, as well as their dependence on shower parameters. These insights will facilitate the first cosmic-ray detections and improve cosmic-ray/neutrino discrimination.
    
    Ponente: Simon Chiche (Inter-University Institute For High Energies)
    
    TeVPA2025_SimonChiche.pdf
- 16:45 → 18:30
  Dark Matter: Indirect Detection: Photons II Room 3.1+3.2 (ADEIT)
  
  Room 3.1+3.2
  
  ADEIT
  
  Moderador: Christopher Cappiello
  - 16:45
    
    Invited: Ten years of Indirect Dark Matter searches at TeV scales with HAWC 15m
    
    While there exists overwhelming evidence pointing to the existence of dark matter (DM) as one of the components of the Universe, “what is the nature of DM?”, remains as one of the unsolved puzzles of modern physics. Several hypotheses and theories propose a new kind of particle to explain DM. Among them, candidates as Weekly Interactive Massive Particles (WIMPs), and ultra-light DM as Axion-like Particles (ALPs) or Dark Photons are the best candidates to explain totally or partially the DM under the context of the Lambda-CDM cosmological model. Footprints of these hypothetical particles should be found at the TeV gamma-ray scales where observatories such as HAWC operate. In this talk, we will review the results of the different indirect searches of DM using HAWC observations of extragalactic and galactic sources and the constraints on the parameters of WIMPs and ALPs.
    
    Ponente: Sergio Hernández Cadena (Tsung-Dao Lee Institute)
    
    hawcTevPA2025.pdf
  - 17:00
    
    Sensitivity of the Cherenkov Telescope Array Observatory to Dwarf Irregular Galaxies 15m
    
    Dwarf irregular galaxies (dIrrs) are rotationally supported galaxies, located in the Local Volume, and are considered to host star-forming regions with a low star-forming rate. Their gamma-ray background signal is expected to be low, making them interesting targets for WIMP Dark Matter (DM) indirect searches. Following previous works on dIrrs, we present the best four dIrrs targets for the forthcoming Cherenkov Telescope Array Observatory (CTAO). Since dIrrs have not been detected yet in gamma rays, in this work, we first explore the detection prospects of dIrrs as astrophysical emitters. Secondly, because the cusp-core problem is important for these objects, we compute the sensitivity prospects to a DM annihilating signal adopting both profiles, including halo substructures. Finally, we show that our DM sensitivity results are competitive with benchmark targets such as galaxy clusters.
    
    Ponente: Jaume Zuriaga-Puig (IFT UAM/CSIC)
    
    TeVPA2025_Jaume_ZuriagaPuig.pdf
  - 17:15
    
    WIMP Dark Matter's Michelson-Morley Moment 15m
    
    The next decade will definitively test the “minimal” dark matter
    paradigm. This is the attractive idea that extending the Standard
    Model with a new electroweak multiplet allows for a simple resolution
    of the Universe’s missing mass puzzle by a thermal relic particle.
    We project CTAO limits for all real SU(2) multiplets consistent with
    unitarity and find that with 500 hours of Galactic Center data, all
    can be excluded, except for the most massive, the 13-plet, as a
    borderline case. I also present new experimental limits for wino
    (3-plet) and 5-plet dark matter from the VERITAS IACT’s observations
    of dwarf spheroidal galaxies (dSphs). The former are comparable to
    other dSphs limits and suggest that a collaboration among existing
    experiments may exclude the thermal relic wino before the completion
    of CTAO South.
    
    Ponente: Matthew Baumgart
    
    wimpTeVPA2025.pdf
  - 17:30
    
    Probing Axion-Like Particles with LST-1 Observations of Multiple Blazars 15m
    
    Axions and axion-like particles (ALPs) are hypothetical particles predicted by several extensions of the Standard Model and compelling dark matter candidates. Their conversion into photons in the presence of magnetic fields can leave distinctive imprints on the photon spectra of astrophysical sources. In gamma-ray astronomy, photon-ALP conversions may produce observable energy-dependent features from GeV to TeV energies. In this study, we search for these signatures in the spectra of four blazars — Mrk 421, Mrk 501, BL Lacertae, and 1ES 1959+650 — using the first Large-Sized Telescope (LST-1) of the future Cherenkov Telescope Array Observatory (CTAO). Our photon-ALP conversion model includes magnetic fields in the relativistic jets, attenuation from the extragalactic background light, and the magnetic field of the Milky Way. Results from individual sources are combined at the likelihood level to derive joint constraints on the ALP parameter space.
    
