Welcome Adress

• Masaya Ishino (The University of Tokyo)
• Michel Gonin (IN2P3 & The University of Tokyo - ILANCE)

Room: Koshiba Hall

Questions in Cosmology for the Decades Ahead

• Jia Liu (Kavli IPMU)

Room: Koshiba Hall Cosmology is entering a new era of powerful surveys across many wavelengths. I will highlight some of the key challenges for the decades ahead: how to resolve current tensions in our data, how to combine information across different probes through cross-correlation, and how to make the best use of modern tools like machine learning. Together, these advances can open new windows on the Universe and shape the next generation of cosmological discovery.

The Simons Observatory: Status and Early Data

• Erik Rosenberg (University of Manchester)

Room: Koshiba Hall The Simons Observatory (SO) is a cosmic microwave background survey experiment located in the Atacama Desert in Chile. SO consists of multiple small-aperture telescopes (SATs) carrying out a focused small-area survey, as well as a large-aperture telescope (LAT) conducting a wide-field, high-resolution survey. The SATs are searching specifically for primordial B-mode polarization sourced by tensor perturbations in the early Universe. LAT science goals include constraining primordial non-Gaussianity and the effective number of relativistic species in the early Universe; measuring the integrated mass, electron pressure and electron momentum distributions in the late-time Universe; constraining neutrino mass and the growth of cosmic structure; producing a galaxy cluster catalogue and measuring the environments around clusters; and other transient, Galactic, and Solar System science goals. The SO mid-frequency SATs saw first light in late 2023, as did the LAT in early 2025; both have since been conducting commissioning and initial science observations. I will present the current status and early results from both surveys.

Astrophysical and cosmological neutrinos: A window to new physics

• Cristina VOLPE (APC)

Room: Koshiba Hall Nature has provided us with powerful neutrino sources, with explosive or violent events, such as core-collapse supernovae that mark the end of the life of massive stars, or binary compact object mergers, like binary neutron star mergers. Neutrinos are intriguing elementary particles with mixings, that weakly interact with matter, which makes them unique messengers of events far in space and time. While neutrinos have already played a remarkable role historically in shaping, since the premises of neutrino astronomy, fundamental knowledge, they keep having a unique role in astrophysical and cosmological environments. In this talk, I will highlight the impact neutrinos have on longstanding open issues such as on the core-collapse supernova explosion mechanism, or on nucleosynthesis processes e.g. the r-process, in relation with supernovae and binary neutron-star merger remnants. I will mention the fact that understanding how neutrinos change flavor in such dense environments is still an open problem. I will discuss the crucial role of future observations, also for the search for new physics. Interestingly, neutrinos from supernovae and binary neutron-star mergers have many similarities with neutrinos in the early Universe, in particular at the MeV epoch. Finally, I will emphasize the importance of discovering the diffuse supernova background from past supernova explosions, which will open a new window in low energy neutrino astrophysics and will constitute a unique laboratory for astrophysics, neutrino physics and the search for new physics. As for the cosmological neutrino background, its observation remains extremely challenging.

Status and prospects of JUNO

• Luca Pelicci (Università degli Studi di Milano and INFN Milano)

Room: Koshiba Hall The Jiangmen Underground Neutrino Observatory (JUNO) is a 20-kiloton multipurpose liquid scintillator detector located in Guangdong province, China, designed to address key open questions in neutrino physics. After completing construction in 2024, JUNO entered a commissioning phase with water filling, followed by a six-month liquid scintillator filling campaign. Full data-taking is expected to begin around September 2025. The detector is situated at an optimized baseline of about 52.5 km from both the Yangjiang and Taishan Nuclear Power Plants, which together provide a high flux of reactor antineutrinos. This location maximizes sensitivity to JUNO’s primary goal: determining the neutrino mass ordering (NMO). By precisely measuring oscillation-induced modulations in the energy spectrum, JUNO aims to determine the NMO with a significance of about 3σ in roughly seven years. Its large target mass, low background, and unprecedented 3% energy resolution at 1 MeV will also enable sub-percent precision measurements of the oscillation parameters Δm^{2}_{21}, sin^{2}(2θ){12}, and Δm^{2}_{31} simultaneously. Beyond reactor antineutrino measurement, JUNO has a broad physics program, including the detection of neutrinos from natural sources such as the Sun, the Earth, the atmosphere, and potential galactic core-collapse supernovae. This talk will present an overview of JUNO’s design and detection principles, highlight its primary and complementary scientific goals, and discuss its prospects for its contributions to neutrino physics in the coming decade.

The Next Frontiers in Particle Physics: from the LHC to the FCC

• Marumi Kado (CERN)

Room: Koshiba Hall With the third update of the European Strategy for Particle Physics soon reaching its conclusion, CERN and the field of high energy physics are at a pivotal and high-stakes moment. The third run of the LHC superb operations will also soon come to an end and yield to the installation of the upgrades of the machine and the experiments during a long shutdown period. With these data, the LHC project has far exceeded its initial expectations, both in terms of data collected and physics results. In this talk, I will discuss the prospects for the High-Luminosity upgrade of the LHC and the FCC projects in the light of the outstanding achievements of the LHC

ATLAS results on Higgs Physics and Electroweak Symmetry Breaking

• Gustaaf Brooijmans (Columbia University)

Room: Koshiba Hall This talk will review recent ATLAS results on Higgs Physics and Electroweak Symmetry Breaking

Cosmology and Hubble tension from Gravitational-Wave Observations

• Atsushi Nishizawa (Hiroshima University)

Room: Koshiba Hall A persistent tension exists between the Hubble constant values inferred from early-Universe observations—such as the cosmic microwave background and baryon acoustic oscillations—and those obtained from local distance-ladder measurements. Gravitational waves (GWs) from compact binary coalescences provide a direct measurement of the luminosity distance from the waveform, offering an independent probe of the cosmic expansion, known as "standard sirens." For neutron-star binaries, source redshifts can be determined through electromagnetic follow-up observations of counterparts detected in coincidence with GW events. In contrast, stellar-mass binary black holes lack electromagnetic counterparts, requiring alternative approaches to obtain redshift information. For ground-based detectors, two such approaches are currently in use: the dark siren and spectral siren methods. In this talk, I will briefly review the methods used for the current GW observation and present recent results from the first part of the fourth LIGO–Virgo–KAGRA observing run. I will also discuss future prospects for cosmological measurements using GW observations.

