Journées de Rencontre Jeunes Chercheur·se·s 2026

22 nov. 2026, 00:00 → 28 nov. 2026, 00:00 Europe/Paris

 

(English version, for French see below)

Organised by the sections "Fields and Particles" and "Nuclear Physics" of the Société Française de Physique (SFP), the "Journées de Rencontre des Jeunes Chercheur·se·s 2026" welcomes all PhD students (from the first to the last year) and young postdocs.

This year it will be held from November 22 to 28, 2026, at the Saint-Jacut Abbey in Saint-Jacut-de-la-Mer (22) – France.

The JRJCs are an occasion for each participant to present their work in a convivial atmosphere and to obtain from their colleagues an overview of the current research going on in France in the domain.

This year the following subjects are proposed : Instrumentation and accelerators - Hadronic physics - Standard Model - Physics beyond the Standard Model - Nuclear structure - Nuclear energy - Medical physics and interdisciplinarity - Gravitational waves - Flavor physics - Astroparticles - Cosmology - Neutrinos - Theory

Presentations can be given either in English or French. The conference social program foresees a half-day trip in the nearby area, as well as a public seminar. The deadline for registration is October 9th, 2026. For any other information please feel free to contact the secretary or any member of the organising committee (see below).

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(Français)

Organisées par les divisions "Champs et Particules" et "Physique Nucléaire" de la Société Française de Physique (SFP), les Journées de Rencontre des Jeunes Chercheur·se·s 2026 s'adressent à tous les étudiants en thèse (de la première à la dernière année) et aux jeunes post-doctorants.

Elles auront lieu du 22 au 28 novembre 2026 et se tiendront à l'abbaye de Saint-Jacut-de-la-Mer (22) – France.

Les JRJC sont l'occasion pour chaque participant de présenter ses travaux de recherche dans une ambiance conviviale et de partager avec ses collègues une vue d'ensemble des différentes recherches menées à l'heure actuelle dans sa spécialité et dans des domaines proches.

Les thèmes proposés cette année sont les suivants : Instrumentation et accélérateurs - Physique hadronique - Modèle Standard - Physique au-delà du Modèle Standard - Structure nucléaire - Énergie nucléaire - Physique médicale et interdisciplinaire - Ondes gravitationelles - Physique des saveurs - Astroparticules - Cosmologie - Neutrinos - Théorie

La langue de travail des JRJC est le français, mais les non-francophones peuvent donner leur exposé en anglais. Le programme social comprend, outre une excursion dans la région, une conférence invitée pouvant être ouvertes au public. Le date limite d'inscription est fixée au 9 octobre 2026. Pour tout renseignement complémentaire, n'hésitez pas à contacter notre secrétariat ou bien un membre du comité d'organisation (voir ici de suite).

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Francois Brun (CEA Saclay)	francois.brun@cea.fr
Luca Cadamuro (IJCLab)	luca.cadamuro@cern.ch
Sami Caroff (LAPP)	sami.caroff@lapp.in2p3.fr
Rachel Delorme (LPSC)	rachel.delorme@lpsc.in2p3.fr
Louis D'Eramo (LPCA)	louis.deramo@clermont.in2p3.fr
Giulia Di Gregorio (IJCLab)	giulia.digregorio@ijclab.in2p3.fr
Andreas Goudelis (LPCA)	andreas.goudelis@clermont.in2p3.fr
Sabrina Sacerdoti (APC)	sacerdoti@apc.in2p3.fr
Thomas Strebler (CPPM)	strebler@cppm.in2p3.fr
Antonio Uras (IP2I)	antonio.uras@cern.ch

Affiche-JRJC2026-V1-2-4K.pdf

Circulaire2026_1_EN.pdf

Circulaire2026_1_FR.pdf

Circulaire2026_2_EN.pdf

Circulaire2026_2_FR.pdf

lun. 23 novembre

Introduction

Standard Model

Président de session: Bruna Osorio Pascual (Laboratoire de Physique Clermont-Auvergne (LPCA))

1 Session overview

Orateur: Bruna Osorio Pascual (Laboratoire de Physique Clermont-Auvergne (LPCA))

2 Talk SM #1

Orateur: Omar ISTAITIA (IJCLab)

10:20 Coffee break

Standard Model

Président de session: Bruna Osorio Pascual (Laboratoire de Physique Clermont-Auvergne (LPCA))