    Ponente: Ivana Batković (University of Padova & INFN Padova)
    
    TeVPa_Batkovic.pdf
  - 17:45
    
    Gamma rays from the Galactic Center strongly constrain thermal relic dark matter 15m
    
    Under the hypothesis that thermal relic particles populate the dark matter halo of the Milky Way, strong indirect signals in cosmic radiation are expected from the regions where the dark matter density is high. In particular, the Galactic Center is potentially hosting the largest indirect signal from dark matter pair-annihilation (or decay), which in many theoretically well-motivated models would produce gamma rays as their final states. More than a decade ago, an unexpected gamma-ray component over astrophysical backgrounds was detected at GeV energies towards the Galactic Center in the data of the Fermi Large Area Telescope. Initially, this excess was considered to be hinting at GeV thermal relics annihilating in the Galactic dark matter halo. However, by using the most advanced analysis techniques and models for the astrophysical backgrounds, recent works have demonstrated that the excess is better explained by a population of millisecond pulsar-like sources in the Galactic bulge. Building on the preference for an explanation in terms of a dim millisecond pulsar bulge population, we present new, strong constraints on thermal relic dark matter that robustly account for and mitigate astrophysical modelling uncertainties of gamma-ray emission in the inner Galaxy. This is achieved by combining adaptive template fitting and pixel count statistical methods to assess the role of sub-threshold point sources in the observed gamma-ray counts, while minimising the mis-modelling of Galactic diffuse emission backgrounds.
    
    Ponente: Christopher Eckner (CNRS/LAPTh)
    
    TeVPA2025_ECKNER.pdf
  - 18:00
    
    Primordial Black Hole evaporation search with MAGIC 15m
    
    Primordial Black Holes (PBHs) are hypothesized to have been formed in the Early Universe as a result of density fluctuations. In recent years, PBHs have gained attention, in part, for the possibility that they can account for a fraction or all the dark matter content of the Universe. PBHs formed with a mass around $10^{14}$g to $10^{15}$g should be evaporating in present times through the emission of Hawking radiation. Such a process leads to a bright burst of very-high-energy (VHE) particles. The primary and secondary VHE photons produced could be detected by gamma-ray experiments. However, no observational evidence has been found yet for PBH evaporation emission, with current upper limits on the local explosion rate set to $181\, \mathrm{pc}^{-3} \mathrm{yr}^{-1}$. In this talk I'll report on the search for PBH evaporation signals in 2000 hours of archival MAGIC data. I'll present the new search methodology, statistical techniques and results of the analyzed data.
    
    Ponente: Elia do Souto Espiñeira (CIEMAT)
    
    Elia_PBHs_MAGIC.pdf
  - 18:15
    
    Invited: CMB constraints on non-minimally coupled ultralight dark matter 15m
    
    In this talk, I will present bounds on the variation of fundamental constants from the cosmic microwave background (CMB). In our theoretically motivated model, the variation is modulated by a scalar field that behaves as an ultralight dark matter (ULDM). We self-consistently compute the effects of the variation of constants on big bang nucleosynthesis (BBN) and propagate those effects to the computation of the CMB spectra. We explore the degeneracies between various effects, such as changes in the primordial Helium fraction, changes due to modified recombination, and the effects on the ULDM. I will present the bounds on the variation of the electron mass and fine structure constant. I will also discuss the implications of the Hubble tension in this context.
    
    Ponente: Subhajit Ghosh (The University of Texas at Austin)
    
    SG_TeVPA_2025.pdf
- 16:45 → 18:30
  Gamma Rays Salón de Actos (ADEIT)
  
  Salón de Actos
  
  ADEIT
  
  Moderador: Judit Pérez-Romero (Center for Astrophysics and Cosmology/ University of Nova Gorica)
  - 16:45
    
    CTAO: The upcoming VHE gamma-ray observatory 15m
    
    The Cherenkov Telescope Array Observatory (CTAO) will be the world's first gamma-ray observatory with majority of observation time in the first 10 years driven by open proposals. Designed to operate for 30 years, with two sites, the Northern site at the Observatorio Roque de los Muchachos and the Southern site at the ESO Observatorio Paranal, CTAO will cover the entire sky with unprecedented sensitivity. Currently under construction, the acceptance of the first telescopes for CTAO is expected in the upcoming years with early Science from intermediate configuration to follow. Surpassing current Cherenkov telescope arrays, the intermediate configuration will produce groundbreaking science results. The early science program of the CTAO will place a strong emphasis on time-domain, multi-messenger and multi-wavelength astronomy. This contribution will provide an update on the status of the CTAO construction project, with a focus on the scientific capabilities of the first intermediate array configurations.
    