New Perspectives onto the Universe in the Era of Multi-Messenger Astrophysics

• Samaya Nissanke (DESY)

Room: Koshiba Hall Since the revolutionary discovery of gravitational wave (GW) emission from a binary black hole merger in 2015, the remarkable GW detectors LIGO, Virgo and KAGRA have detected at least 220 compact object mergers. These events are transforming modern astronomy. In particular, the first binary neutron star merger, dubbed GW170817, was observed in both gravitational and electromagnetic radiation, thus opening up a new era in multi-messenger astrophysics. The multi-messenger characterisation of such an event has enabled major advances into diverse fields of modern physics from gravity, high-energy astrophysics, nuclear physics, to cosmology. In this talk, I will discuss our work in strong-field gravity astrophysics and how combining observations, theory and experiment have been key in making progress in this field. I will present the challenges and the opportunities that have emerged in multi-messenger astrophysics, particularly in the past 8 years, and what the future holds in this new era

Status of the Hyper-Kamiokande experiment

• Lorenzo Périssé (ILANCE - IN2P3 & UTokyo)

Room: Koshiba Hall The Hyper-Kamiokande (Hyper-K) is a next generation long baseline neutrino experiment. The Hyper-K water Cherenkov far detector is designed to succeed the Super-Kamiokande (SK) detector. Currently under construction in Japan, the construction and commissioning of the experiment is expected to be finalized by the end of 2027, with data-taking starting in 2028. Compared to its predecessors, the Hyper-K far detector extended capabilities will amount to a fiducial volume nearly one order of magnitude higher (260 kton total, 190 kton fiducial). It will be instrumented with 20000 high-efficiency 50 cm photodetectors, 1000 multi-photodetectors, electronics and DAQ, that associated with new calibration and monitoring approach, with deliver a broader spectrum of measurement possibilities and higher level of data quality when compared to existing data. Combined with a MegaWatt-class beamline located at the J-PARC accelerator facility and a complex of near and intermediate detectors, the experiment will collect unprecedented number of neutrino interactions for a very broad physics program that includes: the discovery of CP-violation in the lepton sector; precise measurements of neutrino flavor oscillation parameters; testing of Grand Unified Theories with proton decay search; probing for new physic scenarios in the upturn region of solar neutrinos; constraining supernova mechanisms and cosmic star-formation history by observing neutrinos from both individual and diffuse supernova sources (DSNB). The advancement status of Hyper-K far and near detectors including the Intermediate Water Cherenkov Detector (IWCD) will be reported in this presentation, along with its physics goals.

KM3NeT: from deep-sea technology to high-energy neutrino discoveries

• Simone Biagi (INFN - LNS)

Room: Koshiba Hall KM3NeT is a cutting-edge neutrino observatory under construction in the Mediterranean Sea, aimed at exploring fundamental questions in neutrino physics and high-energy astrophysics. The project features two deep-sea Cherenkov detectors: ARCA, located off the coast of Sicily and optimized for detecting cosmic neutrinos in the TeV–PeV range, and ORCA, situated near the French coast, which focuses on precise measurements of atmospheric neutrinos and oscillation parameters in the GeV energy range. Although still under construction, both detectors are already operational and producing competitive scientific results. A landmark achievement is the recent detection by KM3NeT/ARCA of an ultra-high energy neutrino event, referred to as KM3-230213A, with a reconstructed energy of 220 PeV. This observation, representing the highest-energy neutrino ever recorded, marks a significant milestone for the experiment, opening new avenues for studying extreme astrophysical environments and the origin of cosmic neutrinos. In addition to its core scientific program, KM3NeT actively participates in the realm of multi-messenger astronomy, contributing real-time neutrino alerts to global networks and enabling prompt follow-up observations in electromagnetic and gravitational waves. This presentation will provide an update on the status of the KM3NeT infrastructure and its deployment, highlight the latest scientific findings — particularly the implications of the recent high-energy neutrino detection — and outline the potential for future discoveries with the full-scale detector arrays.

From Particles to the Cosmos at Colliders

• Yves Sirois (Laboratoire Leprince-Ringuet, Ecole Polytechnique, Palaiseau)

Room: Koshiba Hall The discovery of the Higgs boson by the ATLAS and CMS experiments at CERN in 2012 revolutionised our understanding of the origin of matter and interactions in the universe. The proof of the existence of a scalar field supports the hypothesis of a spontaneous electroweak symmetry breaking mechanism responsible for the appearance of the mass of the Z0 and W± vector bosons in the very early moments. The discovery by ATLAS and CMS in 2015 of the existence of Yukawa couplings between elementary fermions and the Higgs field highlighted the importance of the “substance” of the vacuum for the story of our universe. Old questions are being exacerbated and new questions are emerging that could offer opportunities for discoveries at large colliders, in conjunction with cosmological observations, in the coming decades.

CMS Results on Beyond the Standard Model Physics

• Ketino Kaadze (Kansas State University)

Room: Koshiba Hall Search for new physics Beyond Standard Model (BSM) is one of the major goals of the CMS physics program at the LHC. A variety of searches beyond SM signatures, including exotic models, BSM particles decaying to top quarks, Higgs bosons, gauge bosons, will be presented.

Hunting gravitational waves with Virgo: status, results and future prospects.

• Matteo Di Giovanni (Scuola Normale Superiore)

Room: Koshiba Hall Since the first gravitational-wave (GW) detection in 2015, GW astronomy has undergone a remarkable expansion, culminating in 90 events observed during the first three observing runs of the Advanced LIGO and Virgo detectors and more than 200 public alerts from the still ongoing fourth observing run. In these discoveries, Virgo played an important role, providing crucial contributions to source localization and parameter estimation. In this talk, I will present an up-to-date overview of the Virgo interferometer, emphasizing its impact within the global network of ground-based detectors. I will also explore the range of ongoing searches, showcasing notable recent results, and conclude with a perspective on forthcoming upgrades.

Recent Results in Very High Energy Gamma-Ray Astronomy

• Armand Fiasson (LAPP - Annecy)

Room: Koshiba Hall In this contribution, I will review recent developments in very high energy (VHE; 30 GeV–100 TeV) gamma-ray astronomy. I will highlight key observational results obtained with the current generation of imaging atmospheric Cherenkov telescopes such as H.E.S.S., MAGIC, and VERITAS. The talk will focus on new insights gained from observations of a wide variety of astrophysical sources, both Galactic and extragalactic, and will discuss how these findings advance our understanding of non-thermal processes in the Universe. I will give also an outlook on first results obtained by upcoming instruments of the Cherenkov Telescope Array Observatory (CTAO).

