XXI International Workshop on Neutrino Telescopes

Sep 29, 2025, 12:00 PM → Oct 3, 2025, 2:00 PM Europe/Rome

Aula Magna (Palazzo del Bo and Centro Culturale San Gaetano)

Chiara Sirignano (Istituto Nazionale di Fisica Nucleare), Elisa Bernardini (Istituto Nazionale di Fisica Nucleare), Mauro Mezzetto (INFN-PD)

The Neutrino Telescopes Workshop takes place every two years and has a long tradition dating back to 1988.

Discountinuing a 36-year tradition, the XXI edition of the Workshop will be held in Padova, not in Venice.

Among many other attractions, Padova hosts two Unesco World Heritage sites: the Botanical Garden and the fourteenth-century fresco cycles: Padova Urbs Picta.

 

The topics that will be discussed will cover the following topics:

Neutrino Properties
Neutrinos Telescopes and Multi-Messenger
Neutrinos Theory and Cosmology
Data Science and Detector R&D

The Workshop is structured in Plenary and Parallel Sessions and a Poster Session is also scheduled.

Talks in Plenary Sessions are reserved for invited speakers only.

Contributed Talks and Posters will be selected by the Local Organizing Committee. Proposals should be submitted through the "Call for Abstracts".

All talks and posters will be included in the Workshop proceedings which will be published under the Zenodo platform.

The XXI International Workshop on Neutrino Telescopes has received the Support of the National Institute for Nuclear Physics (INFN) and the Patronage of the University of Padova; it is organized by INFN Sezione di Padova and by the Physics and Astronomy Department of Padova University.

		under the patronage

 

Sponsored by

    

        

 

Mon, September 29

Plenary Monday

1 Openings

2 Neutrino Astrophysics

Speaker: Francis Halzen (University of Wisconsin Madison)

3 Global fits of neutrino oscillations

Speaker: Conception Gonzalez-Garcia

4 Review of Neutrinoless Double Beta Decay

Speaker: Maura Pavan (Istituto Nazionale di Fisica Nucleare)

4:00 PM Coffee Break

5 Populations Of Binary Compact Objects: Insights From The Fourth Gravitational-Wave Transient Catalog

Speaker: Michela Mapelli (Padova University and Istituto Nazionale di Fisica Nucleare)

6 The Euclid Experiment

Speaker: Pierluigi Monaco (Istituto Nazionale di Fisica Nucleare)

7 Quantum correlations in neutrino oscillations

Speaker: Massimo Blasone (Istituto Nazionale di Fisica Nucleare)

7:00 PM Refreshment at Caffè Pedrocchi

Tue, September 30

Plenary Tuesday

8 Results from the NOvA experiment

Speaker: Martin Frank

9 Results from the T2K experiment

Speaker: Sophie King

10 Results from the Super-Kamiokande experiment

Speaker: Lucas Nascimento Machado (University of Glasgow)

11 Oscillation results from the IceCube experiment

Speaker: Summer Blot (DESY)

11:00 AM Coffee Break

12 Review of Direct Measurements of Neutrino Masses

Speaker: Loredana Gastaldo (Kirchhoff Institute for Physics, Heidelberg University)

13 Latest results form the DESI experiment (with a focus on neutrino masses)

Speaker: Graziano Rossi (Sejong University)

14 Cosmology fits to neutrino masses

Speaker: Eleonora Di Valentino (University of Sheffield)

1:00 PM Lunch

Neutrino Astrophysics

15 Observation of the ultra-high-energy neutrino event KM3-230213A

The KM3NeT infrastructure comprises two detectors currently under construction in the Mediterranean Sea: KM3NeT/ARCA, designed for the study of high-energy cosmic neutrinos, and KM3NeT/ORCA, optimized for neutrino oscillation studies. The two detectors are already actively taking data and already providing competitive results. Indeed, the highest-energy neutrino ever observed was detected on February 13th 2023 with the KM3NeT/ARCA neutrino telescope. The observed particle was a muon, whose energy at the detector exceeded 100 PeV, likely coming from the interaction of a neutrino of even higher energy. In this contribution, the details of the detection, the data analysis that lead to the determination of the properties of the observed particle, and the studies carried out by the KM3NeT collaboration on its origin are reported.

Speaker: Luigi Antonio Fusco (University of Salerno and INFN)

16 Search for cosmic neutrino sources with two years of KM3NeT/ARCA data

Identifying the astrophysical sources of high-energy neutrinos is essential to understanding the most energetic phenomena in the Universe. While the existence of cosmic neutrinos has been established by the IceCube Neutrino Observatory, their origins remain largely unknown. The KM3NeT/ARCA detector, currently under construction in the Mediterranean Sea, is designed to address this question. With an eventual instrumented volume of one cubic kilometre and exceptional angular resolution (better than 0.1° for muon neutrinos with energies above 300 TeV), KM3NeT offers a unique and complementary view of the sky compared to IceCube, covering a broad energy range. As of now, over 10% of the detector has been deployed. This contribution presents the results of binned searches for neutrino point sources and extended sources from known catalogs, as well as an all-sky scan using KM3NeT/ARCA data collected between May 2021 and September 2023 with an evolving detector configuration of up to 21 detection lines.

Speaker: Rasa Simone Muller (Istituto Nazionale di Fisica Nucleare)

17 The very high energy neutrino (and gamma-ray) flux from the Galactic Plane

We present updated predictions for the very high energy neutrino (and gamma-ray) flux from the Galactic Plane. Our calculations includes the diffuse emission produced by interactions of CR with the interstellar gas and the cumulative flux produced by sources that are too faint to be resolved (either by neutrino or gamma-ray telescopes). The diffuse flux calculation includes the possibility of hardening of the cosmic-ray spectral index in the inner Galaxy, recently suggested by Fermi-LAT observations, and implements the galactic-extragalactic transition for CR at PeV energies. We benchmark our predictions with recent gamma-ray data and compare them with recent results of neutrino telescopes.

Speaker: Francesco Lorenzo Villante (Istituto Nazionale di Fisica Nucleare)

18 Updated IceCube Track-Like Dataset for Point-Source Searches: 2008-2022 Public Release

IceCube has continuously performed all-sky searches for point-like neutrino sources using track-like events. In this talk, we discuss the public data release of neutrino candidates detected by IceCube between April 6, 2008 and May 23, 2022. An updated selection and reconstruction for data taken after June 2010 was implemented. These updates were not implemented in the previous point-source tracks data release. This public data release, which includes 14 years of data and binned detector response functions for muon neutrino signal events, shows improved sensitivity in generic time-integrated point source analyses and supersedes previous releases. Along with the most recently published IceCube time-dependent and time-independent all-sky point-source results with this data, we show reproducibility checks using the open-source, Python-based, SkyLLH software.

19 Neutrino Searches with the Pierre Auger Observatory: From New Techniques to Multi-Messenger Opportunities

The Pierre Auger Observatory, equipped with a vast Surface Detector (SD) array, is well suited to search for ultra-high-energy (UHE) neutrinos above $10^{17}$ eV through the identification of deeply penetrating air showers. The Observatory has set some of the most stringent limits on both diffuse and point-like sources of UHE neutrinos and actively contributes to multi-messenger follow-up searches of transient astrophysical events, such as gamma-ray bursts and binary black hole mergers. The sensitivity to UHE neutrinos is continuously being enhanced through several approaches, including the implementation of two additional SD triggers---Time-over-Threshold-deconvolved (ToTd) and Multiplicity-of-Positive Steps (MoPS)---which have improved detection efficiency below $10^{19}$ eV by a factor of 5-10 in the zenith angle range of $60^\circ$ to $75^\circ$. In this contribution, we provide an overview of ongoing neutrino analyses at the Observatory, highlighting a novel identification strategy that incorporates these triggers within a blind search framework. Updated constraints on diffuse and point-source neutrino fluxes will be presented, alongside a discussion of other recent results.

Speaker: Srijan Sehgal (University of Wuppertal)

4:10 PM Coffee Break

20 Status and results of the KM3NeT/ORCA experiment

KM3NeT/ORCA is a water-Cherenkov neutrino telescope under construction in the Mediterranean Sea, 40 km offshore Toulon in France. Its primary goal is to measure the oscillations of atmospheric neutrinos and determine the neutrino mass ordering. The detector is a three-dimensional array of optical sensors, which detect the Cherenkov radiation induced by charged particles produced in neutrino interactions, enabling the reconstruction of the parent neutrino energy and direction. The detector is already operational and has yielded constraints on the oscillation parameters $\Delta m^2_{31}$ and $\theta_{23}$, together with a competitive measurement of tau neutrino appearance. Several searches for new physics have also been conducted by looking for distortions in the neutrino oscillation pattern.

In addition, cosmic-ray studies have been performed with ORCA by measuring atmospheric muon fluxes. ORCA's multi-disciplinary program includes contributions to indirect dark matter searches and astrophysical neutrino detection. These complementary studies highlight ORCA’s potential as a versatile observatory for astroparticle physics research.

Speaker: Alfonso Lazo Pedrajas (Instituto de Física Corpuscular (IFIC))

21 Status and results of the KM3NeT/ARCA experiment

KM3NeT is a multi-site telescope designed to detect and study cosmic neutrinos and their origin, as well as to improve the knowledge of the intrinsic neutrino properties. Composed of two underwater Cherenkov neutrino telescopes located at two deep-sea sites in the Mediterranean, the KM3NeT infrastructure includes KM3NeT-ARCA (Astrophysics Research with Cosmics in the Abyss), offshore Portopalo di Capo Passero (Sicily, Italy), dedicated to the analysis of high-energy astrophysical neutrinos, from hundreds of GeV up to hundreds of PeV, and KM3NeT-ORCA (Oscillation Research with Cosmics in the Abyss), offshore Toulon (France), designed to investigate neutrino oscillation and mass hierarchy through the detection of atmospheric neutrinos from hundreds of MeV up to the TeV scale.
Despite being in a partial configuration, the KM3NeT- ARCA telescope has already yielded groundbreaking results, including the detection of the first ultra-high-energy astrophysical neutrino, KM3-230213A. This significant observation highlights the remarkable capabilities of deep-sea neutrino telescopes and underscores their potential to uncover novel high-energy astrophysical phenomena. This contribution will review the key results already achieved with KM3NeT-ARCA in the field of neutrino astrophysics, underlining the importance of having the KM3NeT detector in the future multi-messenger panorama.