    Ponente: David Green (CTAO)
    
    CTAO_Status_TeVPa_2025_v2.pdf CTAO_Status_TeVPa_2025_v2.pptx
  - 17:00
    
    VHE Supernovae: state of the art and latest observations with the CTAO LST-1 and MAGIC telescopes 15m
    
    Core-collapse supernovae (CCSNe) are explosive astrophysical events that emit radiation across the entire electromagnetic spectrum, extending up to soft gamma rays. Very high-energy (VHE; E > 100 GeV) gamma-ray emission is expected to arise from shock interactions between dense circumstellar material and the supernova ejecta. However, no unambiguous detection has yet been achieved by past or current generations of imaging atmospheric Cherenkov telescopes (IACTs). A key limiting factor is gamma-gamma absorption, whereby VHE photons are attenuated through gamma-gamma interactions with low-energy photons from the supernova photosphere. This effect is particularly significant during the first tens to hundreds of days post-explosion, suppressing GeV–TeV emission.
    Current theoretical models suggest that with the enhanced sensitivity of the upcoming Cherenkov Telescope Array Observatory (CTAO), a bright CCSN could be detected up to distances of 10–70 Mpc after approximately 40 hours of integration time, depending on the strength of the shock interaction and the level of gamma-gamma attenuation. Among existing IACTs, the stereo configuration constituted by the Major Atmospheric Gamma-ray Imaging Cherenkov Telescopes (MAGIC), together with the CTAO’s first Large Sized Telescope (LST-1), stands out due to its low energy threshold and improved sensitivity in the GeV regime—where gamma-ray attenuation is less severe—making it the most promising current setup for detection.
    In this contribution, I will present the current state of CCSN observations at VHE, with a focus on the ongoing follow-up campaign carried out by the LST and MAGIC collaborations. I will highlight the most recent results, which demonstrate the capabilities of the MAGIC+LST-1 configuration and show its potential when combined with multiwavelength observations to improve our understanding of these explosive phenomena.
    
    Ponente: Andrea Simongini (INAF - Osservatorio Astronomico di Roma)
    
    Simongini_Tevpa-1.pdf
  - 17:15
    
    Unexpected Features of Solar Gamma-Ray Emission 15m
    
    Models predict that the Sun can produce bright gamma-ray emission through two separate mechanisms. First, ambient cosmic-ray protons can undergo hadronic interactions with the solar atmosphere producing a bright flux across the solar disk. Second, cosmic-ray electrons can inverse-Compton scatter ambient sunlight to gamma-ray energies.
    
    Observations by the Fermi-LAT and HAWC telescope have elucidated both components, and tracked their evolution across the solar cycle. We find that the inverse-Compton scattering emission from the Sun closely tracks theoretical expectations, verifying models of cosmic-ray transport in the inner heliosphere. The solar disk gamma-ray emission, on the other hand, has three surprising features. First, the gamma-ray emission extends to energies above 3 TeV, implying that Solar magnetic fields can redirect multi-TeV protons. Second, the morphology and spectrum of gamma-ray emission varies significantly over the solar cycle. Third, a significant “spectral-dip” appears between energies of 30-50 GeV. These observations are in significant tension with all current models of solar gamma-ray production.
    