3 Talk SM #3

Orateur: William Roth (LPNHE)

4 Talk SM #4

Orateur: Mlle Hind Taibi

5 Talk SM #5

Orateur: Nicolas Cartalade

6 Latest HL-LHC b-tagging developments and expected impact on di-Higgs sensitivity

The High-Luminosity Large Hadron Collider (HL-LHC) will open new opportunities for the study of rare processes, including Higgs boson pair (di-Higgs) production. Flavour tagging will play a central role in enabling these measurements. This talk presents the expected challenges for flavour tagging in the HL-LHC environment, characterized by unprecedented instantaneous luminosity, high pile-up conditions, and the upgraded ATLAS detector. Particular emphasis is placed on the expected performance of the transformer neural network GN2 when trained and evaluated on simulated Run 4 datasets. In addition, we explore the potential of exploiting relaxed track selections within the GN2 architecture to further enhance flavour-tagging performance, discussing the trade-offs between potential gains in tagging performance and the increased computational resources required for track reconstruction. Finally, the implications for future di-Higgs analyses are discussed, highlighting the critical importance of flavour-tagging performance and reconstruction strategies for achieving sensitivity to this key measurement in the Higgs sector.

Orateur: Vincenzo Triglione (CPPM, Aix-Marseille Université, CNRS/IN2P3 (FR))

12:30 Lunch break

7 Abbay visit

Standard Model

Président de session: Bruna Osorio Pascual (Laboratoire de Physique Clermont-Auvergne (LPCA))

8 Talk SM #6

Orateur: M. Tom FOURNIER (APC Paris CNRS/IN2P3)

9 Talk SM #2

Orateur: Mlle Eléa Paquis (LPSC-Grenoble CNRS/IN2P3)

Theory

Président de session: Quentin Bonnefoy (Uni. de Strasbourg & IPHC)

10 Session overview

Orateur: Quentin Bonnefoy (Uni. de Strasbourg & IPHC)

16:20 Coffee break

Theory

Président de session: Quentin Bonnefoy (Uni. de Strasbourg & IPHC)

11 Piezoaxionic Detection of Axion Dark Matter with Precessing Nuclear Spins

The piezoaxionic effect enables the conversion of axion-induced spin-dependent forces in polarized nuclei into measurable voltages in piezoelectric crystals. We propose a heterodyne detection scheme in which controlled nuclear spin precession mixes the axion oscillation frequency with the nuclear Larmor frequency. This generates sideband signals at shifted frequencies, allowing efficient scanning of axion masses through the applied magnetic field. This approach provides a tunable and noise-resilient strategy to probe QCD axion dark matter in the MHz–GHz range.

Orateur: Baraa Yahya (IPhT (CEA-SACLAY))

12 Axion production in core-collapse supernovae

During the gravitational collapse of a massive star, the proto-neutron-star core reaches extreme densities and temperatures, providing an environment in which QCD axions can be efficiently produced through their interactions with baryonic matter. Axion emission may contribute significantly to the cooling of the newly formed neutron star, and observations of supernova cooling, in particular from SN 1987A, therefore provide stringent constraints on axion-baryon couplings.

In this context, we construct an effective Lagrangian, based on symmetry principles, to systematically describe the interactions between axions and baryons. We investigate the leading axion production mechanisms in the proto-neutron-star medium, modeling baryon interactions via both spin-0 and spin-1 meson exchange; the vector-meson sector is implemented within the Hidden Local Symmetry framework, which we validate against hadron-scattering data.

Orateur: BASILE DEMAIRE-LEPAPE

13 Is the spherical profile enough for gamma-ray dark matter indirect searches?

Recent results from Galactic surveys, such as Gaia, and from hydrodynamical cold dark matter simulations of Milky Way-like galaxies have shown that the galactic dark matter halo likely deviates from spherical symmetry. Its shape and orientation may constitute an additional significant source of uncertainty for indirect dark matter searches. In this work we develop a fast and light computational tool that accommodates different analytical density profiles, triaxial halo shapes and arbitrary halo orientations, and predicts the corresponding gamma-ray flux maps as observed from Earth. We explore the parameter space of a triaxial Galactic dark matter halo with the aim of assessing which configurations are degenerate with, or clearly distinguishable from, the spherical case. The comparison is carried out at the level of the projected two-dimensional gamma-ray flux map of the inner Galactic region rather than at the level of the three-dimensional density distribution, taking into account the sensitivity of the Fermi-LAT telescope as well as the presence of Galactic diffuse emission.