JWST Constraints on Early Galaxy and Black Hole Formation

• Hakim Atek (Institut d'astrophysique de Paris)

Room: Koshiba Hall The field of galaxy formation and evolution is undergoing a transformative renaissance, driven by groundbreaking observational advances. The James Webb Space Telescope (JWST) is revolutionizing our view of the early universe, offering unprecedented insights into the timing and mechanisms behind the formation of the first galaxies and black holes. In this talk, I will present ongoing efforts to build a comprehensive picture of early galaxy and black hole formation, and to understand how the earliest galaxies reshaped the baryonic content of the universe during the epoch of Cosmic Reionization. At the same time, JWST has uncovered a surprising population of black holes at high redshifts, whose masses and abundance challenge existing models of black hole formation and growth.

Dark Energy and Neutrino Mass – Measurements from DESI DR2 using BAO

• Jiaxi Yu (Kavli IPMU)

Room: Koshiba Hall The DESI collaboration (Dark Energy Spectroscopic Instrument) confirmed its groundbreaking results on dynamical dark energy through the largest 3-dimensional Universe map it observed. This talk highlights how DESI Data Release 2 further challenges the ΛCDM paradigm: Baryon Acoustic Oscillation (BAO) measurements reveal a 2-4σ preference for dynamical dark energy, particularly when combined with external cosmic microwave background (CMB) data and Supernovae Ia (SNIa) data. Additionally, DESI sets the tightest upper limit on neutrino mass (Σm𝜈<0.064eV) under ΛCDM, though the posterior distributions intriguingly favour negative values. The dynamical dark energy model relaxes neutrino mass constraints and leaves open the possibility of inverted mass ordering. DESI will release its findings on cosmological parameters and primordial non-Gaussianity with its DR2 in the coming year. These results will further improve our understanding of the dark energy nature, neutrino mass ordering and early-Universe physics.

The Dark Universe with the Subaru Telescope

• Masamune Oguri (Chiba University)

Room: Koshiba Hall With its wide-field observing capability, the Subaru Telescope has been one of the most powerful telescopes in probing the dark Universe with the gravitational lensing effect. In this talk, I will describe the status of cosmological studies using the Subaru Telescope data.

Recent results of the T2K experiment

• Adrien Blanchet (CERN EP-NU)

Room: Koshiba Hall T2K is a neutrino experiment that measures neutrino and antineutrino oscillations using a long baseline of 295km, from the neutrino beam source at JPARC in Japan, to the Super-Kamiokande detector in Kamioka. The ND280 near detector at JPARC measures the properties of the neutrino beam prior to oscillations, while SuperK measures the beam after oscillations. In this talk, the most recent results of neutrino oscillations will be presented, featuring world-leading sensitivities on the search of Charge-Parity violation, by comparing oscillation measurements of neutrinos and antineutrinos. Measurements of the atmospheric oscillation parameters also extracted by observing the disappearance of muon neutrinos and the appearance of electron neutrinos. Combinations with other experiments such as SuperK and NOvA are also presented.

Yemilab (a deep underground laboratory in Korea) Physics

• Hyunsu Lee (Institute for Basic Science)

Room: Koshiba Hall Yemilab is a new underground laboratory in Jeongseon, South Korea, completed in September 2022. Situated at a depth of 1,000 m with an experimental area of 3,000 m², the facility is poised to host world-leading experiments in astroparticle physics. This talk will provide an overview of Yemilab's infrastructure and its pivotal physics programs, which are set to explore some of the most profound questions beyond the Standard Model. The flagship experiments at Yemilab are AMORE-II and COSINE-100U. The AMORE-II experiment will search for neutrinoless double beta decay in Mo-100 nuclei using molybdate-based scintillating crystals operated at millikelvin temperatures. Its goal is to probe the Majorana nature of neutrinos, with an ultimate sensitivity reaching an effective Majorana mass of 17-30 meV, which could provide crucial insights into the matter-antimatter asymmetry of the universe. The COSINE-100U experiment is a direct dark matter search designed to unambiguously verify the long-standing annual modulation signal reported by the DAMA/LIBRA collaboration. This upgraded experiment will utilize the existing low-background NaI(Tl) crystals, but with a novel encapsulation technique that significantly improves light collection by approximately 45%. Operating at low temperatures, COSINE-100U will feature enhanced sensitivity, especially for low-mass dark matter searches. Furthermore, Yemilab features a 6,300 m³ multipurpose cavern intended to house a next-generation large-scale neutrino detector. This future facility will enable a broad physics program, including high-precision measurements of solar neutrinos and searches for sterile neutrinos and dark photons. This presentation will cover the status and scientific goals of these key projects, highlighting Yemilab's role in advancing the frontiers of fundamental physics.

Gravittational wave science with LISA

• Astrid Lamberts (Observatoire de la Côte d'Azur)

Room: Koshiba Hall The LISA mission will detect milliHertz gravitational waves from space. In this band, we expect to observe thousands of white dwarf binaires in the Milky Way as well as supermassive black holes in the distant Universe. Certain detections should allow new tests of fundamental physics and cosmology measurements. In this presentation I will review the science objectives of the mission and some aspects of data analysis.

Cold Atom Quantum Technology to Explore Fundamental Physics

• Oliver Buchmueller (Imperial College London)

Room: Koshiba Hall In this presentation, I will outline the scientific opportunities presented by a multi-stage programme based on cold atom quantum technology. The central objectives of this programme include the search for ultra-light dark matter, the exploration of gravitational waves in the mid-frequency range—specifically between the peak sensitivities of LISA and LIGO/Virgo/KAGRA/INDIGO/Einstein Telescope/Cosmic Explorer experiments—and the investigation of other frontiers in fundamental physics. This programme will complement other planned dark matter searches, probe mergers involving intermediate-mass black holes, and explore early-universe cosmology. I will particularly focus on key activities in this field, such as the AION project in the UK and the international Terrestrial Very-Long-Baseline Atom Interferometry (TVLBAI) initiative, which is currently in the process of forming a proto-collaboration. The TVLBAI initiative aspires to establish a global network of large-scale atom interferometers designed to detect ultra-light dark matter and gravitational waves, with the ultimate aim of deploying kilometre-scale detectors by the mid-2030s. This collaboration is dedicated to developing a comprehensive roadmap, which will outline the scientific and technological milestones essential for the success of these groundbreaking detectors. Relevant References: • AION Collaboration. (2020). “AION: An Atom Interferometer Observatory and Network.” Journal of Cosmology and Astroparticle Physics, 2020(05), 011. arXiv:1911.11755 • Abend, S., et al. (2024). “Terrestrial Very-Long-Baseline Atom Interferometry: Workshop Summary.” AVS Quantum Science, 6(2), 024701. arXiv:2310.08183 • Abdalla, A., Abe, M., Abend, S., et al. (2025). “Terrestrial Very-Long-Baseline Atom Interferometry: Summary of the Second Workshop.” EPJ Quantum Technology, 12(1), Article 42. https://doi.org/10.1140/epjqt/s40507-025-00344-3