    Ponente: Tim Linden (Stockholm University)
    
    tevpa2025_linden.pdf
  - 17:30
    
    MeV cosmic-ray electrons modify the TeV pair-beam plasma instability 15m
    
    Relativistic pair beams formed in the intergalactic medium (IGM) by TeV gamma rays from blazars are expected to generate a detectable electromagnetic cascade in the GeV range. However, this cascade is notably absent in the spectra of many hard-spectrum TeV blazars. One common explanation is that weak intergalactic magnetic fields deflect the resulting electron-positron pairs out of our line of sight. An alternative explanation suggests that electrostatic beam-plasma instabilities deplete the pairs' energy before a cascade can form. While recent studies indicate that scattering by oblique electrostatic modes causes minimal energy loss, these modes may be damped by linear Landau damping (LLD) due to the presence of MeV-scale cosmic-ray electrons in the IGM. In this study, we examine how LLD influences the energy-loss efficiency of plasma instabilities in pair beams from 1ES 0229+200. Our results show that LLD strongly suppresses oblique modes while allowing quasi-parallel modes to grow significantly, thereby boosting the instability’s energy-loss efficiency by over an order of magnitude.
    
    Ponente: Mahmoud Alawashra (DESY)
    
    Plasma_instability.PPTX
  - 17:45
    
    Combining Lorentz invariance violation of photons in the extragalactic propagation and in the detection stage 15m
    
    We investigate the effects of Lorentz invariance violation (LIV) on photon interactions, considering both intergalactic propagation (Breit-Wheeler process) and atmospheric interactions (Bethe-Heitler process). By incorporating LIV into the theoretical framework, we analyze how it modifies key quantities such as the cross section, threshold energy, and mean free path of photons traveling through intergalactic space. In addition, we study its impact on extensive air showers initiated by high-energy photons, demonstrating that LIV can alter the cross section of the primary interaction in the atmosphere. Additionally, we also test the photon interactions in the Earth crust, to evaluate if they can induce upward-going showers. Our results highlight the necessity of accounting for both propagation effects in intergalactic space and interactions in the atmosphere when evaluating LIV signatures. Even small deviations from Lorentz invariance can lead to measurable changes in astroparticle propagation and photon dynamics, offering new opportunities to test quantum gravity theories through high-energy astrophysical observations.
    
    Ponente: Denise Boncioli (University of L'Aquila and INFN-LNGS)
    
    Boncioli_TeVPA_GammaRaySession_2025.pdf
  - 18:00
    
    First Lorentz Invariance Violation constraint from a cooperation of Imaging Atmospheric Cherenkov Telescopes 15m
    
    Lorentz invariance violation (LIV) is a speculated consequence of some models of quantum gravity. It is modelled as a modified dispersion relation of massless particles. One direct effect of LIV is energy-dependent photon group velocity. This hypothesis is tested by measuring time delays in the arrival of high-energy photons from astrophysical sources. Suitable targets are variable, distant and highly energetic sources, such as pulsars, gamma-ray bursts (GRBs), and flaring active galactic nuclei (AGN). However, a major challenge arises from possible intrinsic energy-time correlation due to source-specific emission processes. To improve the precision of these measurements and distinguish potential LIV-induced delays from intrinsic effects, a collaborative effort has been established among major Imaging Atmospheric Cherenkov Telescopes (IACTs): H.E.S.S., MAGIC, VERITAS, and the first Large-Sized Telescope (LST-1) of CTAO. The Gamma-ray LIV Working Group (γLIV WG) combines observational data from multiple types of sources, enhancing the sensitivity and robustness of LIV searches. We present the first results on the LIV energy scale derived from a combination of real data from IACT experiments.
    
    Ponente: Tomislav Terzić (University of Rijeka, Faculty of Physics)
    
    TeVPA2025_LIVwithIACTs_TTerzic.pdf
  - 18:15
    
    TeV Survey of the LMC with H.E.S.S. 15m
    
    The Large Magellanic Cloud (LMC) is a satellite galaxy, orbiting the Milky Way at a distance of approximately $50 \text{kpc}$. This galactic neighbour contains some of the most luminous TeV gamma-ray sources; namely N$~$157B, the first extra-galactic pulsar wind nebula detected, the supernova remnant N$~$132D, the young massive stellar clusters 30$~$Dor$~$C and R$~$136, and the gamma-ray binary LMC$~$P3. The LMC is the only other galaxy where individual gamma-ray emitting source classes are detected. The High Energy Stereoscopic System (H.E.S.S.) has observed the LMC over the past 20 years with a total observation time of more than 700 hours. These observations were partly conducted in survey mode, so that any point in the LMC is observed with a minimum exposure of 30 hours. A systematic blind search for steady point-like sources has been performed on this data set. In this talk we will present first results of this search.
    