Speaker: Antonio Marinelli (Dipartimento di Fisica, Università "Federico II")

22 TAMBO: A Deep-Valley Neutrino Observatory

The discovery of point sources of astrophysical neutrinos is a primary aim of neutrino astrophysics. To date, discovering such point sources has proven difficult because of the large atmospheric background neutrino telescopes must contend with. Because of this, only a handful of neutrino sources have been identified over the past 15 years. The development of high-purity detection techniques that minimize atmospheric backgrounds is thus an urgent need in neutrino astronomy.

TAMBO is a next-generation neutrino telescope designed to perform a nearly background-free measurement of the neutrino sky. This high purity is achieved by the fact that TAMBO is sensitive only to $\geq$ 1 PeV $\nu_\tau$, where the atmospheric background flux is significantly smaller than the astrophysical flux. TAMBO will comprise an array of water Cherenkov and plastic scintillator detectors deployed on the face of a deep valley, such as the Colca Canyon in the Peruvian Andes, with its unique geometry facilitating the high-purity measurement of astrophysical tau neutrinos. In this talk, I will present the prospects of TAMBO in the context of next-generation neutrino observatories and provide an overview of the roadmap of TAMBO-100, a pathfinder experiment.

Speaker: Will Thompson (Harvard University)

23 Status of the Trinity PeV Neutrino Observatory

The Trinity Neutrino Observatory aims to cover an energy range from 1 PeV to 1 EeV using imaging atmospheric Cherenkov telescopes (IACTs) located at various sites to detect Earth-skimming neutrinos. The development of Tinity is organized into three phases.
The first phase, which involved the successful operation of the Trinity Demonstrator— a small Cherenkov telescope deployed on Frisco Peak in Utah— is complete. The Demonstrator saw its first light on October 3, 2023, and has since recorded several hundred hours of data. The insights gained from operating the Demonstrator and analyzing its data have informed the design of Trinity One, the next phase towards the full Trinity Observatory.
Trinity One will be the first telescope of the Trinity Observatory, capable of observing neutrino point sources across fifty percent of the sky with unprecedented sensitivity. I will report on the status of the Trinity Observatory, highlighting the lessons learned from the Demonstrator along with the current status and design of Trinity One and its expected performance.

Speaker: Nepomuk Otte (Georgia Institute of Technology)

24 Searches for Gamma-Ray Counterparts of IceCube Neutrino Events in the AGILE Public Data Archive

Elena Gasparri (1), Rosa Poggiani (1), Carlotta Pittori (2,3), Fabrizio Lucarelli (2,3), Paolo Giommi (4)
(1) Department of Physics “E. Fermi”, University of Pisa, Italy
(2) INAF/OAR, Monte Porzio Catone (RM), Italy.
(3) SSDC/ASI, Roma, Italy
(4) Associated to Italian Space Agency, ASI, Roma, Italy

The search for gamma ray counterparts of IceCube neutrino events is a key item for understanding the role of blazars as possible sources of cosmic high energy neutrinos. We have searched the counterparts of IceCube neutrinos events in the AGILE gamma-ray satellite public data archive that occurred in the interval 2018-2020.
We present the candidate counterpart sources in the error regions centered on the detected neutrinos and report their light curves and Spectral Energy Distributions, together with the estimates of the gamma ray flux above 100 MeV for the AGILE detections. The possible associations with blazar systems are discussed.

Speaker: Prof. Rosa Poggiani (University of Pisa)

25 Improving Track Reconstruction with Standard Arrows in IceCube

Reconstructing the incoming direction of muons is a fundamental task in neutrino astronomy. In water- and ice-Cherenkov telescopes, accurate muon reconstruction is important to the entire span of an analysis, from background rejection to accurately determining the position of neutrino point sources. It is therefore crucial to both optimize and understand the performance of muon track reconstruction in neutrino telescopes.

In this talk, we introduce the idea of “standard arrows,” muons with an enhanced pointing precision enabled by their interaction with a small plastic scintillator detector deployed inside of an optical module. Because of their exquisite pointing resolution, we expect standard arrow datasets can have wide applicability in neutrino telescopes, including verifying muon reconstruction algorithms and serving as training sets for machine learning models. Lastly, we will detail R&D efforts on such a scintillator detector to be deployed as part of the IceCube Upgrade, along with its expected performance.

Speaker: Will Thompson (Harvard University)

Neutrino Physics

26 Global Analysis of Neutrino Oscillations and Mass Constraints in the Era of Subpercent Precision

The landscape of neutrino physics is entering a transformative phase, driven by unprecedented experimental precision and expanding data from diverse probes. In this work, we present a comprehensive update of global three-neutrino (3ν) oscillation parameters, reflecting measurements available up to early 2025. Key results include a sub-percent determination of the atmospheric mass splitting |∆m²| and refined constraints on θ13 and θ23. At the same time, the elusive unknowns—mass ordering, CP violation, and θ23 octant—remain open, with only weak statistical preferences. On the non-oscillation front, we update upper bounds on absolute neutrino masses from β-decay, neutrinoless double β-decay, and cosmological observations, noting emerging tensions that hint at either hidden systematics or new physics beyond the standard cosmological model. With JUNO and other next-generation experiments on the horizon, the coming years will test the coherence of the 3ν paradigm at the subpercent level. This evolving precision frontier opens new avenues to probe the fundamental nature of neutrinos and their connections to the broader structure of the universe.

Speaker: Antonio Marrone (Istituto Nazionale di Fisica Nucleare)

27 MicroBooNE's beyond the Standard Model physics program

MicroBooNE is an 85-tonne active mass liquid argon time projection chamber (LArTPC) at Fermilab. Between 2015-2021, the detector recorded neutrino interactions from the Booster Neutrino Beam (BNB) and Neutrinos at the Main Injector (NuMI) beams. MicroBooNE's capabilities for fine-grained tracking, particle identification, and calorimetry make it a powerful detector not just to explore neutrino physics, but also for Beyond the Standard Model (BSM) physics. This talk will discuss MicroBooNE's BSM program, including recently released searches for dark neutrino decay to an e+e- pair, dark trident processes, and heavy neutral leptons. The talk will also discuss the status of other ongoing analyses. Furthermore, we will present efforts to develop tools for BSM analyses that will also be useful for the upcoming Deep Underground Neutrino Experiment (DUNE).

Speaker: MicroBooNE Collaboration

28 Neutrino oscillations with atmospheric neutrinos in JUNO

The Jiangmen Underground Neutrino Observatory (JUNO) is a next-generation neutrino experiment in South China that is currently in the final stages of commissioning. Situated beneath 650 meters of rock overburden ($\sim$1800 meters water equivalent), JUNO’s central detector features a 20-kiloton liquid scintillator target enclosed within a 35.4-meter-diameter acrylic sphere. It achieves a remarkable 78% photocathode coverage through a hybrid array of 17,612 large (20-inch) and 25,600 small (3-inch) photomultiplier tubes. This extensive coverage is essential to meet the experiment’s goal of an unprecedented energy resolution of 3% at 1 MeV.
JUNO’s primary objective is to determine the neutrino mass ordering (NMO) using reactor antineutrinos. However, it also has the potential to probe atmospheric neutrino oscillations through matter effects, offering an independent sensitivity to NMO. When combined, these measurements can enhance JUNO’s overall sensitivity. Notably, JUNO will be the first experiment to explore GeV-scale atmospheric neutrino oscillations using a large, homogeneous liquid scintillator detector. In contrast to conventional water Cherenkov detectors, JUNO’s liquid scintillator requires the development of novel reconstruction techniques to identify neutrino flavors, differentiate between neutrinos and antineutrinos, and reconstruct particle direction and energy in the GeV range.
This talk will be focused on recent advancements toward these goals, including progress in reconstructing the energy and direction of atmospheric neutrinos, identifying neutrino flavor and type, and suppressing background events. Preliminary sensitivity studies will also be discussed.

Speaker: Vanessa Cerrone (University of Padova / INFN Padova)

29 Neutrino and Beyond Standard Model Physics Searches at the CERN ProtoDUNE Detectors

Neutrino beams directed at liquid argon time projection chamber (LArTPC) detectors is a promising means of searching for beyond Standard Model (BSM) physics, such as heavy neutral leptons. The CERN Neutrino Platform hosts two full-scale LArTPC prototypes (the ProtoDUNE detectors) that are proving the technology to be deployed by the Deep Underground Neutrino Experiment (DUNE). Recent studies indicate that these prototypes could also have the potential to detect long-lived BSM particles from one of the targets (T2) in CERN’s north area that is exposed to the 400 GeV SPS beam. In addition, the prototypes are expected to observe a substantial flux of neutrinos from the SPS beam, which would be a source of background in any BSM search. Detecting these neutrinos is therefore a key demonstration of the feasibility of any future BSM program. A sample of high-energy neutrino events may also be of broader use to the DUNE collaboration. For example, by testing the performance of reconstruction algorithms on highly energetic neutrino interactions. This talk will highlight the status of our analysis and prospects for establishing a BSM physics program at the CERN Neutrino Platform.

Speaker: Ciaran Mark Hasnip (CERN)

30 Neutrino mass ordering sensitivity and Precision measurement of oscillation parameters in JUNO

The Jiangmen Underground Neutrino Observatory (JUNO) is a 20-kiloton liquid scintillator detector located $\sim$650 m underground in southern China, now in final commissioning phase. Its central detector, equipped with 17612 20-inch LPMTs and 25600 3-inch SPMTs, achieves total $78\%$ photo-coverage for high energy resolution.