Orateur: Margherita Scuderi (Laboratoire de physique théorique et hautes énergies (LPTHE), Sorbonne université)

mar. 24 novembre

Astroparticle

Président de session: Daniel Kerszberg (LPNHE, CNRS/IN2P3)

14 Session overview

Orateur: Daniel Kerszberg (LPNHE, CNRS/IN2P3)

15 Talk Astro #1

Orateur: Lukas Arda (APC Paris)

16 Talk Astro #2

Orateur: David Fernando Freitas da Silva Cavalcante (APC (Université Paris Cité))

10:20 Coffee break

Astroparticle

Président de session: Daniel Kerszberg (LPNHE, CNRS/IN2P3)

17 Talk Astro #4

Orateur: Justin Albinet

18 Talk Astro #5

Orateur: titouan girault (IRFU, CEA Paris-Saclay, Université Paris-Saclay)

19 Cherenkov background for high-mass WIMP searches with DarkSide-20k

The existence of dark matter is firmly established by astrophysical and cosmological observations, yet its particle nature remains one of the most compelling open questions in physics. Among the proposed candidates, Weakly Interacting Massive Particles (WIMPs) are particularly well motivated by the so-called “WIMP miracle”: a weakly interacting, stable particle with electroweak-scale mass naturally reproduces the observed dark matter relic density through thermal freeze-out.
The DarkSide-20k experiment, currently under construction at LNGS, is a next-generation dual-phase Time Projection Chamber containing 50 tonnes of radiopure argon. Data taking is expected to begin in 2029 and continue for a decade. The experiment aims to achieve world-leading sensitivity to both low-mass WIMPs around 1 GeV and high-mass WIMPs above few tens of GeV. For high-mass WIMPs, the detection strategy relies on measuring scintillation and ionization signals produced by particle interactions in liquid argon, enabling three-dimensional reconstruction of the interaction point and fiducialization of the active volume to suppress external backgrounds. In addition, the time profile of the scintillation signal, known as Pulse Shape Discrimination (PSD), is used to distinguish nuclear recoil signals from electron recoil backgrounds.
In this work, I present an overview of the search for high-mass WIMPs with DarkSide-20k, with particular focus on the impact of Cherenkov-induced backgrounds on PSD and their implications for the projected sensitivity of the experiment.

Orateur: Manuel Pronesti (CPPM, Aix-Marseille Université, CNRS/IN2P3)

20 Talk Astro #6

Orateur: Pierre Geneste (CEA-IRFU-DPhP)

12:35 Lunch break

Astroparticle

Président de session: Daniel Kerszberg (LPNHE, CNRS/IN2P3)

21 Talk Astro #7

Orateurs: Ugo LAINÉ (Subatech-KM3NeT), Ugo Lainé (Subatech-KM3NeT)

22 Talk Astro #3

Orateur: Mulan Ahmed (IJCLap)

Flavor Physics

Président de session: Tommaso Fulghesu (Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France)

23 Session overview

Orateur: Tommaso Fulghesu (Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France)

24 Talk Flavour #1

Orateur: Valério Di Bella (IPHC)

25 Talk Flavour #2

Orateurs: Fatemeh NOURI (IJCLab), Fatemeh Nouri (IJCLab, Paris-Saclay)

16:10 Coffee break

Neutrino physics

Président de session: Emile Lavaut (IPHC CNRS)

26 Session Overview

Orateur: Emile Lavaut (IPHC CNRS)

27 Talk Neutrino #6

Orateur: Gaby BRENOT

28 Talk Neutrino #7

Orateur: Matteo Loup (APC)

mer. 25 novembre

Neutrino physics

Président de session: Emile Lavaut (IPHC CNRS)

29 Precision Measurement of Oscillation Parameters and Determination of the Mass Order of Neutrinos in the JUNO Experiment