ATLAS results on Beyond the Standard Model Physics

• Valerio Ippolito (Istituto Nazionale di Fisica Nucleare)

Room: Koshiba Hall Many theories beyond the Standard Model (SM) have been proposed to address several of the SM shortcomings, such as explaining why the Higgs boson is so light, the origin of neutrino masses, or the observed pattern of masses and mixing angles in the quark and lepton sectors. Many of these beyond-the-SM extensions predict new particles or interactions directly accessible at the LHC. This talk will present some highlights on recent searches based on Run 2 and Run 3 data collected by the ATLAS collaboration.

Recent results and future prospects from the Belle II experiment

• Michele Veronesi

Room: Koshiba Hall The Belle and Belle II experiments have collected a combined sample of 1.2 ab$^{-1}$ of $e^+e^- \to B \overline{B}$ collisions at a centre-of-mass energy corresponding to the $\Upsilon(4S)$ resonances. These data, with low particle multiplicity and constrained initial state kinematics, are an ideal environment for studying the properties of bottom mesons, such as semileptonic and rare electroweak penguin decays to final states with missing energy from neutrinos, and search for dark sector particles in the mass range from a few MeV to 10 GeV. In addition, the boost provided by the asymmetric SuperKEKB collider allows to perform measurements of time-dependent CP violation. These samples also contain a large number of $e^+e^- \to c\overline{c}$ and $e^+e^- \to \tau^+\tau^-$ pairs, which are used to study the properties of charm hadrons and tau leptons. In this talk we will present recent results and future prospects from several areas of the Belle II physics program.

Cosmic Inflation: From Small to Large Scales

• Jason Kristiano (Kyoto University)

Room: Koshiba Hall Structures in the universe can be formed because of small inhomogeneities at a very early time. These inhomogeneities originate from quantum fluctuations stretched by cosmic inflation. As we know from wave mechanics, fluctuations are characterized by amplitude and wavelength. Fluctuations with wavelength as long as observable universe, with amplitude around 0.00001, can explain cosmic microwave background observations and galaxies density correlations in large-scale structures. However, for the short-wavelength one, so far there have been no observational constraints on the amplitude. If the amplitude exceeds 0.1, they can collapse to form primordial black holes. These primordial black holes can have interesting consequences, such as explaining dark matter or LIGO-Virgo-KAGRA black holes. So far, these theoretical predictions rely on linear perturbation theory. However, it is reasonable to expect large nonlinearities due to large fluctuations, which are manifested in coupling between small and large scales. In this talk, I will review primordial black holes formation in single-field inflation and recent progress on nonlinear computation. I will argue that large amplitudes of short-wavelength fluctuations can coherently amplify the long-wavelength one by loop corrections. I will also explain some issues on regularization and renormalization of these loops.

The Euclid mission and the quest for dark energy

• Francis Bernardeau (IPhT Saclay)

Room: Koshiba Hall After introducing the scientific and observational concepts on which the instruments of Euclid have been based, I will present an overview of ongoing and forthcoming surveys, outlining their key characteristics and timelines for observations and data releases. Particular emphasis will be placed on revisiting the mission’s core scientific objectives, with a focus on the specific probes and observables employed to constrain the dark energy properties. In particular, I will explore how Euclid's observations can be used to gain insights into our understanding of the development of gravitational instabilities accros cosmic scales and time.

Primordial Gravitational Wave Measurement with the LiteBIRD Space Mission

• Guillaume Patanchon (ILANCE)

Room: Koshiba Hall LiteBIRD (Lite satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection) is a JAXA-led space mission designed to probe the primordial universe by measuring the polarization of the cosmic microwave background (CMB) with unprecedented sensitivity. Scheduled for launch in the 2030s, LiteBIRD aims to detect the imprint of primordial gravitational waves through large-scale B-mode polarization, providing a powerful test of inflationary cosmology. The mission will carry out a full-sky survey over three years from the second Lagrange point (L2), with broad frequency coverage and high sensitivity—both essential for disentangling the cosmological signal from other polarized emissions. In this talk, I will present LiteBIRD’s scientific goals, observation strategy, instrument technology and design, as well as the challenges involved in extracting the tiny B-mode signal from the data. These include separating polarized Galactic emissions—primarily thermal dust and synchrotron radiation—and characterizing and mitigating instrumental systematics.

Gravitational-wave astronomy using ground-based detectors

• Ajith Parameswaran (Tata Institute of Fundamental Research, Bangalore)

Room: Koshiba Hall Recent detections of gravitational waves (GWs) have ushered in a new branch of astronomy. During their past observing runs, the LIGO and Virgo detectors have observed over two hundred mergers of compact binaries involving black holes and neutron stars. These discoveries have enabled novel tests of general relativity, offered new probes of cosmology and dense nuclear matter, and posed intriguing questions about the astrophysical formation mechanisms of compact binaries. This talk will present an overview of the key results from GW observations to date and discuss future prospects in this rapidly evolving field.

Unlocking the Non-Thermal Universe: Future Gamma-Ray Discoveries with CTAO

• Monica Seglar-Arroyo (Institut de Fisica d'Altes Energies (IFAE))

Room: Koshiba Hall The Cherenkov Telescope Array Observatory (CTAO) will be the world’s first open, ground-based gamma-ray observatory, offering full-sky coverage through two sites — the Northern site at the Observatorio Roque de los Muchachos (La Palma, Spain), and the Southern site at the ESO Observatorio Paranal (Chile). Designed for a 30-year operation, CTAO will deliver groundbreaking insights across a wide range of topics — from cosmic rays acceleration process, to the nature of extreme astrophysical environments, and probes of fundamental physics. CTAO will significantly surpass the sensitivity, angular resolution, and energy coverage of current imaging Cherenkov telescope arrays. The Large-Sized Telescope 1 (LST-1), operational since 2018, is hinting full CTAO array capabilities through early results on gamma-ray bursts (GRBs), active galactic nuclei (AGNs), pulsars, and novae. Once the full array is operational, CTAO will cover an energy range from 20 GeV to 300 TeV with unprecedented precision. This contribution presents an update on the status of the CTAO project and outlines its broad scientific capabilities. Special attention will be given to its performance in the time multi-messenger domain. CTAO’s design enables rapid slewing, a large effective collecting area, and high temporal resolution, uniquely positioning the observatory to capture fast transients and respond in real time to multi-messenger events. Its role in time-domain, multi-wavelength, and multi-messenger astrophysics will be crucial to unlocking the dynamic, non-thermal universe.