JUNO’s primary goals are to determine the neutrino mass ordering (NMO) and precisely measure the neutrino oscillation parameters $\Delta m^2_{31}$, $\Delta m^2_{21}$, and $\rm{sin}^2\theta_{12}$. The reactor neutrinos, emitted from two nuclear power plants at $\sim$53 km baseline corresponding to solar oscillation maximum, are detected via inverse beta decay (IBD) reaction. The neutrino mass ordering manifests as subtle energy-dependent phase shifts in the energy spectrum, which JUNO resolves via its unprecedented energy resolution ($\leq3\%$ at 1 MeV) and accurate energy scale control (overall non-linearity effects $<1\%$). This capability enables JUNO to achieve $3\sigma$ NMO sensitivity in about 7 years of data-taking. Moreover, the large target mass and great energy resolution enables JUNO to independently measure $\Delta m^2_{31}$, $\Delta m^2_{21}$, and $\rm{sin}^2\theta_{12}$ with sub-percent precision. Such high-precision measurements will play an important role in global analysis of neutrino oscillation, specially, using synergies with accelerator neutrino experiments to boost the NMO sensitivity of JUNO.

This contribution will focus on the latest studies of oscillation physics with reactor neutrinos at JUNO, including the sensitivity of NMO and precise measurement of neutrino parameters.

Speaker: Han Zhang (Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, China)

4:10 PM Coffee Break

31 The CUPID 0νββ experiment

Neutrinoless double-beta decay (0νββ) is a key process in addressing some of the most significant open questions in particle physics, namely the conservation of lepton number and the Majorana nature of the neutrino. Over the past decades, extensive efforts have been dedicated to improving the sensitivity of 0νββ half-life measurements across multiple isotopes. The next generation of experiments aims to probe half-lives greater than 10²⁷ years, reaching the sensitivity required to explore the Inverted-Ordering region of the neutrino mass spectrum. Among the various techniques employed, low-temperature calorimetry has proven exceptionally promising and is expected to maintain a leading role in future searches, particularly through the CUPID experiment. CUPID (CUORE Upgrade with Particle IDentification) will search for the 0νββ decay of ¹⁰⁰Mo, leveraging the existing cryogenic infrastructure and expertise gained from CUORE, the first tonne-scale low-temperature calorimeter array, currently operating at the Laboratori Nazionali del Gran Sasso in Italy. CUPID will utilize scintillating Li₂MoO₄ crystals enriched in ¹⁰⁰Mo, coupled with light detectors featuring Neganov-Trofimov-Luke amplification. With a total isotope mass of 240 kg, CUPID is designed to achieve a background index of 10⁻⁴ counts/keV/kg/year and a FWHM energy resolution of 5 keV. This performance will allow for a 3σ discovery sensitivity of 1.0 × 10²⁷ years after 10 live-years of data-taking, corresponding to an effective Majorana neutrino mass sensitivity in the range of 12–21 meV. In this talk, we will present the current status of the CUPID experiment and outline the upcoming steps toward its construction.

Speaker: Stefano Dell'Oro (Istituto Nazionale di Fisica Nucleare)

32 Latest results from the CUORE experiment

Latest results from the CUORE experiment

CUORE collaboration

The Cryogenic Underground Observatory for Rare Events (CUORE) is the first bolometric experiment searching for 0νββ decay that has successfully reached the one-tonne mass scale. The detector, located at the LNGS in Italy, consists of an array of 988 TeO$_2$ crystals arranged in a compact cylindrical structure of 19 towers. CUORE has been collecting data continuously at ~10 mK since 2017, achieving a 90% uptime and amassing over 2.5 tonne-years of TeO$_2$ exposure. In March 2024 the collaboration released the most recent result of the search for 0νββ, corresponding to two tonne-year TeO$_2$ exposure. This is the largest amount of data ever acquired with a solid state cryogenic detector, which allows for further improvement in the CUORE sensitivity. In this talk, we will present the current status of the CUORE search for 0νββ with the updated statistics of two tonne yr exposure. This statistics also allows for one of the most detailed background reconstructions in the field and enables a precision measurement of the $^{130}$Te 2νββ decay half-life.

Speaker: Elena Ferri (Istituto Nazionale di Fisica Nucleare)

33 LEGEND: 0νββ decay search with germanium detectors

The LEGEND experiment searches for the neutrinoless double-beta (0νββ) decay of Ge-76 using isotopically-enriched high-purity germanium (HPGe) detectors with the ultimate discovery sensitivity beyond a half-life of 10^28 years. The project is conducted in stages. The first one, LEGEND-200, was steadily accumulating physics data at LNGS (Laboratori Nazionali del Gran Sasso, Italy) for more than one year with 140 kg of HPGe detectors. In 2024 the Collaboration unblinded the first data to check the sensitivity of the experiment and study the composition of the LEGEND-200 background, which was slightly higher than predicted based on screening measurements of the components. The detector array was subsequently disassembled to investigate the source of the elevated background, with nearby components undergoing re-cleaning and/or replacement as necessary. LEGEND-200 is scheduled to resume data taking in 2025. In this talk we will present the performance of the ongoing experiment and give an update on the status of its second phase: LEGEND-1000.
This work is supported by the U.S. DOE and the NSF, the LANL, ORNL and LBNL LDRD programs; the European ERC and Horizon programs; the German DFG, BMBF, and MPG; the Italian INFN; the Polish NCN and MNiSW; the Czech MEYS; the Slovak RDA; the Swiss SNF; the UK STFC; the Canadian NSERC and CFI; the LNGS and SURF facilities.

Speaker: Dr Konstantin Gusev (TUM)

34 Status of the SuperNEMO Experiment and physics objectives

The SuperNEMO experiment began physics data-taking in April 2025, becoming the only operational double beta decay detector with full topological event reconstruction, enabled by its unique tracker–calorimeter design. This topology-based approach offers powerful background rejection and is particularly well-suited for probing a broad spectrum of beyond-the-Standard-Model (BSM) scenarios. The detector, located at the Laboratoire Souterrain de Modane (LSM) in France, utilizes $6.11$~kg of enriched $^{82}$Se as its double beta decay source.

We present the physics goals defined by the SuperNEMO collaboration in the context of BSM physics, along with sensitivity estimates to exotic decay modes based on detailed simulations using a newly developed multi-dimensional analysis framework.

Speaker: Maros Petro (IEAP CTU in Prague)

35 Searches for Solar Neutrino in XENONnT experiment

The XENONnT experiment, a 5.9-tonne liquid xenon time projection chamber primarily designed for dark matter searches, recently achieved a significant milestone in neutrino physics with the first direct indication of nuclear recoils from solar $^8$B neutrinos via coherent elastic neutrino-nucleus scattering (CE$\nu$NS). This groundbreaking detection demonstrates XENONnT's unprecedented low-energy detection capabilities and ultra-low background environment, which motivates further solar neutrino searches. This presentation will provide updates on the ongoing search for solar $pp$ neutrinos interacting through neutrino-electron elastic scattering, utilizing data from the first two science runs.

Speaker: Giovanni Volta (Max-Planck-Institut für Kernphysik)

36 Status of the nuGeN experiment at Kalinin NPP.

The $\nu$GeN experiment is aimed at studying rare processes from antineutrino scattering in the close vicinity of the reactor core of the Kalinin Nuclear Power Plant (KNPP) at Udomlya, Russia. The experimental setup is installed under reactor unit #3 of KNPP on the moving platform, which allows changing the distance from the center of the 3.1 GW$_{th}$ core from 11.1 to 12.2 m. In this way, we obtain an enormous antineutrino flux of (3.6-4.4)x10$^{13}$ $\nu$/cm$^2$/s. Materials of the reactor surrounding provide about 50 m w.e. overburden, which serves as a good shielding against cosmic radiation. In combination with a low ambient background, it gives us a unique opportunity to investigate antineutrino properties at the best experimental location in the world. To detect signals from the neutrino scattering, we use a high-purity, low-threshold germanium detector surrounded by passive and active shielding. A specially developed acquisition system allows suppressing events that correspond to noise. The current status of the experimental setup, data taking, and new results will be presented.

Speaker: Alexey Lubashevskiy (Joint Institute for Nuclear Research)

37 Enhancing Low-Energy Neutrino Sensitivity in Super-Kamiokande with the Wide-band Intelligent Trigger

Speaker: Lucas Nascimento Machado (University of Glasgow)

7:00 PM Poster Session Cocktail

Wed, October 1

Neutrino Physics

38 NA61/SHINE experiment for neutrino physics

For atmospheric and long-baseline neutrino oscillation experiments, as well as astro-neutrino-like supernova neutrinos, understanding hadron reactions is essential for neutrino generation. Neutrinos are produced by striking a nucleus such as carbon, nitrogen or oxygen with a primary proton, and then the emitted hadrons, such as pions and kaons, decay in flight providing neutrinos. The hadron interaction is a primary source of the atmospheric and beam neutrino flux prediction uncertainty. Therefore, accurate hadron production and hadron-nucleus interaction measurements are critical. This is one of the objectives of the NA61/SHINE experiment at the Super Proton Synchrotron at CERN. In this presentation, the results of the neutrino program are reviewed. Next, the recent measurements for T2K and Fermilab long-baseline neutrino experiments are presented. Finally, we discuss the prospects for future hadron production measurements including a low-energy beamline that may extend NA61/SHINE’s physics program in the near future. The low-energy hadron production measurements will be beneficial for not only neutrino oscillation experiments but also supernova neutrino observations because atmospheric neutrinos are one of serious backgrounds.