    Ponente: Edwin Mckie (University of the Witwatersrand)
    
    HESS_LMC_Mckie_TeVPA2025.pdf
- 16:45 → 18:30
  Neutrinos: Nonstandard neutrino physics & Primordial neutrinos Room 1.1+1.2 (ADEIT)
  
  Room 1.1+1.2
  
  ADEIT
  
  Moderador: Mauricio Bustamante (Niels Bohr Institute, University of Copenhagen)
  - 16:45
    
    Determination of the High-Energy Neutrino-Nucleon Cross Section with Muon Tracks around the TeV 15m
    
    Over the past decade, high-energy neutrino events have been piling up, resulting in a large statistical dataset covering a broad range of energies and directions. As neutrinos traverse the Earth, they undergo energy- and angle-dependent attenuation, which encodes information about the neutrino–nucleon cross section. In this work, we extract the neutrino–nucleon cross section using a large sample of upward-going muon neutrino events in the 0.5–10 TeV range, detected by IceCube. By analyzing the angular distribution of 305,735 track-like events, we determine the cross section in multiple energy bins. The analysis accounts for systematic uncertainties, including those related to the neutrino flux and the detector.
    
    Ponente: Rasmi Hajjar (CCAPP - Ohio State University)
    
    RHajjar_tevpa_xsection_neutrinos.pdf
  - 17:00
    
    KM3NeT/ARCA sensitivity to neutrino quantum decoherence 15m
    
    In the framework of open quantum systems, neutrino may interact with their surrounding environment, introducing stochastic fluctuations to their quantum phase. This perturbation causes a gradual loss of coherence during neutrino propagation, a phenomenon known as decoherence, which alters the neutrino oscillation probabilities.
    KM3NeT/ARCA is a water Cherenkov detector currently under construction in the Mediterranean Sea. Its design is optimized to detect neutrinos in the TeV to PeV energy range, covering both atmospheric and cosmic neutrino fluxes. This study explores the impact of decoherence effects on the expected neutrino flux composition within the energy range observable by ARCA. Furthermore, the detector’s sensitivity to decoherence effects is evaluated across different models of energy dependence.
    
    Ponente: Nadja Lessing (IFIC, CSIC-UV)
    
    Slides_DecoARCA115_TeVPA_KM3NeT_NLessing.pdf
  - 17:15
    
    An inclusive search for neutrino di-muon events at IceCube 15m
    
    Charm-induced di-muons observed in neutrino experiments have played a pivotal role in advancing our understanding of quantum chromodynamics. IceCube is positioned to observe di-muon events at energies beyond those available to previous neutrino beam experiments, thereby probing novel regions of light quark dynamics within the proton. In this presentation, I will discuss the current status of IceCube’s di-muon searches and outline prospects for future work.
    
    Ponente: Pavel Zhelnin (Harvard University)
    
    TeVPA2025_dimuons.pdf
  - 17:30
    
    Constraints on Neutrino Secret Interactions from High energy neutrinos scattering on CνB 15m
    
    We present new constraints on neutrino secret interactions (νSI) using high-energy and ultra high-energy astrophysical neutrinos as probes of new physics beyond the Standard Model. By studying neutrinos from established sources, such as SN1987A, NGC 1068, TXS 0506+056, PKS 0735+178, and the extreme-energy KM3-230213A event, we explore the potential interactions of Dirac neutrinos with a massive spin-one boson during their propagation through the Cosmic Neutrino Background (CνB). Notably, the KM3-230213A event allows us to probe an entirely new scale of interaction strength and reveals sensitivity to heavier mediator masses previously beyond reach.
    
    Our analysis covers both ultra-relativistic and non-relativistic regimes, deriving exclusion limits on the νSI coupling constant across the full mediator mass range. We examine flavor-universal and flavor-non-universal coupling scenarios, the latter are often addressed in discussions about cosmological tensions such as H₀ and S₈ discrepancies.
    