The Hubble Tension

• Sherry Suyu (Max Planck Institute for Astrophysics / Technical University of Munich)

Room: Koshiba Hall The Hubble constant (H0) is a key parameter in cosmology that sets the expansion rate and the age of the Universe. Independent determinations of H0 are important to ascertain the possible need of new physics beyond the standard cosmological model, given the tension in current H0 measurements from the cosmic microwave background observations of Planck and the local distance ladder from the SH0ES program. I will give an overview of recent H0 measurements from different methods, with a focus on strong gravitational lensing as a competitive cosmological probe.

Outlook on Neutrino Theory and Phenomenology

• Salvador Rosauro Alcaraz (INFN Sezione di Bologna)

Room: Koshiba Hall The discovery of neutrino oscillations, and hence of nonzero neutrino masses, provides one of the clearest indications of physics beyond the Standard Model. In this talk, we will review theoretical developments that address the origin of neutrino masses and discuss their phenomenological implications.

Recent results and status of the SNO+ experiment on its journey towards Neutrinoless Double Beta Decay

• Will Parker (University of Oxford)

Room: Koshiba Hall SNO+ is a large, multi-purpose neutrino detector located 2 km underground at SNOLAB, Canada, with the main goal of searching for the neutrinoless double beta decay ($0\nu\beta\beta$) of $^{130}$Te. The detector is currently operating with 780 tonnes of liquid scintillator as its active target mass. The combination of high light yield, low intrinsic background levels, and steadily increasing livetime enables the SNO+ collaboration to pursue a broad physics program. This includes measurements of solar neutrinos, detection of antineutrinos from nuclear reactors and from the Earth, as well as searches for other rare processes. SNO+ performed the first observation of the charged-current interaction of solar neutrinos with $^{13}$C, marking a significant milestone in low-energy neutrino detection and demonstrating the detector’s sensitivity to rare interaction channels. In parallel, the spectral analysis of reactor antineutrino oscillation led SNO+ to obtain the second-most precise determination of $\Delta m^{2}_{21}$ and to perform the first measurement of the flux of geoneutrinos in the Western Hemisphere. The scintillator data is also being used to quantify backgrounds and understand the detector response in preparation for the search of neutrinoless double beta decay. In a first phase, SNO+ will perform this search with 0.5% of natural tellurium by weight, targeting a predicted half-life sensitivity of $2\times10^{26}$ years (90% CL) with 3 years of livetime, followed by higher tellurium loadings, up to 3%, for sensitivities above $10^{27}$ years. In this talk I will present the most recent physics results from the analysis of the SNO+ scintillator data, and will discuss the status and prospects for the neutrinoless double beta decay search.

Probing the Nature of Neutrino Mass

• Karsten Heeger (Yale University)

Room: Koshiba Hall The discovery of neutrino oscillation has shown that neutrinos have non-zero mass but the nature of neutrino mass and the absolute mass scale remain unknown. Neutrinoless double beta decay (0νββ) is uniquely suited to probe the Majorana nature of neutrinos and determine the effective neutrino mass. CUORE, the Cryogenic Underground Observatory for Rare Events (CUORE) and its upgrade CUPID aim to search for 0νββ down to the level of the inverted mass ordering using the world’s largest bolometric detector. Project 8 represents a novel approach to directly measure the absolute neutrino mass using cyclotron radiation emission spectroscopy. In this talk. I will present the latest results from CUORE, the plans for CUPID, and the prospect for measuring the neutrino mass with Project 8

Physics and Status of Linear e+e- Higgs factory projects

• Taikan Suehara (ICEPP, The University of Tokyo)

Room: Koshiba Hall Development of linear e+e- collider with >= 250 GeV center-of-mass energy has a long history. One of the milestones is the publishment of ILC technical design report in 2013, proposing a global ILC project. Recently for the coming European strategy update, a LC facility at CERN is also proposed and is under discussion as a possible flagship project at CERN. In this talk I will present the physics and technology aspects of linear Higgs factory projects, with a highlight to comparison as well as synergies to the circular options, and possible ways to proceed.

CMS results on Quark and lepton Flavor Physics

• Riccardo Manzoni (ETH Zurich)

Room: Koshiba Hall CMS results on Quark and lepton Flavor Physics

ALICE Highlights and Upgrade Plans

• Jacek Otwinowski (Institute of Nuclear Physics Polish Academy of Sciences)

Room: Koshiba Hall A Large Ion Collider Experiment (ALICE) is one of the four major experiments at the Large Hadron Collider (LHC). It was designed to study the properties of the quark-gluon plasma (QGP) - a state of extremely hot and dense matter in which quarks and gluons are deconfined. This state is created in high-energy heavy-ion collisions and resembles the conditions of the early universe moments after the Big Bang. Since 2009, ALICE has successfully collected data from various collision systems, including A–A (Pb–Pb, Xe–Xe, O–O), p–A (p–Pb, p–O), and pp. This presentation will review recent highlights from ALICE and outline its ambitious short- and long-term upgrade plans.

ATLAS Results on Quark and Lepton Flavor Physics

• Sally Seidel (University of New Mexico)

Room: Koshiba Hall Measurements by the ATLAS Experiment of quark and lepton flavor processes, using the LHC Run 2 data, are presented. These include differential cross section measurements of charmed mesons and a new precision measurement of the neutral B meson lifetime. They also include tests of lepton flavor universality in W-boson decays and in the context of high mass top pair-lepton pair production, as well as a search for charged lepton flavor violation in top quark production.