Speaker: Yusuke Koshio (Okayama university)

39 MicroBooNE’s cross-section program for future long-baseline oscillations

Making high-precision measurements of neutrino oscillation parameters requires an unprecedented understanding of neutrino-nucleus scattering. This is especially urgent for upcoming experiments like DUNE and Hyper-K. To help fulfill this need, MicroBooNE has produced an extensive set of neutrino cross-section results that probe both the leptonic and hadronic components of the interaction. This talk will present our recent results in channels that are critical for a variety of oscillation measurements on argon, including DUNE. They include our first measurements of $\nu_{e}$CC interactions on argon with a single charged pion in the final state, which are dominant interaction modes in the energy range for DUNE. These, combined with additional MicroBooNE $\nu_{e}$CC measurements can also help shed more light on the $\nu_{e}$/$\nu_{\mu}$ cross-section ratio which is an important systematic uncertainty for $\nu_{e}$ appearance searches. In addition, we present new results in the quasielastic-like 1mu1p channel which can more directly inform sub-GeV atmospheric neutrino oscillation measurements at DUNE. These results are able to probe the extent to which the interaction model influences the reconstruction of the neutrino direction, given our fixed beam orientation, thus highlighting its sensitivity to various nuclear effects and modeling of final state interactions.

Speaker: London Cooper Troendle

40 Recent cross-section results from MicroBooNE

MicroBooNE is a Liquid Argon Time Projection Chamber, able to image neutrino interactions with excellent spatial and timing resolution, enabling the identification of complex final states resulting from neutrino-nucleus interactions. As a result, MicroBooNE has produced a variety of neutrino cross-section measurements on argon, spanning almost four orders of magnitude and across all major interaction modes - pionless, neutral and charged pion production, neutral current interactions as well as rare final states including strange mesons and baryons such as Λ, η and K. This talk will present MicroBooNE’s recent measurements, including the latest $\nu_{\mu}$CC results without any pions in the final state, measurements of NC and CC pi0 production on argon as well as our first results of kaon production in argon. This talk will showcase our unique sensitivity to probing neutrino interaction models at both the nucleon and nuclear levels.

Speaker: Jairo Rodriguez Rondon

41 Neutron Production in Neutrino-Nucleus Interactions with T2K

T2K is a long-baseline experiment which measures parameters of neutrino oscillations. This can be done by analyzing the interaction of neutrinos close to the point of beam production and 295 km downstream. The detector located near the beam source, called ND280, primarily measures the interactions of neutrinos with carbon nuclei. The particles produced as a result of the interactions deposit energy in ND280 which is used to characterize the incoming neutrino flux and neutrino cross-sections before oscillations occur. Detecting a neutron and analyzing those events is tied to the understanding of final state interactions (FSI) models. Charged-current neutrino quasielastic scattering, the dominant interaction in the energy range of T2K, can produce a neutron only via FSI. Thus, by selecting events with no mesons, but with at least one neutron, and a negative muon, a selection enhanced in FSI events is obtained. Comparing these events to the ones with no identified neutron provides a better understanding of FSI and nuclear effects. However, neutrons are not easy to detect and because of this, they provide uncertainties in identifying the interactions happening in the detector and measuring cross-sections. ND280 has a newly installed Super Fine-Grained Detector (SFGD) made of plastic scintillator cubes. The upgraded detector capable of better position resolution and 3D reconstruction opens up the possibilities of improving the efficiency of neutron detection. Neutrons often leave a cluster, which is basically a few hits in neighbouring cubes, or less likely, a track produced by a proton knocked out by the neutron. With the sub-ns timing resolution achievable in the SFGD, the neutron's kinetic energy can be reconstructed using the measured time-of-flight. The talk will discuss which set of variables have been identified to distinguish true neutron tracks/clusters from background, and on the event level, neutron producing events from events without neutrons.

Speaker: Asit Srivastava (Johannes Gutenberg - Universität Mainz)

42 Latest neutrino cross-section results from T2K

The T2K experiment's primary off-axis near detector, ND280, has the essential role of constraining the main systematic uncertainties that affect neutrino oscillation measurements. Among the leading sources of these uncertainties are neutrino-nucleon interaction cross sections, which must be more precisely understood to fully exploit the potential of current and future long-baseline neutrino experiments. ND280 is a multi-layered magnetised tracking detector with an variety of different target nuclei; it is capable of making precise measurements of cross-section topologies which form the main signal and background channels in T2K's oscillation analysis and is particularly well suited for studying rare interaction channels relevant to the $\nu_\mu \rightarrow \nu_e$​ appearance signal. The cross-section measurements obtained at ND280 directly inform the theoretical models of neutrino interactions, helping to refine our understanding of this field and enabling more accurate determinations of oscillation parameters. This talk will present several novel cross-section results from T2K, including new measurements in muon neutrino charged current interactions with and without pions and world-first measurements of neutral-current single pion production and electron neutrino charged-current pion production on carbon.

Speaker: Dr Anna Holin (RAL-STFC)

10:30 AM Coffee Break

43 Search for coherent elastic neutrino-nucleus scattering with the NUCLEUS Experiment

Coherent Elastic Neutrino-Nucleus Scattering (CEνNS) is a Standard Model process in which a neutrino scatters coherently off an entire nucleus via weak neutral current interactions. First predicted by Freedman in 1973, it remained undetected for over four decades due to the extremely low nuclear recoil energies it produces. In recent years, CEνNS has emerged as a powerful probe for a broad range of physics scenarios, marking a new era in neutrino physics. In this talk, I will present the current status and prospects of the NUCLEUS experiment, which is designed to measure the CEνNS cross-section with high precision and probe the regime of full coherence. The detector employs cryogenic calorimeters based on CaWO₄ and Al₂O₃ crystals, with a total target mass of approximately 10 grams and a nuclear recoil energy threshold as low as 20 eV. The experiment will exploit the intense antineutrino flux from the two reactor cores of the Chooz-B nuclear power plant in France. Following a successful commissioning campaign at the Technical University of Munich (TUM), including the simultaneous operation of different subsystems and a dedicated measurement for background model validation, NUCLEUS is now being relocated to its final experimental site.

Speaker: Mattia Atzori Corona (Istituto Nazionale di Fisica Nucleare)

44 The first neutrino mass measurement of HOLMES experiment

The first neutrino mass measurement of HOLMES experiment

HOLMES collaboration

The determination of the absolute neutrino mass scale remains a fundamental open question in particle physics, with profound implications for both the Standard Model and cosmology. The only model-independent method for measuring the neutrino mass relies on the kinematic analysis of beta decay or electron capture (EC) decay, assuming only momentum and energy conservation. Embedding the radioactive source inside the detector ensures that all the energy is measured except the fraction carried away by the neutrino, minimizing the systematic uncertanties. Such calorimetric approach is chosen by the HOLMES experiment.

The HOLMES experiment investigates the EC decay of $^{163}$Ho using an array of ion-implanted transition-edge sensor (TES) microcalorimeters. These superconducting devices operate in the transition region between resistive and superconducting states at temperatures around 100 mK. Each TES is coupled to an $^{163}$Ho implanted gold absorber. The temperature rise following an interaction is proportional to the deposited energy. The readout system is based on microwave SQUID Multiplexing ($\mu$MUX), enabling the simultaneous monitoring of multiple detectors with minimal cabling.

During the first phase, Holmium was successfully implanted into an array of 48 detectors, with an activity ranging from tens of mBq to 0.6 Bq, with an average value of 0.27 Bq, constituting the first prototype of the final detector system. The total activity was approximately 15 Bq. Two physics runs, each lasting two months, produced a high-statistics calorimetric spectrum of $^{163}$Ho. Data-taking periods ranged from two to five consecutive days, with a duty cycle of 82\% and a discarded event rate below 1\%. HOLMES achieved an average energy resolution of 6 eV FWHM.

We present the most stringent bound on electron neutrino mass obtained with a scalable low
temperature microcalorimeter array by the HOLMES experiment. Over two months, with a total of $7 \times 10^7$ decay events, we set a Bayesian upper bound on the effective electron neutrino mass of $m_{\beta} < 27$ eV/c$^2$ at 90\% CI.

The results on the neutrino mass limit confirm the feasibility of $^{163}$Ho calorimetry for next-generation neutrino mass experiments and highlight the potential of a TES-based approach to push the sensitivity of direct neutrino mass measurements beyond the current state of the art. The scalability of this technique enables larger arrays with enhanced statistics, paving the way for sub-eV sensitivity. During the next phase of the experiment we aim to scale up the detector arrays, optimize the readout, and enhance the implantation efficiency.

Speaker: Elena Ferri (Istituto Nazionale di Fisica Nucleare)

45 Neutrino Physics with PTOLEMY: from the mass measurement to the CNB detection

The cosmic neutrino background is a form of radiation emitted one second after the Big Bang. It is the most abundant source of neutrinos in the Universe; however, due to its extremely low energy, it has never been directly detected. PTOLEMY aims at exploring new experimental techniques to detect the cosmic neutrino background by exploiting neutrino capture on a tritium target. This goal imposes several technological challenges, both in materials science — for the development of a solid tritium target — and in the detection of radio frequencies combined with an innovative electromagnetic spectrometer. Another critical challenge is the measurement of electron energy with extremely high resolution (50 meV), a fundamental requirement that could be achieved by employing micro calorimeters e.g. TES or electrostatic analyzers. Both tecnologies will be tested in the framework of the electron detection system.
PTOLEMY is now entering the construction phase of its demonstrator, which will allow the detector proof of principle, laying the groundwork for the first experimental’s physics goal: the measurement of the neutrino mass. The current status and future developments of the project will be presented.

Speaker: Francesca Maria Pofi (Istituto Nazionale di Fisica Nucleare)

46 First observation of reactor antineutrinos by coherent scattering with CONUS+

The CONUS+ reactor antineutrino experiment investigates coherent elastic neutrino nucleus scattering (CEvNS) on germanium nuclei at nuclear reactors. Due to the relatively high cross section of this interaction, this can be achieved with detectors in the kilogram mass range, whereas a typical neutrino detector using other interactions has a target mass of several tons. In 2023, the CONUS setup was relocated from a reactor in Brokdorf, Germany, to the Leibstadt nuclear power plant in Switzerland. There, the CONUS+ experiment acquires data at a distance of 20.7 m from the reactor core using optimized germanium detectors with very low energy thresholds. The first observation of a CEvNS signal from a nuclear reactor was achieved. In 119 days of reactor operation, (395±106) antineutrinos were measured, compared to a predicted number of (347±59) events.

