Dixième Assemblée Générale du GdR Ondes Gravitationnelles

5 oct. 2026, 10:00 → 6 oct. 2026, 23:00 Europe/Paris

 

(English version below)

Le GdR Ondes Gravitationnelles (http://gdrgw.in2p3.fr/) a été créé en 2017 avec le but de rassembler la communauté scientifique intéressée par l’exploration de l’Univers avec les ondes gravitationnelles, et de lui fournir des occasions de rencontres et de discussions communes. 

La dixième assemblée générale du GdR Ondes Gravitationnelles se tiendra en présentiel à l'Institut de Physique des Deux Infinis de Lyon (IP2I). Elle couvrira les thèmes d’intérêt du GdR, représentés par ses Groupes de Travail.

L’événement s’étendra sur deux journées, les 5 et 6 octobre, avec une alternance de présentations scientifiques et de discussions. Le 5 octobre au soir, une session posters sera organisée, accompagnée d’un cocktail convivial. 

L'inscription à cette réunion est obligatoire avant le 5 septembre 2026. Il faut, au préalable, devenir membre du GdR en s'inscrivant sur le site http://gdrgw.in2p3.fr/ si vous ne l'êtes pas déjà.

La date limite pour envoyer une contribution est le 5 septembre 2026.

Veuillez noter que plusieurs groupes de travail organiseront des réunions satellites le 7 octobre dans les mêmes locaux à l'IP2I Lyon. L'inscription à ces réunions doit se faire séparément via les agendas dédiés (voir ici pour plus d'informations). 

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The GdR Gravitational Waves (http://gdrgw.in2p3.fr/) was established in 2017 to bring together the scientific community interested in exploring the Universe through gravitational waves and to provide opportunities for shared meetings and discussions.

The tenth general assembly of the GdR Gravitational Waves will be held in person at the Institute of Physics of the Two Infinities in Lyon (IP2I). It will cover the GdR's areas of interest, as represented by its Working Groups.

The event will span two days, October 5th and 6th, featuring a mix of scientific presentations and discussions. On the evening of October 5th, a poster session will be held, during a networking cocktail.

Registration for this meeting is mandatory by September 5, 2026. You must first become a member of the GdR by registering on the website http://gdrgw.in2p3.fr/ if you are not already.
The deadline for submitting a contribution is also September 5, 2026.

Please note that several working groups will organise satellite meetings on October 7th in the same venue at IP2I Lyon. Registration for these meetings has to be done separately on the dedicated agendas (see here for more information). 

 

          
    

 

 

 

lun. 5 octobre

Breaks: Café et accueil

General: Intro talks and discussion

Working groups sessions: Prédictions et suivi des signaux multi-messagers

Présidents de session: Floriane Cangemi (UPC/APC), Dr Marion Pillas (IAP), Olivier GODET (IRAP)

1 Constraining the search for gravitational waves from binary neutron star mergers with kilonovae observations

The joint observation of gravitational waves (GWs) from a binary neutron star (BNS) merger (GW170817), together with a short Gamma-Ray Burst (GRB 170817A) and a kilonova (AT2017gfo), marked the birth of multimessenger astronomy with GWs, and clearly demonstrated the huge informative power of multimessenger observations. In the future more BNS merger and kilonova detections are expected, thanks to the increasing sensitivity of GW detectors and the advent of new electromagnetic facilities such as the Vera C. Rubin Observatory. However, the association between a BNS merger and a kilonova might not be trivial: the detection of a kilonova might not coincide with the onset of the EM emission, making it difficult to clearly define a temporal window to assess the coincidence with a GW event. In this talk, we investigate the possibility to constrain the BNS merger time from kilonova light curves, taking into account different observing conditions and with focus on the Vera C. Rubin Observatory. We used different kilonova models and different inference frameworks to simulate and fit kilonova light curves. We explored different possible cadence and different wavelength coverage for observations, to investigate how the different observing conditions can affect the capability to recover the BNS merger time. The tests performed also include real data related to AT2017gfo, plus four GRBs that have been associated to possible kilonova candidates.
Finally, we present the implementation of a targeted search looking for GW candidates in coincidence with kilonovae that will be seen by Vera Rubin. We present the results applied on GW170817 - AT2017gfo using the estimation of the merger time and the binary masses inferred from the kilonova lightcurve to constrain the GW search parameter space.