The mass in the Galactic Center

• Stefan Gillessen (MPE)

Room: Koshiba Hall Near-infrared observations of individual stellar orbits have revealed that the Galactic Center hosts a compact mass of around 4.3 million solar masses, honored with the Nobel prize in physics in 2020. By the advent of near-infread interferometry, the resolution and astrometric precision have been increased recently by almost an order of magnitude, turning the stellar system around Sgr A* into a laboratory for testing general relativity aorund a large mass. Further, stellar orbits probe the Newtonian mass content in the Galactic Center, and provide stringent constraints on how much dark objects can reside around Sgr A*, and constitutes thus a test case for the dynamical modelling used to predict extreme-mass ratio inspiral rates for gravitational wave observations.

Role of interstellar bubbles and molecular filaments in the formation of stars

• Doris Arzoumanian (Kyushu University)

Room: Koshiba Hall Star formation is a continuous cycle of interchange of matter and energy between stars and the interstellar medium of galaxies. As a result of a complex interplay between gravitational, kinetic, and magnetic energies, shock compressions, and heating/cooling processes, the matter is assembled from the diffuse, large-scales to the dense, small-scales, where gravity prevails over the pressure forces, thereby driving the gravitational collapse into dense cores, the seeds of future stars. In this presentation, I will review recent theoretical and observational works proposing a comprehensive physical scenario for the growth of dense structures from giant interstellar bubbles driven by stellar feedback on ~50-100 pc scales to parsec-scale molecular filaments down to <0.1pc dense cores and 100-1000 au scale protoplanetary disks, where new planets form.

Radio Detection: Advances, Challenges, and Future Directions

• Olivier Martineau (LPNHE)

Room: Koshiba Hall Pioneered in the early 2000’s, radio is now an established technique for the detection of ultra-high energy particles of cosmic origin. I will introduce the basic concepts of radio emission by the extensive particle showers induced by the interaction in the atmosphere of these cosmic messengers, and the detection of these electromagnetic radiations by radio antennas. I will present the experimental status of the main projects in the field, stress the challenges specific to autonomous radio detection, and review the prospects in the field for the next decade.

Fast radio bursts as precursor radio emission from monster shocks

• Arno Vanthieghem (Observatoire de Paris)

Room: Koshiba Hall It has been proposed recently that the breaking of MHD waves in the inner magnetosphere of strongly magnetized neutron stars can power different types of high-energy transients. Motivated by these considerations, we study the steepening and dissipation of a strongly magnetized fast magnetosonic wave propagating in a declining background magnetic field, by means of particle-in-cell simulations that encompass MHD scales. Our analysis confirms the formation of a monster shock, that dissipates about half of the fast magnetosonic wave energy. It also reveals, for the first time, the generation of a high-frequency precursor wave by a synchrotron maser instability at the monster shock front, carrying a fraction of 0.1% of the total energy dissipated at the shock. The spectrum of the precursor wave exhibits several sharp harmonic peaks, with frequencies in the GHz band under conditions anticipated in magnetars. Such signals may appear as fast radio bursts.

Observing gravitational waves with Pulsar Timing Array

• Stanislav Babak (APC)

Room: Koshiba Hall Several Pulsar Timing Array (PTA) collaborations are currently searching for gravitational waves (GWs) in the nano-Hz frequency band by monitoring a network of millisecond pulsars. This review will first introduce the fundamental principles behind detecting GWs through long-term timing of pulsars. We then briefly discuss different GW sources accessible to PTAs and the detection of the emerging stochastic GW signal. Finally, we focus on GWs produced by a population of supermassive black hole binaries and explore their expected properties using insights from the large-scale hydrodynamic simulation Horizon-AGN.

Recent NOvA Results and the Joint NOvA–T2K Analysis

• Mayly Sanchez (Florida State University)

Room: Koshiba Hall NOvA is one of the two leading long-baseline neutrino oscillation experiments currently in operation. It uses the 700 kW NuMI neutrino beam at Fermilab directed towards northern Minnesota in the US with two functionally identical scintillator-based detectors placed 810 km apart at off-axis locations. An arrangement that largely cancels common systematic uncertainties in neutrino oscillation measurements. By analyzing neutrino charged-current interactions in these detectors, the NOvA experiment studies muon neutrino disappearance and electron neutrino appearance to probe still undetermined physics parameters, such as the neutrino mass ordering, CP violation and the octant of the large mixing angle. NOvA can also study the disappearance of all three known neutrino flavors by analyzing neutral current interactions, thus enabling searches for physics beyond the three-flavor paradigm, such as mixing with light sterile neutrinos. In this talk, I will present the latest NOvA results and discuss the joint analysis performed together with the T2K collaboration, which combines the data sets of both experiments to enhance sensitivity to CP violation and neutrino mass ordering.

Supernova and transient science with the telescope network including Subaru

• Keiichi Maeda (Kyoto University)

Room: Koshiba Hall Recent development in transient observations has revealed a rich diversity of a transient zoo. Discovering new transients and characterize their natures requires global telescope networks involving various telescopes and instruments at different locations. The Subaru telescope has been playing unique roles in the network, including (1) the capability of performing a deep and wide survey to discover new transients with a different parameter space than other survey telescopes with the smaller diameter, (2) the potential in search for optical counterparts of transients discovered either in different wavelengths or different messengers (e.g., gravitational wave), and (3) deep follow-up observations of transients with different modes (e.g., polarization). In this talk, I will introduce some recent activities of transient observations including the findings obtained with the Subaru telescope in these aspects, especially focusing on the emerging diversity of supernova explosions that calls for a major update in the stellar evolution theory.

The Universe at z > 10 and the first population of stars and galaxies

• Denis Burgarella (Laboratoire d'Astrophysique de Marseille)

Room: Koshiba Hall The discovery of UV-bright galaxies at redshifts z > 10 by JWST, now complemented by ALMA detections of dust and gas emission, has opened an observational window onto the first few hundred million years of cosmic history. These galaxies appear more numerous, more massive, and more evolved than predicted by standard ΛCDM-based models of early structure formation. Their existence poses a tension with theoretical expectations based on the limited time available for halo growth, star formation, and metal enrichment. In this talk, I will review the current observational landscape: the rapidly increasing sample of high-z galaxy candidates, constraints from their UV luminosity functions, and spectroscopic confirmations. I will emphasize the implications for models of early galaxy formation, including star formation efficiency, feedback. ALMA observations add further weight to the puzzle by revealing significant dust and metal content at unexpectedly early time but no confirmed detections of the very first generation of stars. This tension—between what we see and what standard theory allows—invites a broader reflection on the interface between observational cosmology and fundamental physics. Are these galaxies outliers, or are we witnessing early hints that physics at the largest scales is probing constraints rooted in the microphysics of the early Universe? This question lies at the heart of the physics of the two infinities.