Speaker: Christian Buck (Max-Planck-Institut fuer Kernphysik Heidelberg)

47 Neutrino studies with FASER

The FASER experiment at the LHC is designed to search for light, weakly-coupled new particles, and to study high-energy neutrinos. The experiment has been running since 2022, and has collected nearly 200/fb of pp collision data. FASER has released several neutrino results including the first observation of electron and muon neutrinos at a particle collider, the first measurement of the muon and electron neutrino interaction cross sections in the TeV energy range, and the first differential measurement with muon neutrinos and anti-neutrinos. This talk will summarise the FASER experiment, the neutrino results, and discuss future prospects for FASER neutrino results.

Speaker: Yuxiao Wang

48 The Scattering and Neutrino Detector at the LHC

SND@LHC is a compact and stand-alone experiment to perform measurements with neutrinos produced at the LHC in a hitherto unexplored pseudo-rapidity region of $7.2 < \eta < 8.4$, complementary to all the other experiments at the LHC. The experiment is located 480 m downstream of IP1 in the unused TI18 tunnel. The detector is composed of a hybrid system based on an 800 kg target mass of tungsten plates, interleaved with emulsion and electronic trackers, followed downstream by a calorimeter and a muon system. The configuration allows efficiently distinguishing between all three neutrino flavours, opening a unique opportunity to probe physics of heavy flavour production at the LHC in the region that is not accessible to ATLAS, CMS and LHCb. This region is of particular interest also for future circular colliders and for predictions of very high-energy atmospheric neutrinos. The detector concept is also well suited to searching for Feebly Interacting Particles via signatures of scattering in the detector target. The first phase aims at operating the detector throughout LHC Run 3 to collect a total of 250 fb$^{−1}$. The presentation will focus on the results of the data taken in 2022-2023 and report the status of the analysis of 2024 data.

Speaker: Fabio Alicante (Istituto Nazionale di Fisica Nucleare)

Neutrino Theory & Cosmology

49 The linear point as cosmic ruler for robust inferences of neutrino masses: tests and applications to the Euclid mission

The large-scale distribution of galaxies retains imprints of acoustic waves that propagated through the primordial baryon-photon plasma. These waves leave a characteristic signature in the galaxy two-point correlation function, known as the Linear Point (LP). The LP is defined as the midpoint between the peak and dip of the correlation function at scales around 150 Mpc, and in recent years, it has emerged as a novel and robust cosmic ruler.

In this talk, I will explain that the Linear Point is a cosmological standard ruler and it crucially enables us to measure cosmic distances without the need to model the impact of non-linearities on the clustering correlation function. The LP maintains its standard ruler properties even in cosmologies with massive neutrinos and thus it is highly relevant for the cosmological inference of the sum of neutrino masses. Recent analyses suggest an unexpected result, that the highest probability region for the sum of the neutrino masses is in the interval m_nu < 0.06 eV. Therefore exploiting complementary observables like the LP is crucial to shed light on such findings.

Finally, I will present ongoing work in the context of the Euclid mission. We are assessing the accuracy and expected precision of LP measurements using mock catalogs (dark matter particles, halos, and galaxies) tailored to Euclid’s specifications. This preparatory analysis is crucial for applying the LP method to upcoming Euclid data, ultimately aiming to constrain cosmological parameters and the sum of neutrino masses with Euclid.

Speaker: Angelo Giuseppe Ferrari (Istituto Nazionale di Fisica Nucleare)

50 Neutrino flavor instabilities: onset and development

At high enough neutrino densities, the phenomenology of flavor conversion may be governed by neutrino-neutrino coherent forward scattering. In contrast to neutral current scattering on charged leptons, this process can be flavor-changing. The coherent nature of the interaction then implies that a large amount of neutrinos can undergo flavor conversion simultaneously. This collective effect is prone to runaway modes, which can change the flavor content of a neutrino ensemble on very short time scales. Capturing these instabilities is crucial in order to accurately model the large-scale dynamics of compact astrophysical objects. In this talk, I will describe the appearance and evolution of collective flavor instabilities in simple models of neutrino-dense media and provide simple recipes to predict the final flavor configuration.

Speaker: Manuel Goimil-García (Niels Bohr Institute, University of Copenhagen).
Contact: manuel.garcia@nbi.ku.dk

Speaker: Manuel Goimil-García (Niels Bohr Institute, University of Copenhagen)

51 From the Gallium Anomaly to Electroweak Couplings: Neutrinos as Probes of the Standard Model

The Standard Model (SM) has long provided a remarkably successful framework for describing fundamental interactions. However, persistent anomalies in the neutrino sector, most notably the long-standing Gallium Anomaly, suggest potential deviations that warrant further investigation. In this talk, I address both the reinterpretation of the neutrino-gallium cross section and precision constraints from neutrino-electron scattering. First, I discuss a revised calculation of the neutrino–gallium charged-current cross section [1], incorporating updated inputs and refined modeling of the transition dynamics. Our results indicate a systematic shift in the predicted interaction rate, with intriguing implications for the calibration of solar neutrino detectors and for the possible existence of sterile neutrinos.

In parallel, I present a global fit of neutrino-electron scattering (νES) data [2] from TEXONO, LAMPF, LSND, BNL-E734, and CHARM-II, complemented by solar neutrino measurements from direct dark matter detection experiments such as LZ, XENONnT, and PandaX. These allow us to extract robust constraints on the vector and axial-vector neutrino-electron neutral current couplings, while explicitly accounting for flavor-dependent effects and momentum-transfer corrections.
The analysis reveals two viable solutions: one in close agreement with the SM prediction, and a degenerate alternative currently favored by the data. I emphasize the crucial role of radiative corrections and energy dependence in reducing theoretical uncertainties. Looking ahead, I show that next-generation dark matter detectors will have the sensitivity needed to resolve these degeneracies and deliver unprecedented tests of electroweak theory in the neutrino sector.

Speaker: Matteo Cadeddu (Istituto Nazionale di Fisica Nucleare)

52 Low-energy windows into the electromagnetic properties of neutrinos

Neutrinos are among the most mysterious particles in the Standard Model, and their possible electromagnetic properties offer a compelling window into physics beyond the standard framework. Features such as a non-zero magnetic moment, a finite charge radius, or a tiny electric charge (millicharge) are not only theoretically intriguing, but also experimentally accessible through precision measurements at low energies.
This talk explores recent progress in probing these properties using two complementary approaches: coherent elastic neutrino-nucleus scattering (CEvNS) and neutrino-electron scattering from various neutrino sources. On the CEvNS side, I will present results from recent reactor- and accelerator-based experiments, including data from the COHERENT collaboration [1] and new measurements at nuclear power facilities using high-purity germanium detectors, such as CONUS+ [2].
In parallel, I will discuss how direct dark matter detection experiments, originally designed for WIMP searches, have become powerful tools for neutrino physics [3,4]. Their sensitivity to solar neutrinos interacting with both atomic electrons and nuclei enables them to set competitive constraints on neutrino electromagnetic couplings. Notably, the complementarity of these approaches provides a unique opportunity to explore possible flavor structures within neutrino electromagnetic scenarios.
Taken together, these diverse experimental results allow us to place stringent, model-independent bounds on neutrino electromagnetic properties and point toward new avenues in the quest for physics beyond the Standard Model.

Speaker: Dr Nicola Cargioli (Istituto Nazionale di Fisica Nucleare-Sezione di Cagliari)

53 When the Fog Lifts: Constraining Light Mediators with CEνNS Signals

The recent observation of Coherent Elastic Neutrino–Nucleus Scattering (CEνNS) from solar $\rm ^8B$ neutrinos by dark matter direct detection experiments marks the first detection 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.

Speaker: Pablo Blanco (IFT UAM/CSIC)

10:30 AM Coffee Break

54 Testing dark sectors with vector mediators using ANTARES and IceCube search data for neutrino lines from dark matter annihilation in the galactic halo

Vector boson mediation between visible and dark sectors is a popular theoretical proposal awaiting experimental test for different model parameter ranges. We take advantage of the enhancement on thermally averaged annihilation cross section $\langle \sigma v \rangle$ in the present day universe as compared to its early universe value from two parameter scenarios, namely the resonance enhancement scenario with $2m_\chi\simeq m_V$ or Sommerfeld enhancement scenario with $m_\chi > m_V$ and $\alpha_\chi \gg v$. Here $m_\chi$ and $m_V$ are masses of dark matter (DM) and vector boson mediator, respectively, while $\alpha_\chi $ is defined as $g_\chi^2/4\pi$ with $g_\chi$ the coupling between DM and vector boson mediator. Using ANTARES and IceCube published upper bounds on $\langle \sigma (\chi\bar{\chi}\to \nu\bar{\nu}) v \rangle$ from their searches for $\chi\bar{\chi}\to \nu\bar{\nu}$ in the galactic halo and the estimated sensitivities of these detectors to $\chi\bar{\chi}\to VV \to \nu\bar{\nu}\nu\bar{\nu}$, we derive (expected) constraints to dark sector parameters. For $m_\chi\gg m_V$, we found that the $m_\chi$ range would be tightly constrained by analyzing the annihilation channel $\chi\bar{\chi}\to VV \to \nu\bar{\nu}\nu\bar{\nu}$.

Speaker: Prof. Guey-Lin Lin (National Yang Ming Chiao Tung University, Taiwan)

55 Quantum Gravity at Neutrino Telescopes: Probing New Frontiers with Neutrinos

Quantum gravitational effects are expected to reveal themselves at extreme energies, cosmological distances, in a break-down of standard quantum mechanics, or in the breaking of global symmetries. Neutrinos offer a unique potential to probe such effects: they are perfect quantum probes, their masses may be related to lepton number or flavor and thus global symmetry breaking and extra-galactic neutrinos have been observed at energies way above the PeV scale. We discuss Lepton Number Violation, Quantum-Gravitational Decoherence, Altered Dispersion Relations, Holographic Scaling  and Entanglement Measures and assess the future perspectives to probe quantum gravity at neutrino telescopes.