    Ponente: Mariia Petropavlova (MFF CU, IEAP CVUT)
    
    Petropvlova TeVPa 06.11.2025.pdf
  - 17:45
    
    Signatures of quasi-Dirac neutrinos in the high-energy astrophysical neutrino flux 15m
    
    Although the sources of astrophysical neutrinos are still unknown, they are believed to be produced by a diffuse population of sources in the distant universe. Measurements of the astrophysical flux can thus be sensitive to energy-dependent propagation effects, such as the very long baseline oscillations that would occur if neutrinos are quasi-Dirac. Assuming simple models of the source flux, we find that these oscillations can still be resolved even when integrated over wide distributions in source redshift. We use two sets of IceCube all-sky flux measurements, made with muon and all-flavor neutrino samples, to set constraints on quasi-Dirac mass-splittings between $10^{-19}$ and $10^{-18} \textrm{eV}^2$. To contextualize the significance of our results, we also compute the expected sensitivity of IceCube’s astrophysical flux measurements from multiple realizations. Our results are not significantly impacted by alternative spectral hypotheses or redshift distributions.
    
    Ponente: Kiara Carloni (Harvard University)
    
    TeVPA_2025_v2.pdf
  - 18:00
    
    Primordial High Energy Neutrinos 15m
    
    Among the few ways that allow or could allow us to probe the early Universe from the observation of a flux of primordial particles, there is one possibility which has been little studied: the observation today of high energy neutrinos which could have been emitted short after the Big Bang, from the decay or annihilation of early universe relics.
    We perform a general study of such a possibility. To this end we first emphasize that these neutrinos could display various kind of sharp spectral features, resulting from the primary energy spectrum at emission, and from how this spectrum is smoothed by redshift and radiative correction effects.
    Next we determine the ranges of mass (from a fraction of eV all the way to the Planck scale) and lifetime of the source particles along which we do not/we do expect that the sharp spectral feature will be altered by interactions of the neutrinos on their way to the detector, mainly with the cosmic neutrino background or between themselves.
    We also study the theoretical (i.e.~mainly BBN and CMB) and observational constraints which hold on such a possibility. This allows us to delineate the regions of parameter space (mass, lifetime and abundance) that are already excluded, hopeless for future observation or, instead, which could lead to the observation of such neutrinos in a near future.
    
    Ponente: Nicolas Grimbaum Yamamoto (Université Libre de Bruxelles)
    
    TeVPA 2025 .pdf
  - 18:15
    
    New approach for study of dynamics of neutrinos in the primordial era 15m
    
    Cosmological observations, such as Big Bang Nucleosynthesis (BBN) and the Cosmic Microwave Background (CMB), provide vital insights into the early Universe, allowing us to trace its evolution to times as short as t∼0.01 s and to test extensions of the Standard Model. Accurately modeling the non-trivial dynamics of neutrinos in the decoupling era typically requires solving a system of Boltzmann equations numerically, a method that comes with inherent limitations, particularly in terms of computational efficiency for high neutrino energies. In this talk, a novel approach based on the Direct Simulation Monte Carlo (DSMC) method is presented, which offers significant advantages over traditional techniques, particularly in scenarios involving high-energy neutrino injections.
    
    Ponente: Vsevolod Syvolap (Instituto de Física Teórica, Madrid)
    
    TeVpa_Syvolap.pdf
- 20:30 → 22:30
  
  Conference dinner 2h Ateneo Mercantil
  
  Ateneo Mercantil
viernes, 7 noviembre
- 9:00 → 10:30
  Plenary Session: IX Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Gabrijela Zaharijas (Center for Astrophysics and Cosmology, University of Nova Gorica)
  - 9:00
    
    On the low-power extragalactic gamma-ray sky 30m
    
    This presentation covers aspects - from a theoreticians point of view - of some recent developments on extragalactic low-power gamma-ray sources, with focus on active galactic nuclei.
    
    Ponente: Anita Reimer (University of Innsbruck)
    
    TeVPA2025_AReimer.pdf TeVPA2025_AReimer.pptx
  - 9:30
    
    Collider dark matter searches 30m
    
    The nature of dark matter, one of the most compelling open questions in fundamental physics, is still unknown. A comprehensive search program has developed over the past decades, spanning direct detection experiments, indirect detection via astrophysical signals, and collider-based production. In this talk, we focus on collider searches for dark matter, particularly at the Large Hadron Collider, and discuss how these efforts complement other detection approaches. We will touch upon the theoretical frameworks commonly used to interpret collider results, and highlight recent results and constraints, where initial emphasis on mono-X searches and invisible Higgs decays have over the past years been extended to include long-lived particle searches, light mediators or non-minimal dark sectors. We will conclude with future prospects for collider-based dark matter detection, and how these integrate into a global, multi-pronged strategy to uncover the particle nature of dark matter.
    