Low-Energy-beyond-the-Standard-Model Experiments

• Toshiyuki Iwamoto (The University of Tokyo)

Room: Koshiba Hall I will review the low energy experiments which will look for new physics beyond the Standard Model.

Detector Technology

• Yuji Enari (KEK IPNS)

Room: Koshiba Hall Detectors play a pivotal role in advancing particle physics. The evolution of detector technologies starting from on-going experiments at the LHC, and outlines the emerging trends shaping the design of next-generation collider detectors will be reviewed. Key developments include increased granularity with low material, low power consumption, and the integration of real-time data processing will be discussed. Then, I will highlight recent progress on low temperature sensors, which are essential technology for future experiments. Review on needs of temperature for particle physics experiments and their technology to achieve the environment. Development plan in Japan, including cryo-CMOS and low-cost cryogenics system will be discussed.

AI and Machine Learning for Neutrino Physics

• Patrick de Perio (Kavli IPMU, University of Tokyo)

Room: Koshiba Hall Neutrino experiments around the world are entering a regime where statistical uncertainties are no longer dominant, placing new emphasis on controlling systematics. Alongside advances in detector technology, this shift demands unprecedented precision in detector modeling, simulation, event reconstruction, analysis, and experimental design and operations. Future techniques must be rapid, scalable, and capable of addressing high-dimensional data by extracting maximal information from complex event topologies while mitigating mismodeling effects. This talk surveys the key challenges facing neutrino physics and highlights emerging AI/ML approaches that offer promising solutions.

Advances in Reactor Neutrino Measurements

• J. Pedro Ochoa-Ricoux (University of California, Irvine)

Room: Koshiba Hall The intense and well-characterized neutrino flux produced by the beta decays of fission products in nuclear reactors offers a powerful tool to study the properties of these elusive particles. This talk will present an overview of recent advances from reactor neutrino experiments at short baselines, including precision measurements of neutrino oscillation parameters and searches for physics beyond the Standard Model.

Newest results from Super-Kamiokande

• Andrew Santos

Room: Koshiba Hall The Super-Kamiokande (SK) experiment is a world-leading, 50-kton water Cherenkov detector in Japan. Since the last iteration of the P2I Conference in 2023, several important results have been made public by SK, and we explore highlights here. These include the newest analysis of solar neutrinos, the hunt for the Diffuse Supernova Neutrino Background, and latest atmospheric neutrino oscillation results. We will also underline the important impact of introducing gadolinium sulfate into the water at 0.01% and 0.03% Gd-loading by mass in 2020 and 2022, respectively.

Status and perspectives of KAGRA

• Soichiro Morisaki (Research Center for the Early Universe, the University of Tokyo, Japan.)

Room: Koshiba Hall KAGRA is an underground interferometric gravitational-wave detector located in Kamioka, Gifu, Japan. It began observations in 2020 and achieved its first joint run with LIGO and Virgo in 2025. In this talk, I will present the current status of KAGRA and discuss its future prospects.

Strong-Field Tests of Gravity with Gravitational Waves: Current Status and Future Directions

• Kent Yagi (University of Virginia)

Room: Koshiba Hall Gravitational waves provide a unique window into the strong-field regime of gravity, offering powerful opportunities to test general relativity and explore possible deviations. In this talk, I will review the current status of gravitational-wave–based tests of gravity and summarize the key insights gained so far. I will then discuss how upcoming observations with next-generation detectors will enhance these tests, and what new physics we may uncover in the near future.

CMS Results on the Higgs Boson and Electroweak Physics

• Andrey Pozdnyakov (RWTH Aachen University)

Room: Koshiba Hall In this presentation, we explore the production mechanisms of W, Z, and Higgs bosons, alongside the top quark, at the Large Hadron Collider (LHC). We examine how these particles are detected using the capabilities of the CMS Experiment. The talk will highlight the latest advancements in Higgs boson physics, focusing on detailed measurements of its production rates across various decay channels. Additionally, we will present recent significant findings in electroweak physics involving W, Z, and top particles. These results offer valuable insights into fundamental particle interactions and contribute to our understanding of the Standard Model.

LHCb overview

• Sergey BARSUK (IJCLab)

Room: Koshiba Hall Latest results from LHCb and future perspectives will be presented.

Neutrino oscillations: challenges and perspectives from an experimentalist point of view

• Christophe Bronner (Yokohama National University)

Room: Koshiba Hall Since the discovery of neutrino oscillations at the end of the 20th centuries, experiments studying the have reached a number of milestones and measured most of the parameters of the standard 3 flavor oscillation model with increasing precision. Experiments are now trying to address the remaining open questions (CP symmetry in oscillations and neutrino mass ordering in particular) which require measuring more subtle variations in the oscillation patterns. In this presentation, we will look at some of the specific challenges faced by these experiments and ideas proposed to address them, as well as perpectives in terms of both measuring parameters of the model, and testing the standard oscillation framework in search of new physics.

12 Years of Discoveries from the IceCube Neutrino Observatory

• Naoko Kurahashi Neilson (Drexel University)

Room: Koshiba Hall The IceCube Neutrino Observatory has made milestone observations in neutrino astronomy, multi-messenger astronomy, cosmic-ray physics, and particle physics for over a decade. This talk will cover historic triumphs, including those that started the field of neutrino astronomy, as well as recent highlights such as the observation of the Galactic Plane in neutrinos, the emergence of Seyfert galaxy NGC 1068 as a steady high-energy neutrino source, and competitive neutrino oscillation parameter measurements. The ongoing IceCube Upgrade deploys newly developed detector modules and will increase our understanding of our detector and the properties of the instrumented ice. The effort also leads the way to a future generation neutrino observatory, IceCube-Gen2, with capabilities to answer many questions raised by these discoveries.

Mapping the Dark Universe: Prospects for Dark Matter Science with Euclid

• Linda Blot (CD3, Kavli IPMU)

Room: Koshiba Hall The Euclid space telescope, launched by the European Space Agency, is set to transform our understanding of the dark sector by delivering high-precision measurements of weak gravitational lensing and galaxy clustering across 15,000 square degrees of the sky. This unprecedented data set will enable detailed mapping of the large-scale structure of the Universe and provide powerful tools to probe the nature of dark matter beyond the standard cold dark matter paradigm. Euclid's sensitivity to the matter distribution over cosmic time opens up the possibility to test models involving warm dark matter, ultra-light scalar fields, self-interacting dark matter, and other non-standard scenarios. In this talk, I will present an overview of the scientific potential of Euclid for dark matter research, focusing on the observational strategies and theoretical frameworks being developed ahead of the mission’s first data release. I will highlight how Euclid’s photometric and spectroscopic capabilities can be combined with other probes, including cosmic microwave background data, strong lensing, and stellar stream studies, to constrain the clustering, interactions, and microphysical properties of dark matter.