Speaker: Heinrich Paes (TU Dortmund University)

Data Science and Detector R&D

56 Dynamic positioning and orientation calibrations of the KM3NeT/ORCA detector

KM3NeT/ORCA is a water Cherenkov neutrino detector currently under construction in the Mediterranean Sea as part of the wider KM3NeT observatory, at a depth of 2450m offshore from Toulon, France. In its current configuration, it consists of 24 detection units out of a planned 115, each with 18 Digital Optical Modules comprising an 18” glass sphere containing 31 3” photomultipler tubes. In order to obtain the desired accuracy for the reconstructed directions of detected neutrino events, both the positions and orientations of each DOM must be known, as these can change due to the movement of the detection units with deep sea currents. The positions are measured using the detection of acoustic signals from known base emitters by piezo-electric receivers, and orientations are recorded with compasses within each DOM. We detail the methods used and show the evolution of these calibrated positions and orientations for KM3NeT/ORCA up to the present day, demonstrating the bootstrapping mechanism used to derive newer configurations from old, and the stability of the deployed detector units through their operation.

Speaker: Rogan Clark (UCLouvain CP3)

57 IceCube PMT efficiency measurement with atmospheric muons

The IceCube neutrino observatory - comprised of a cubic kilometer of ice instrumented with over 5000 photo-multiplier tubes (PMTs) - has achieved world-leading precision measurements of atmospheric neutrino oscillation parameters in recent years. Such measurements inherently perform a simultaneous optical calibration of the detector, constraining relevant systematic uncertainties such as the efficiency of IceCube's PMTs. Independent calibration of this quantity would reinforce future oscillation measurements. In this talk, an in situ PMT efficiency calibration method is presented, with atmospheric muons - detected abundantly in IceCube at several kHz - serving as a “standard candle” light source. A small sample of well-reconstructed, minimum ionizing muon events is procured, and used to measure the PMT efficiency. The current results of this analysis are presented, as well as other potential applications of the aforementioned muon event sample for data-driven validation of event reconstruction algorithms.

Speaker: Daniel Durnford (University of Alberta)

58 The data acquisition system for Phase-2 of the KM3NeT/ARCA neutrino telescope

The KM3NeT observatory hosts two undersea neutrino telescopes, ARCA and ORCA, located at two abyssal sites of the Mediterranean sea. The detectors consist of a 3D array of optical modules, each housing 31 3-inch photomultiplier tubes to detect Cherenkov light emitted by charged particles produced in neutrino interactions in water. Although still under construction, both detectors are already using the same data acquisition model in compliance with the triggerless-streaming readout approach. In this architecture all the data collected by optical modules are transmitted to shore, where online processes running on dedicated resources filter and record relevant data for physics analyses and calibration procedures. To accomplish the target scientific goals, stringent constraints on the precision of the position and timing of the modules are set. In particular the clock distribution must provide a nanosecond synchronisation of the modules which are tens of kilometers away from the on-shore clock references and occupy large volumes that, in the case of ARCA, can reach the cubic kilometer scale. This requirement is met by exploiting the White Rabbit technology.
ORCA telescope and Phase-1 of the ARCA telescope, which accounts for 13% of the total instrumented detector, are based on a custom White Rabbit implementation that deviates significantly from the standard design. Recently the connection layout of the ARCA telescope was significantly revised to accomplish a mandatory optimisation necessary to scale it to the cubic kilometer size. In this new scenario, which is referred to as the Phase 2 of ARCA construction, it was possible to revise also the implementation of the White Rabbit technology, restoring the original standard design.

In this contribution the evolution of the ARCA data acquisition system from Phase 1 to Phase 2 is reviewed, focusing on the revised White Rabbit-based architecture, its role in both data transmission and time synchronization, its implementation with the new detector components that were recently deployed and are operational since the fall of 2024, and the integration of Phase-1 and Phase-2 sectors.

Speaker: Francesco Benfenati Gualandi (Istituto Nazionale di Fisica Nucleare)

59 Physics-driven optimization of the TRIDENT neutrino telescope

Building on the remarkable successes in neutrino astronomy in recent years, TRIDENT is a planned, large-scale neutrino telescope that seeks to advance the frontier of high-energy astrophysical neutrino detection. TRIDENT is to be deployed 3.5 km deep in the “Hai-ling Basin” of the South China Sea, expecting to span approximately 10 km³ of seawater with ~km-long strings equipped with optical modules. Its design targets two primary scientific goals: rapid identification of multiple astrophysical neutrino sources and accurately measuring the flavour composition of the observed neutrino flux. Meeting both of these objectives simultaneously demands a holistic optimization of the detector’s geometry, which impacts angular resolution, detection efficiency of each neutrino flavour, and the accessible energy spectrum. This talk will explore how TRIDENT’s design choices influence its ability to uncover new sources and resolve their flavour signatures. Additionally, developments in enhancing sensitivity core-collapse supernovae will be presented.

Speaker: Iwan Morton-Blake (Tsung-Dao Lee Institute / Shanghai Jiao Tong University)

1:00 PM Lunch

Plenary Wednesday

60 IceCube Results on Astrophysics

Speaker: Angela Zegarelli

61 Galactic cosmic rays, propagation, gamma-rays and neutrinos

Speaker: Andrii Neronov (University of Geneva)

62 The Pacific Ocean Neutrino Experiment: status and first line

Speaker: Matthias Danninger (Simon Fraser University)

63 Results from the Pierre Auger experiment

Speaker: Dr Marcus Niechciol (Center for Particle Physics Siegen, University of Siegen)

4:30 PM Coffee Break

64 Neutrino experiments at the LHC

Speaker: Tomoko Ariga (Kyushu University)

65 Anomalies in neutrino oscillations and physics beyond the Standard Model

Speaker: Antonio Palazzo (Istituto Nazionale di Fisica Nucleare)

66 New results from the Icarus experiment (with an on-line connection with FNAL)

7:30 PM Social Dinner

Thu, October 2

Data Science and Detector R&D

67 Development of early warning method using pre-supernova neutrino light curves

Pre-supernova neutrinos are predominantly produced through thermal processes and nuclear weak interactions in massive stars during the final stages of stellar evolution, with increasing energy and luminosity. The detection of these neutrinos provides an early warning of core-collapse supernovae to neutrino, gravitational wave, and electromagnetic telescopes.
KamLAND, a 1-kiloton liquid scintillator detector, and Super-Kamiokande, a 22.5-kiloton water Cherenkov detector, are both capable of detecting electron antineutrinos through inverse beta decay under low-background conditions, using delayed coincidence technique. Both detectors are sensitive to pre-supernova neutrinos from stars within $\mathcal{O}$(100) parsecs and have already implemented pre-supernova neutrino alarm systems. These alarm systems are based on the significance of statistical excess over the background event rate.
To enable earlier warning, we develop new alarm method incorporating the time evolution of the expected pre-supernova neutrino flux. In this presentation, we report the latest status of this new method, including the alarm significance evaluations based on Monte Carlo simulations assuming KamLAND and Super-Kamiokande.

Speaker: Keita Saito (Tohoku university)

68 The RES-NOVA astroparticle physics observatory

Core-collapse Supernovae (SN) represent critical astronomical events where nearly an entire star's binding energy is emitted as neutrinos. RES-NOVA addresses a significant challenge in astroparticle physics by introducing a novel neutrino detection method using cryogenic detectors constructed from ultra-pure archaeological lead (Pb). The project's key innovation lies in leveraging Coherent Elastic Neutrino-Nucleus Scattering (CEvNS), a detection mechanism with a cross-section approximately 10^4 times larger than traditional detection channels like inverse-beta decay or electron-scattering.
The proposed detector array offers unprecedented sensitivity through its unique design. With a compact volume of just (30 cm)^3, RES-NOVA can survey approximately 90% of potential galactic SNe. The cryogenic detectors utilize Pb with extremely low intrinsic radioactivity, optimized for a low energy threshold and minimal background interference. This approach enables comprehensive measurement of SN neutrino signals while eliminating uncertainties related to neutrino flavor oscillations.
Beyond SN research, the technology presents broad applications in astroparticle physics. The low-energy threshold and advanced background reduction techniques make these detectors promising for multi-messenger astronomy, Dark Matter searches, and fundamental neutrino property studies.
In this contribution, we will present the current experimental efforts focused on the realization of this new technology. Results on the first prototype detectors will be presented, as well as sensitivity projections for the full detector operations. RES-NOVA represents a significant technological advancement, potentially establishing the foundation for a next-generation neutrino and dark matter observatory.

Speaker: Luca Pattavina (Univesity of Milano-Bicocca & INFN)

69 Toward UHE Neutrinos: Calibration and Acoustic Paths in P-ONE and beyond

The Pacific Ocean Neutrino Experiment (P-ONE) is a new large-volume neutrino telescope planned for installation in the Pacific Ocean off the West Coast of Canada. In the ocean, ever-changing conditions necessitate precise calibration systems to continuously monitor the detector. Primarily, ocean currents will sway the one-km-tall mooring lines over time, and detector positioning is crucial for maintaining accurate neutrino pointing performance. The acoustic system of P-ONE will comprise multiple piezo-acoustic receivers in every detector module, combined with autonomous and cabled acoustic seafloor infrastructure. Geometry calibration with this system is performed by monitoring the time-of-flight between acoustic emitters and receivers and then multi-laterating the receiver positions. The P-ONE array of acoustic sensors and the need for acoustic ray-tracing simulations also open the opportunity to search for more exotic acoustic signatures, for example, thermo-acoustic pulses induced by ultra-high-energy (UHE) neutrino interactions. In this talk, I will present the architecture and performance of the P-ONE acoustic system and discuss how one can use acoustics beyond calibration and for the future detection of UHE neutrinos.