    Ponente: Steven Lowette (Vrije Universiteit Brussel)
    
    251107_Lowette_TeVPA25_ColliderDMSearches.pdf
  - 10:00
    
    Multimessenger astrophysics 30m
    
    Multimessenger astrophysics represents a unique opportunity to link particle physics, astronomy, and cosmology. The method for combining different observational probes has been opened up by the opportunity to relate traditional multiwavelength astronomy with the advent of refined and more sensitive neutrino detectors, γ-ray telescopes, gravitational wave interferometers, and space and ground-based cosmic ray apparatus. The talk will discuss the various interconnections among these different probes, highlighting the most relevant results, key ingredients of discoveries, and prospects for the future.
    
    Ponente: Maurizio Spurio (University of Bologna (Italy) and INFN)
    
    TeVPA2025-Spurio.pptx
- 10:30 → 11:00
  
  Coffee Break 30m Dome (Fundación Bancaja)
  
  Dome
  
  Fundación Bancaja
- 11:00 → 12:00
  Plenary Session: X Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Juande Zornoza (IFIC (CSIC-UV))
  - 11:00
    
    New ideas on dark matter searches 30m
    
    In this talk I will review some recent developments in direct detection methods looking for wavelike dark matter including axion dark matter.
    
    Ponente: Christina Gao (Southern University of Science and Technology)
    
    TeVPA25_Gao.pdf
  - 11:30
    
    Cosmic Connections to Particle Physics 30m
    
    In this talk I will survey the complementarity of cosmological and laboratory probes with various developments in elementary particle theory, including dark sector physics and non-standard cosmological histories.
    
    Ponente: Gordan Krnjaic (University of Chicago)
    
    TeVPA2025.pdf
- 12:00 → 12:30
  Concluding Talk Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Moderador: Juande Zornoza (IFIC (CSIC-UV))
  
  Welcome_TeVPa2026_Tendo.pdf
  - 12:00
    
    Conference Summary 30m
    
    Ponente: Dan Hooper (University of Wisconsin-Madison)
    
    Hooper-Valencia-2025.pdf
- 12:30 → 12:40
  
  Concluding Talk: Concluding Words and Announcement of TeVPA 2026 Auditorium (Fundación Bancaja)
  
  Auditorium
  
  Fundación Bancaja
  
  Welcome_TeVPa2026_Tendo.pdf
- 12:40 → 13:30
  
  Lunch box 50m Dome (Fundación Bancaja)
  
  Dome
  
  Fundación Bancaja
- 16:30 → 18:30
  
  Guided City Tour 2h Entrance (ADEIT)
  
  Entrance
  
  ADEIT

TeVPA 2025 - Valencia, Spain

Hall

Fundación Bancaja

Auditorium

Fundación Bancaja

Dome

Fundación Bancaja

Auditorium

Fundación Bancaja

ADEIT

Room 3.1+3.2

ADEIT

Salón de Actos

ADEIT

Salón de Grados

ADEIT

Room 2.1+2.2

ADEIT

Room 1.1+1.2

ADEIT

ADEIT

Room 1.1+1.2

ADEIT

Room 3.1+3.2

ADEIT

Room 2.1+2.2

ADEIT

Salón de Actos

ADEIT

Salón de Grados

ADEIT

ADEIT

Auditorium

Fundación Bancaja

Dome

Fundación Bancaja

Auditorium

Fundación Bancaja

ADEIT

Room 2.1+2.2

ADEIT

Salón de Grados

ADEIT

Room 3.1+3.2

ADEIT

Salón de Actos

ADEIT

Room 1.1+1.2

ADEIT

ADEIT

Room 2.1+2.2

ADEIT

Salón de Grados

ADEIT

Room 3.1+3.2

ADEIT

Salón de Actos

ADEIT

Room 1.1+1.2

ADEIT

Auditorium

Fundación Bancaja

Dome

Fundación Bancaja

Auditorium

Fundación Bancaja

ADEIT

Room 2.1+2.2

ADEIT

Room 3.1+3.2

ADEIT

Salón de Actos

ADEIT

Salón de Grados

ADEIT

Room 1.1+1.2

ADEIT

ADEIT

Room 2.1+2.2

ADEIT