Dark Matter: the odds have changed

• Joe Silk (IAP)

Room: Koshiba Hall The strongest experimental evidence for dark matter is the Galactic Center gamma-ray excess observed by the Fermi telescope and even predicted prior to discovery as a potential dark matter signature via WIMP dark matter self-annihilations. However, an equally compelling explanation of the excess gamma-ray flux appeals to a population of old millisecond pulsars that also accounts for the observed boxy morphology inferred from the bulge old star population. We employ a set of Milky Way-like galaxies found in the Hestia constrained simulations of the local universe to explore the rich morphology of the central dark matter distribution, motivated by the GAIA discovery of a vigorous early merging history of the Milky Way galaxy. We predict a significantly non-spherical gamma-ray morphology from the WIMP interpretation. Future experiments, such as the Cherenkov Telescope Array, that extend to higher energies, should distinguish between the competing interpretations.

Vera C. Rubin Observatory : future of cosmology with the world's largest digital camera

• Enya Van den Abeele

Room: Koshiba Hall The NSF-DOE Vera C. Rubin Observatory revealed its first images to the world on June 23 2025, taken with the world's largest digital camera. With a field of view of 9.6 deg², this 3200-megapixel camera will scan the entire southern sky in only three nights and in six color bands over a period of ten years. Combined with wide-field optics, the Vera C. Rubin camera will produce images of unprecedented depth, revealing very distant and faint objects that have not yet been observed. This ten-years survey called LSST (Large Survey of Space and Time) is expected to drive significant progress in cosmology and astrophysics, particularly in constraining dark matter and dark energy. After presenting the observatory with a focus on French contributions, I will provide an overview of the scientific topics that will be addressed using Rubin data. I will place particular emphasis on cosmological analyses that can be performed using the weak lensing probe, highlighting the importance of photometric and astrometric calibration in order to achieve the high-precision objectives.

The Einstein Telescope: challenges and opportunities of a third-generation detector

• Ulyana Dupletsa (HEPHY - OEAW)

Room: Koshiba Hall The Einstein Telescope (ET) is a European project for a third-generation gravitational-wave detector designed to increase the sensitivity of present interferometers by approximately one order of magnitude. Two reference designs are currently under investigation: a triangular-shaped detector with 10 km arms, and a configuration with two L-shaped detectors with 15 km arms, both located in Europe. Each arm will host a ‘xylophone’ setup of two interferometers: one optimized for high frequencies, the other, cryogenic, for low frequencies. This design will significantly expand the observable volume of the Universe and improve source parameter estimation. In this contribution, we outline the scientific program of the ET, tracing the project's evolution, current status, and prospects. We give an overview of the technological challenges, especially for the low-frequency instrument, and the scientific reach of a third-generation detector like ET, highlighting the potential for discoveries in fundamental physics, multi-messenger astrophysics, and cosmology.

Future Accelerators Projects

• Nicolas Morange (IJCLab)

Room: Koshiba Hall While the HL-LHC will be the only high-energy collider running in the next decade, the need for a deeper understanding of the electroweak symmetry breaking and the searches for physics beyond the Standard Model call for a next generation of accelerators. The concensus in the particle physics community is that of a Higgs factory and an exploration machine in the 10-TeV energy regime. The ongoing process of the Update of the European Strategy for Particle Physics provides an opportunity to compare these projects for the post-LHC era: circular e+e- and hadron colliders, linear e+e- colliders, and muon colliders. This presentation will review the various future accelerator projects proposed, in terms of physics programme, challenges, and timescales. A particular focus will be put on CERN's Future Circular Collider, whose feasibility study was successfully completed for the Strategy Update.

Beyond the Standard Model (Theoretical overview)

• Ryuichiro Kitano (YITP, Kyoto U.)

Room: Koshiba Hall I review the current status of Beyond the Standard Model physics. From the perspectives of flavor, electroweak interactions, QED, QCD, gravity, and cosmology, I discuss the theoretical frameworks suggested by these viewpoints and explore how they can be tested experimentally.

Multi-Messenger Astronomy

• Natalia Lewandowska (State University of New York at Oswego)

Room: Koshiba Hall In the age of ground-based and space telescopes it has been well established that multi-wavelength observations of astrophysical sources are a crucial observing strategy to unravel their physics. What began once with the multi-wavelength study of the messenger of the electromagnetic force has advanced in the last decades also towards the messengers of the other three fundamental forces: the gravitational, weak and strong nuclear forces. In this talk I will give a general overview of this now established field known as "Multi-Messenger Astronomy" with a focus on very fast rotating and highly magnetized neutron stars known as pulsars as well as black holes.

JWST: A Game Changer for the Study of Exoplanets

• Pierre-Olivier Lagage (CEA)

Room: Koshiba Hall Are we alone in the universe? For decades, scientists have sought to place our Solar System in a broader cosmic context. A major breakthrough occurred in 1995, when Michel Mayor and Didier Queloz discovered the first exoplanet orbiting a Sun-like star—a milestone that earned them the 2019 Nobel Prize in Physics. Since then, over 6,000 exoplanets have been detected, revealing an astonishing diversity: from hot Jupiters in close orbits to super-Earths, lava worlds, ocean planets—many with no equivalent in our Solar System. While the search for new exoplanets continues, a new chapter is now being written, thanks to the James Webb Space Telescope (JWST): the characterization of exoplanet atmospheres. In this talk, I will briefly review what we have learned so far about the atmospheres of giant exoplanets, and then focus on rocky exoplanets. I will show how the measurement of the temperature of exoplanets can help determining whether or not they possess an atmosphere. In particular, I will highlight recent findings from the TRAPPIST-1 system—a remarkable system of a very small star surrounded by seven Earth-sized planets, three of which lie in the so-called "habitable zone." I will end by looking ahead the next-generation observatories that will be specially designed to search for biosignatures in the atmosphere of Earth-like exoplanet orbiting Sun-like stars.

The Physics of the two Infinities; a personal view from an experimental physicist

• Takaaki Kajita (University Tokyo)

Room: Koshiba Hall I will present what I think are important to further understand the smallest particles and the largest Universe as seen as an experimental physicist.