Speaker: Felix Henningsen (Simon Fraser University)

70 Controlling data systematics in Euclid spectroscopy with simulations and real observations

Euclid is a mission of the European Space Agency (ESA), designed to investigate the content and evolution of the Universe. Launched in July 2023, the satellite will collect data for at least six years, covering one-third of the sky. Euclid holds the promise to provide crucial new constraints on relevant cosmological parameters, including the sum of the neutrino masses.

Accurate cosmological inference from Euclid data requires careful treatment of observational systematics, which could bias the measured galaxy distribution and distort parameter estimation. Galaxy clustering analyses, in particular, depend on a detailed understanding of the purity and completeness of the cosmological sample. The idea is to assess these properties using two complementary approaches: simulations and deep observations of reference fields. While simulations offer a controlled environment with known inputs, they must be computationally efficient and account for instrumental effects that are not fully understood. Indeed, certain detector non-idealities, such as persistence and snowballs, remain difficult to model accurately, limiting the realism of such simulations. However, deeper observations are confined to small sky regions and present complex selection functions, limiting their representativeness of the data sample.

We first present a fully simulated pipeline to assess the systematic effects, such as spectral overlap, which is one of the main challenges of Euclid's slitless spectroscopic technique. We also present a complementary approach in which we simulate only the spectra; those are then injected into real Euclid images and then processed through the full data pipeline. This method naturally inherits instrumental systematics from real data, offering a more realistic characterisation of purity and completeness. Though computationally intensive, it enables the assessment of systematics over larger sky areas and provides a valuable complementary strategy for robust cosmological analyses and neutrino mass investigations.

Speaker: Francesca Passalacqua (Istituto Nazionale di Fisica Nucleare)

Neutrino Physics

71 Status of the Short-Baseline Near Detector at Fermilab

The Short-Baseline Near Detector (SBND) is one of three liquid argon time projection chamber (LArTPC) neutrino detectors positioned along the axis of the Booster Neutrino Beam (BNB) at Fermilab, and serves as the near detector in the Short-Baseline Neutrino (SBN) Program. The SBND detector completed commissioning and began taking neutrino data in the summer of 2024, and is expected to record about 2 million neutrino interactions per year. Using its superb tracking and calorimetric capabilities, and powerful light collection system, SBND will soon carry out a rich program of neutrino interaction measurements and novel searches for physics beyond the Standard Model (BSM). As the near detector, it will enable the full potential of the SBN sterile neutrino program by precisely characterizing the unoscillated neutrino beam, constraining BNB flux and neutrino-argon cross-section systematic uncertainties. In this talk, the current status and future prospects of SBND are discussed.

Speaker: Miquel Nebot Guinot

72 Investigations of the MiniBooNE anomaly and sterile neutrinos with MicroBooNE

MicroBooNE uses a liquid argon time projection chamber (LArTPC) detector to investigate the observed anomalous low energy excess (LEE) of single electromagnetic shower events reported by the MiniBooNE experiment. After five years of data taking from two accelerator beamlines at Fermilab, MicroBooNE has recently published results testing explanations for the MiniBooNE anomaly, including three single-photon searches spanning multiple underlying processes and topologies, and an electron neutrino search utilizing the full 5-year dataset collected with the Booster Neutrino Beam (BNB). Additionally, we present the status of MicroBooNE's 3+1 sterile neutrino oscillation analysis leveraging both the BNB and Neutrinos at the Main Injector (NuMI) beamlines.

Speaker: Fan Gao

73 Precision neutrino interaction measurements with the nuSCOPE experiment

The poor knowledge of neutrino cross sections at the GeV scale is projected to be responsible for some of the leading sources of uncertainty in next-generation oscillation experiments. Building on the ideas and R&D from ENUBET and NuTAG, we present a proposal for the nuSCOPE experiment (see arXiv:2503.21589). nuSCOPE is a high-precision, short-baseline neutrino experiment at CERN that employs neutrino monitoring and tagging. This allows for an exceptionally well controlled muon and electron neutrino flux, with the extraordinary capacity to reconstruct neutrino energy on an event-by-event basis. The opens up the possibility for a wealth of cross-section measurements usually reserved only for electron-scattering experiments. In this talk we show highlights of projected measurements, demonstrating the experiment's unique ability to directly measure aspects of neutrino interaction physics responsible for dominant sources of systematic uncertainty for the upcoming DUNE and Hyper-K experiments, including neutrino energy response functions and muon/electron neutrino cross-section ratios.

Speakers: Laura Munteanu (CERN), Stephen Dolan (CERN)

74 Solar and supernova neutrinos in DUNE

The Deep Underground Neutrino Experiment (DUNE) will provide a unique opportunity to simultaneously measure the oscillation parameters in the high (GeV) and low (few MeV) energy regimes. DUNE's liquid argon time projection chamber (LArTPC) technology provides a charged-current (CC) and an elastic-scattering (ES) interaction channel that, when simultaneously exploited, enable precision measurements of the $^8$B solar neutrino flux and offer the opportunity to make the first measurement ever of the much smaller hep solar neutrino flux. Additionally, DUNE will be uniquely sensitive to electron-flavour neutrinos from galactic core-collapse supernovae; it will play a key role in complementing water Cherenkov and scintillator detectors, providing a wealth of information about the early stages of core collapse.

This talk will present recent simulations for DUNE's expected sensitivity to supernova and solar neutrinos, and discuss strategies for mitigating the backgrounds of such challenging measurements.

Speaker: Andres Lopez Moreno (LAPP)

10:30 AM Coffee Break

Data Science and Detector R&D

75 Performance of the High-Angle Time Projection Chambers in the Upgraded T2K Off-Axis Near Detector

The off-axis magnetic near detector of the T2K experiment has undergone a significant upgrade, including the construction and installation of two new Time Projection Chambers featuring innovative resistive Micromegas technology and a field cage composed of thin composite walls. This contribution provides a detailed description of the new components of the chambers, including the gas system, gas monitoring chambers, and data acquisition system. Additionally, it reports the results of extensive testing using both neutrino beams and cosmic rays, with comparisons between data and Monte Carlo simulations. The new detectors achieve improved spatial resolution and enhanced particle identification capabilities which are crucial for the precision goals of the T2K experiment.

Speaker: Matteo Feltre (Istituto Nazionale di Fisica Nucleare)

76 Super Fine-Grained Detector for improved neutrino interaction measurements in T2K

The Tokai-to-Kamioka (T2K) experiment is a long-baseline neutrino experiment. T2K obtained results that exclude the CP conservation with a 90% confidence level so far. Toward more precise measurements of the oscillation parameters, T2K experiment recently started operation of upgraded near detectors to further reduce major systematic errors on the neutrino-nucleus interaction. An upstream part of the near detector complex, ND280, was replaced with three detectors: the Super Fine-Grained Detector (SuperFGD), two High-Angle TPCs (HATs), and Time of Flight detectors (ToFs). SuperFGD is a novel target tracker which consists of about two million plastic scintillator cubes packed in about 2 m $\times$ 2 m $\times$ 0.6 m dimension. Scintillation light from the cube is read out by about 56 thousand channels from three directions through wavelength-shifting fibers and photo sensors. It provides 3D track reconstruction, 4 phi angular acceptance, calorimetry, and detection capability of neutrons and low energy protons. We report detector design, construction, operation status and its performances from the physics run with a full detector starting since June 2024.

Speaker: Tsunayuki Matsubara

77 First results from T2K's upgraded near detector

T2K is a long-baseline experiment measuring neutrino and antineutrino oscillations by observing the disappearance of muon neutrinos, as well as the appearance of electron neutrinos, over a long 295km distance. The ND280 near detector at J-PARC plays a crucial role to minimise the systematic uncertainties related to the neutrino flux and neutrino-nucleus cross-sections as it measures the neutrino beam at a ND site before it oscillates. The ND280 detector has recently been upgraded with a new suite of sub-detectors: a high granularity SuperFGD with 2 million optically-isolated scintillating cubes read out by wavelength shifting fibres and 55000 Multi-Pixel Photon Counters; two horizontal Time-Projection Chambers instrumented with resistive Micromegas, and additionally six panels of scintillating bars for precise time-of-flight measurements. These new detectors permit analyses with lower tracking thresholds, 4pi angular acceptance and the measurement of kinematics of neutrons produced in neutrino interactions. In this talk, new data using the upgraded ND280 detector configuration will be discussed, highlighting significant performance improvements.

Speaker: Dr Anna Holin (RAL-STFC)

78 Background Components of the JUNO Liquid Scintillator

The Jiangmen Underground Neutrino Observatory (JUNO) is a 20-kton liquid scintillator detector housed in a laboratory approximately 650 meters underground. Its primary scientific goal is to determine the neutrino mass ordering by studying the oscillated anti-neutrino flux emitted from two nuclear power plants located 53 kilometers away. Given the extremely low expected signal rate, only 60 anti-neutrino interaction counts per day, precise control of radioactive background sources is critical. JUNO also serves as an excellent facility for solar neutrino measurements, which demands even stricter radioactivity control.
This contribution systematically discusses the anticipated background components in JUNO’s liquid scintillator, and their impact on scientific goal.

Speaker: Guanda Gong (Institute of High Energy Physics, Chinese Academy of Sciences)

79 The KM3NeT Digital Optical Module: a multi-PMT approach

The KM3NeT Collaboration is deploying an advanced deep-sea neutrino detector in the Mediterranean Sea, aiming to explore neutrinos across a broad energy spectrum. This is achieved through two detectors, ARCA and ORCA, that share the same Cherenkov detection principle, but differ in their geometrical layout to address distinct physics goals. A central component of KM3NeT is its novel Digital Optical Module (DOM), which features 31 three-inch photomultiplier tubes within a single pressure-resistant glass sphere. This multi-PMT configuration marks a significant advancement over traditional single-PMT designs, offering a larger effective photocathode area and enabling superior timing accuracy,
directional resolution, and calibration capabilities. To meet the demands of large-scale deployment (6210 DOMs are foreseen in total for the full-size detectors), the DOMs are assembled simultaneously at eight different integration sites using a rigorously standardized process. This talk will give an overview of the KM3NeT optical module technology and the integration strategy adopted to support large-scale deployment.