Neutrinos are among the most abundant particles in the Universe, yet remain some of the least understood. We discovered only recently they have mass, thanks to a phenomenon called “neutrino oscillation”. Neutrinos can exist in different states, called flavors, and each flavor is a combination of different three mass states. One open question concerns the ordering of these mass states. The Jiangmen Underground Neutrino Observatory (JUNO), a 20-kiloton liquid scintillator detector built 650 meters underground in southern China, was designed to answer this question. By detecting antineutrinos emitted by the nearby Taishan and Yangjiang nuclear power plants, JUNO measures a subtle interference pattern in their energy spectrum that encodes which mass ordering nature has chosen. After six years of data taking, three of the key parameters governing neutrino oscillations will be measured with a precision of 0.6% or better, among the most precise ever achieved in this field. This measurement is also expected to reach a significance of ~3σ for the Neutrino mass ordering (NMO).
Reaching this level of precision is as much a statistical challenge as an experimental one. In this contribution, I will present the methodology in the analysis of JUNO's data : a careful treatment of systematic uncertainties and a dedicated statistical techniques that convert the measurements into a mass-ordering significance and reliable confidence intervals.

Orateur: Mathis Roinsard (Subatech)

30 Talk Neutrino #2

Orateur: Dario Pullia (APC, CERN)

31 SPMT energy and timing calibration for CCSN neutrinos with JUNO experiment

The JUNO experiment is a 20 kton liquid scintillator detector, designed primarily to determine the neutrino mass ordering within the next few years. Its large size also makes it well suited to detect neutrinos from the next galactic core-collapse supernova (CCSN). Such an event would be a unique opportunity to understand the mechanisms behind CCSNe, which are not yet fully understood. The only time neutrinos from a CCSN have been detected was in 1987, when SN1987A exploded in the Large Magellanic Cloud: only 24 neutrinos were recorded, by three experiments, Kamiokande-II, IMB and Baksan. Despite this low number of events, the detection was a major discovery, but it was not enough to discriminate between explosion mechanism models. For a CCSN at 10 kpc, JUNO expects more than 5000 events, about 200 times more than for SN1987A, without counting the contributions of other experiments. In this context, it is essential to prepare for this moment by tuning the event selection with Monte Carlo simulations and by calibrating JUNO’s different subsystems. My thesis focuses mainly on the time and energy calibration of the Small-PMT system (SPMT) using different calibration sources, and on event selection during a nearby CCSN, taking into account effects such as event pile-up and afterpulses.

Orateur: Jonas Buchholz (Université de Bordeaux)

10:15 Coffee break

Neutrino physics

Président de session: Emile Lavaut (IPHC CNRS)

32 Talk Neutrino #4

Orateurs: Ben Carew (LPNHE), Benjamin Carew (LPNHE)

Hadronic Physics

33 Session Overview

34 Talk hadronic #1

Orateur: Emma Weiler

35 Talk hadronic #2

Orateur: Sacha MEHAT (IJCLAB)

12:30 Lunch break

36 Visite to Dinan

jeu. 26 novembre

Cosmology

Président de session: Anna Niemiec (LPSC)

37 Session Overview

Orateur: Anna Niemiec (LPSC)

38 High angular resolution Sunyaev-Zel’dovich effect observations of galaxy cluster

Galaxy cluster are the most massive gravitationally bound structures in the Universe, thus, they are of great cosmological interest. Indeed, their mass and redshift distribution can be used to constrain cosmological parameters.
In order to study clusters we can use the thermal Sunyaev-Zel'dovich (tSZ) effect that is produced by the inverse Compton interaction of CMB photons with the hot gas of the clusters and which is not affected by cosmological dimming.
The tSZ effect is directly proportional to the electron pressure integrated along the line-of-sight and along with X-ray data it allows us to study cluster thermodynamic properties. Moreover, under the hypothesis of hydrostatic equilibrium it's then possible to obtain a lower biased estimate of the total mass of the cluster and establish scaling relations.
Physical processes in individual clusters as merging events, shocks and turbulence can modify this hydrostatic bias and then limit the cosmological exploitation of the cluster sample. At this regard high resolution tSZ observations are particularly useful as they allow to characterize cluster spatial properties and morphology.
In this talk we will present 18 arcsec resolution NIKA2 tSZ observations at 150 GHz of a CHEXMATE cluster of galaxies presenting a disturbed morphology. Combining with X-ray data we will derive the main cluster thermodynamic quantities in terms of radial profiles and associate 2D residuals to physical cluster properties. We will also discuss how higher resolution tSZ observations with the NOEMA IRAM interferometer are of interest to probe the cluster inner regions down to BCG scales.