Speaker: Dr Immacolata Carmen Rea (Istituto Nazionale di Fisica Nucleare)

80 The Calibration Of The Most Precise LArTPC Detector Ever To Be Built – DUNE

The Deep Underground Neutrino Experiment, DUNE, is a next-generation, long-baseline, neutrino experiment and flagship project of the U.S. It is poised to perform some of the most precise measurements of the properties of neutrinos to elucidate their role in the outstanding matter-antimatter asymmetry. DUNE will make use of the most intense neutrino beam, produced at the Fermi National Accelerator Laboratory, and which is directed at its Far Detector (FD) located 800 miles away and a mile underground at the Sanford Underground Research facility in Lead, South Dakota.
At a nominal 70 kilotons of liquid argon in four identical modules, the DUNE far detector will be the largest Liquid Argon Time Projection Chamber (LArTPC)-based neutrino observatory in the world. The level of precision required to answer the questions sought after by DUNE results in unprecedented requirements in our understanding of the detector response. We must, therefore, carefully address various systematic uncertainties, particularly those in position and energy reconstruction of neutrino interactions and their byproducts. I will talk about the challenges involved in calibrating the largest LArTPC ever to be built and elaborate on the novel calibration systems, tailored for DUNE, to provide the precision required to achieve future breakthrough discoveries.

Speaker: David Rivera

Neutrino Astrophysics

81 Galactic and extra-galactic core-collapse supernova neutrino flux detection in the LEGEND muon veto

The LEGEND Collaboration advances an experimental program to search for the neutrinoless double-beta decay of $^{76}$Ge.
It has recently released the first results on the decay search based on 61 kg yr of data collected by the first stage of the experiment, LEGEND-200. It operates high-purity germanium (HPGe) detectors enriched in $^{76}$Ge immersed in a cryostat filled with pure liquid argon. The cryostat is deployed in a tank filled with 590 m$^3$ of purified
water, instrumented with photomultiplier tubes to tag cosmic-ray induced muon events, and to passively shield the detectors against environmental radioactivity.
The second stage of the experiment, LEGEND-1000, aims to operate up to one ton of HPGe detectors enriched in $^{76}$Ge with different proposals to optimize the water tank features.
In this presentation, we explore the detection capabilities and sensitivity of the LEGEND muon veto in both phases of the experiment to the neutrino flux from core-collapse supernovae. The ability to identify the time of black hole formation is also discussed.

This work is supported by the U.S. DOE, and the NSF, the LANL, ORNL and LBNL LDRD programs; the European ERC and Horizon programs; the German DFG, BMBF, and MPG; the Italian INFN; the Polish NCN and MNiSW; the Czech MEYS; the Slovak RDA; the Swiss SNF; the UK STFC; the Canadian NSERC and CFI; the LNGS and SURF facilities.

Speaker: Valentina Biancacci (GSSI, INFN)

82 Hunting neutrinos from hybrid stars

Hybrid stars, also know as Thorne-Zytkow Objects (TZOs), have been predicted to form when a neutron star is engulfed by by another star, likely a red giant or super-giant. Then, accretion onto a neutron star can lead to a significant emission of neutrinos of all flavours with energies of 1–100 MeV. Since the neutrino signal is expected to largely vary in time (from milliseconds to thousands of years), we propose detection strategies tailored to the signal duration. We find that neutrino detection from TZOs up to the Small Magellanic Cloud is within the reach of current- and next-generation neutrino telescopes. Neutrino searches complement the ongoing observational efforts across the electromagnetic spectrum and gravitational wave detection prospects and would be of pivotal importance to probe this population of exotic stellar objects.

Speaker: Pablo Martínez-Miravé (Niels Bohr Institute, University of Copenhagen)

83 Search for Ultra-High-Energy Neutrinos from Gamma-Ray Bursts with the Pierre Auger Observatory

The Pierre Auger Observatory has excellent sensitivity to ultra-high-energy (UHE) neutrinos. The Surface Detector array is used to search for highly inclined neutrino-induced air showers, which, though not observed yet, have clear characteristic signatures. Due to the null observation of UHE neutrinos, we obtain upper luminosity limits on individual gamma-ray bursts from the public catalog GRBweb, that are in the field of view of the Observatory for neutrino searches. As the predicted neutrino luminosity from these sources strongly depends on the modeled emission mechanisms and dissipative processes, we obtain the limits using different neutrino spectra corresponding to distinct scenarios such as the one-zone fireball model. The spectra are calculated using the source code "Cosmic Ray Stochastic Interactions for Propagation" (CRISP), to compute quantities related to the propagation of heavier primaries within the source environment.

Speaker: Therese Paulsen (Bergische Universität Wuppertal)

84 Prospects of neutrino observations of the Central Molecular Zone and Cygnus Cocoon

In this contribution we obtained the neutrino expectations of KM3NeT/ARCA for the Central Molecular Zone (CMZ) and the Cygnus Cocoon. The CMZ extends for a few hundred parsecs around the Galactic center, containing the massive molecular clouds Sgr A, Sgr B, and Sgr C which can act as targets for the high energy cosmic rays. The Cygnus Cocoon is a massive star-forming region of a few hundred parsecs in the Galactic plane. It contains regions with high gas densities and a young stellar population. The high energy emission from these regions is expected to be dominated by the interactions of cosmic-rays with the molecular gas, which translate into gamma-ray and neutrinos production. Here we present a search for neutrino emission from these two regions. We explored the sensitivities of the current KM3NeT/ARCA geometry as well as the case of the complete future detector.

Speaker: Dr Marouane Benhassi (Istituto Nazionale di Fisica Nucleare)

85 Probing Dark Matter–Neutrino Interactions through High Energy Neutrino Observations from AGN

Dark Matter (DM) accounts for a substantial fraction of the universe’s mass-energy content, yet its particle nature remains one of the most profound open questions in physics. Neutrinos, with their extremely weak interactions and cosmic reach, offer a unique probe of new physics scenarios involving DM. One intriguing possibility arises in the vicinity of supermassive black holes, where gravitationally induced dark matter overdensities, in other words,''DM spikes", may significantly alter the propagation of high-energy neutrinos emitted by active galactic nuclei (AGN). In particular, neutrino-DM scattering in such dense environments can lead to observable attenuation features in the neutrino flux.

Recent detections of high energy neutrinos from point-like extragalactic sources, most notably the blazar TXS 0506+056 and the radio-loud Seyfert galaxy NGC 1068, by the IceCube Neutrino Observatory present an unprecedented opportunity to search for such effects. In this study, we leverage publicly available IceCube data to jointly analyze these sources and place constraints on the neutrino–DM scattering cross-section. By combining multiple AGN neutrino observations, we enhance our sensitivity to potential deviations from standard astrophysical expectations, offering constraints on dark matter interactions at energy scales far beyond those accessible by terrestrial experiments.

Speakers: Khushboo Dixit (Centre for Astro-Particle Physics, University of Johannesburg), Soebur Razzaque (University of Johannesburg Centre for Astro-Particle Physics)

86 Status of Realtime Neutrino Alerts in IceCube

Neutrino astronomy benefits from multimessenger collaboration, particularly in the search for time-variable astrophysical sources. Identifying statistically significant astrophysical neutrino flares amid a sea of atmospheric muon and neutrino background remains challenging. In the case of a true neutrino flare, coincident detections of electromagnetic activity can strengthen the case for an astrophysical origin. The IceCube neutrino observatory nearly continuously monitors the full sky making it well suited to provide targets of opportunity for follow-up by pointed instruments. Given this, IceCube has implemented a realtime program that provides neutrino alerts to the multimessenger community. These alerts fall into three major categories: single high-energy event alerts, multiple-event (or cluster) alerts, and rapid follow-up analyses of interesting transient phenomena. A major milestone of this program was the observation of a multiwavelength flare from the blazar TXS 0506+056, triggered by an IceCube alert from a single, high-energy neutrino event. In this presentation, we will provide an overview of the realtime program and highlight recent efforts to update IceCube’s cluster alerts.

Speaker: Sarah Louise Mancina (Università degli Studi di Padova)

1:00 PM Lunch

Plenary Thursday

87 The Hyper-Kamiokande experiment

Speaker: Sammy Valder (STFC UKRI, UK)

88 The DUNE Experiment

89 The JUNO Experiment

Speaker: Monica Sisti (Istituto Nazionale di Fisica Nucleare)

90 KM3NeT-ORCA

4:30 PM Coffee Break

91 Neutrino Physics at a Muon Collider

Speaker: Andrea Wulzer (ICREA & IFAE)

92 Tagged Neutrino Beams

Speaker: Mathieu Perrin-Terrin (Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France)

93 Experimental strategies to measure GeV Neutrino Cross Sections

Speaker: Julia Tena Vidal

8:00 PM Visit to Cappella degli Scrovegni

Fri, October 3

Plenary Friday

94 Neutrino Telescopes in China

Speaker: Donglian Xu

95 KM3NeT-ARCA

Speaker: Antonio Marinelli (Istituto Nazionale di Fisica Nucleare)

96 Radio detection of astrophysical neutrinos

Speaker: Joerg Hoerandel (Radboud University Nijmegen)

10:30 AM Coffee Break

97 Low-scale leptogenesis with Dirac phase CP-violation

Speaker: Alessandro Granelli (Istituto Nazionale di Fisica Nucleare)

98 Oscillation physics with a million neutrino atmospheric events

Speaker: Ivan Martinez Soler (Durham U. and IPPP)

99 Nuclear Astrophysics

Speaker: Federico Ferraro (Istituto Nazionale di Fisica Nucleare)

100 Vision Talk

Speaker: Hitoshi Murayama (UC Berkeley, LBNL, Kavli IPMU Tokyo)