Orateur: Victor Chalamet (LPSC)

39 Talk Cosmo #4

Orateur: Théotime Hallouin (LPCA/CNRS)

10:20 Coffee break

Cosmology

Président de session: Anna Niemiec (LPSC)

40 Measuring the Expansion of the Universe with Gravitational Waves

Gravitational waves were predicted in 1916 by Albert Einstein through his theory of general relativity. A century later, on 14 September 2015, the first signal was detected by the LIGO-Virgo Collaboration through interferometric measurements of spacetime distortions produced by the coalescence of two compact objects$^{[1]}$.

This new observational window on the Universe has opened the door to a wide range of astrophysical and cosmological studies. In particular, gravitational wave signals can be used to infer cosmological parameters such as the expansion rate of the Universe – the Hubble constant $H_0$. Observations of black hole and neutron star mergers may help resolve the so-called “Hubble tension”$^{[2]}$, a persistent discrepancy between independent measurements of $H_0$ in modern cosmology.

However, this approach relies on accurately localizing the source of the signal, which remains challenging, especially for binary black hole mergers that lack electromagnetic counterparts. In this work, we present the dark siren method$^{[3]}$, a statistical framework that improves the $H_0$ estimation using compact binary coalescences by combining gravitational-wave data with galaxy catalogs.

Compact binary coalescences are particularly valuable because the luminosity distance to the source is directly encoded in the signal. The key missing parameter is the redshift of the source, which is required to infer the expansion rate. The dark siren method uses Bayesian inference with a redshift prior information extracted from galaxy catalogs considered as potential host of gravitational wave sources. This additional information contributes to overcome the intrinsic degeneracy between source masses and redshift, better constraining the values of $H_0$.

[1] LIGO Scientific Collaboration and Virgo Collaboration, GW150914: The Advanced LIGO Detectors in the Era of First Discoveries, 2016
[2] Verde, L., Treu, T. & Riess, A.G. Tensions between the early and late Universe, 2019
[3] Gray, R. et al. Joint cosmological and gravitational-wave population inference using dark sirens and galaxy catalogues, 2023.

Orateur: Maxime Bloch (Subatech (UMR 6457))

41 Talk Cosmo #5

Orateurs: Eva Elkhoury (Qubic), Eva Elkhoury (APC)

42 3x2pt Cosmology with Euclid

Galaxy clustering allows the study of galaxy distribution across the Universe, revealing critical insights into the structure of the Universe, its dynamics and the nature of dark energy. On the other hand, weak lensing enables the inference of dark matter distribution by analyzing the deformation of background galaxies by foreground masses.

The 3x2pt method, which combines galaxy clustering, cosmic shear, and galaxy-galaxy lensing, is one of the most promising approaches to leveraging these observations. This method maximizes information on cosmological parameters, particularly those related to dark energy, by using complementary measurements to reduce potential systematic biases and break degeneracies. My work aims to exploit the upcoming data from the Euclid mission to conduct an in-depth study of galaxy clustering and to perform a comprehensive 3x2pt analysis.

In this talk I will discuss the advantages of using 3x2pt cosmology, the tools needed, as well as the catalogue and data vector-level tests that I am doing for Euclid Data Release 1 (DR1).

Orateur: Urwa Shoaib

Interdisciplinary

Président de session: Rachel Delorme (LPSC, Grenoble)

43 Session Overview

Orateur: Rachel Delorme (LPSC, Grenoble)

12:35 Lunch break

44 Invited talk

Interdisciplinary

Président de session: Rachel Delorme (LPSC, Grenoble)

45 Talk Interdisciplinary #1

Orateur: Louis Hardouin

46 Talk Interdisc. #2

Orateur: Violette GUITTET

Beyond Standard Model

47 Session Overview

Orateur: Angela Burger (L2I Toulouse, CNRS/IN2P3, Université de Toulouse)

16:20 Coffee break

Beyond Standard Model

Président de session: Angela Burger (L2I Toulouse, CNRS/IN2P3, Université de Toulouse)

48 Talk BSM #2

Orateur: Melvyn Putra Wirawan

49 Talk BSM #1

Orateur: Xavier MADRE (IPHC)

50 SPELS@WISArD : Spectrum of 32P ELectron Shape at WISArD

Author: Ana¨ıs L´epine, LP2iB, on behalf of the WISArD collaboration
The Standard Model (SM) of particle physics has proven to be a successful
theory describing three of the four fundamental interactions. However, some
open questions remain and motivate precise measurements to search for evidence
of physics beyond the SM predictions. Nuclear β-decay provides a sensitive
probe of the weak interaction sector, for instance, precise measurements of the
shape of the β-energy spectrum can be used to search for exotic currents by
extracting the Fierz term bF.
To constrain possible extensions of the SM at the same level as direct searches
at high energy, the required precision on bF must be at the level of a few 10−3.
This raises several experimental challenges, in particular partial energy deposi-
tion caused by electron backscattering.
The SPELS (Spectrum of 32P ELectron Shape) project addresses this issue
by placing two detectors, facing each other, inside the magnetic field of WIS-
ArD’s superconducting magnet. This setup ensures a 4π solid angle and guides
the backscattered particles from one detector to the opposite one, thereby min-
imizing the energy loss of β particles from backscattering.
Following the first β-spectrum shape measurement at WISArD in 2020, using
scintillators and silicon photomultipliers, significant upgrades have been made.
A key improvement is the use of lithium-drifted silicon (Si(Li)) detectors, which
provide a higher energy resolution and a lower energy threshold. To cool these
detectors down, a new cooling system, based on active glycol circulation and
Peltier elements has been developed in Leuven. The setup has been optimized
at LP2iB in Bordeaux and a first successful commissioning run was conducted in
February 2026 at ISOLDE with an 114In source. The final data-taking campaign
was in July, with measurements of the β-shapes of 32P and 114In, two isotopes
with long lifetimes and endpoint energies in the 1-3 MeV range, where sensitivity
to the Fierz term is optimal. The analysis is currently ongoing, and preliminary
results will be presented.

Orateur: Anaïs LEPINE

ven. 27 novembre

10:15 Coffee break

Instrumentation

Président de session: Marion Missio (Université Clermont Auvergne)

51 Session Overview

Orateur: Marion Missio (Université Clermont Auvergne)

52 Talk Instru #1

Orateur: Augustin DEMAGNY

53 Analysis of HGCAL timing performance in the 2025-2026 testbeam campaign at CERN

The High-Luminosity phase of the Large Hadron Collider (HL-LHC), is expected to start in 2030. It will bring around a 2.5-to-4-fold increase in instantaneous luminosity, raising pileup up to 200 collisions per bunch crossing and increasing radiation damage to the detectors. To cope with this pileup and replace aging components, several subdetectors of the major experiments must be upgraded ahead of the HL phase.

In CMS, the endcap calorimeters will be replaced by the High-Granularity Calorimeter (HGCAL), a 47-layer silicon and scintillator detector combining electromagnetic and hadronic sections in a single structure. It will provide precise position, time and energy measurements, targeting a time resolution under 30 ps at cluster level to enable accurate event reconstruction despite the increased pileup.

Several testbeam campaigns have been carried out at CERN over the past years to prepare HGCAL's commissioning. We present a summary of the timing performance analysis from the 2025-2026 campaign: after a broad introduction to HGCAL and the testbeams, we will focus on the timing studies and their results, including the use of Micro-Channel Plate detectors as time reference.

Orateur: Ewan Heeder (CEA Paris-Saclay)

54 Talk Instru #6

Orateur: Mariya Mollova (APC-Paris)

12:30 Lunch break

Instrumentation

Président de session: Marion Missio (Université Clermont Auvergne)

55 Performance Studies and Optimization of the Backward Electromagnetic Calorimeter for the ePIC Detector at the Electron–Ion Collider

The Relativistic Heavy Ion Collider (RHIC) will be revamped as the Electron-Ion Collider (EIC), and the STAR detector will be replaced by the ePIC detector. We are developing backward electromagnetic calorimeters (ECal) to meet the energy-resolution requirements listed in the EIC Yellow Report. The energy resolution of the backward ECal prototype was measured during a beam test at the Deutsches Elektronen-Synchrotron (DESY), which met the EIC requirements for electron beam energies below 6 GeV. This study will present the progress of backward ECal prototype measurements.

Orateur: Chun-Ting Kuan

56 Talk Instru #4

Orateur: Veronica CAZZOLA (LPNHE)

57 Talk Instru #5

Orateur: Amélie CLÉMENT (LP2IB)

58 Talk Instru #3

Orateur: Anas Basheer (anas.basheer@univ-lille.fr)

16:10 Coffee break