Orateur: Noah Jamsin (IJCLAB and IAP)

2 Search for joint sources of neutrinos and gravitational waves with ANTARES and KM3NeT

Astrophysical neutrinos are expected to be produced during transient phenomena that also produce gravitational waves, such as compact binary coalescences, in particular those involving neutron stars, or core-collapse supernovae. Gravitational waves are routinely detected by the LIGO-Virgo-KAGRA interferometers, while the ANTARES and KM3NeT deep-sea neutrino telescopes are sensitive to neutrino interactions in a wide range of energies, from MeV to PeV. The contribution reviews recent searches for common sources of neutrinos and gravitational waves using ANTARES and KM3NeT data during the third observing run, as well as current studies with the fourth observing run and prospects. It will cover both studies, including significant gravitational wave events and those using subthreshold triggers. The observations are then converted to various constraints on the population of common sources (neutrino luminosity, rate density).

Orateur: Mathieu Lamoureux (APC)

3 Memory effect from neutron star merger counterparts

The gravitational-wave (GW) memory effect is a prediction of general relativity, characterized by a permanent change in spacetime geometry. Although it has not yet been observed, next-generation detectors such as the Einstein Telescope (ET) and the Laser Interferometer Space Antenna (LISA) are expected to provide the sensitivity required for its first detection. GW memory comprises two distinct contributions: the nonlinear memory, generated by the self-interaction of GWs, and the linear memory, originating from the anisotropic emission of matter and radiation associated with astrophysical transients. In this talk, I will show how we quantify both nonlinear and linear memory contributions produced during binary neutron star mergers, including those from GWs, gamma-ray bursts (GRB) prompt and afterglow emissions, neutrinos, dynamical and disk-wind ejecta, and kilonova emission; and I will discuss their detectability with ET and LISA through two specific applications. First, I will focus on the multi-messenger event GW170817-GRB 170817A-AT2017gfo. Secondly, I will present our assessment of GRB memory across a synthetic population, showing that only extreme-energy and favorably oriented configurations could produce a detectable signal.

Orateur: Thomas Brabant (University of Liege)

Talks invités: Multi-Messenger Astronomy in the Era of Gravitational Waves

Présidents de session: Susanna Diana VERGANI (CNRS-Observatoire de Paris), Viola Sordini (IP2I Lyon)

Breaks: Repas de midi

Working groups sessions: Tests de la relativité générale et théories alternatives

Présidents de session: Eugeny BABICHEV (IJCLab), karim Noui (IJCLab, Paris Saclay University)

4 Catching non-linear memory effect with LISA & PTA

The gravitational memory effect is an unobserved prediction of general relativity, which states that gravitational waves can leave a permanent strain in spacetime. We investigated the prospects for detecting this memory effect with LISA from a massive black hole binary merger. Using Bayesian analysis, we assessed the conditions under which the memory signal can be confidently identified in LISA data. We were able to highlight a region of the source parameter space in which memory detection is likely, and compared these results with simulated populations of MBHBs to estimate the number of memory events LISA may see during its lifetime. Our analysis shows that LISA can detect the memory effect and constrain its amplitude, providing a probe for fundamental physics. Meanwhile, work has been carried out to search for memory imprints in PTA data. With the upcoming EPTA and IPTA-DR3, we are preparing to search for memory in these new data.

Orateur: Adrien Cogez (CEA/IRFU/DPhP)

5 New Aspects of spontaneous scalarization of black holes beyond General relativity

Spontaneous scalarization is a mechanism that allows black holes to develop a non-trivial profile of a scalar field “scalar hair” because of tachyonic instabilities, enabling tests of gravity beyond General Relativity. Motivated by stability and threshold issues in Gauss-Bonnet scalarization, we propose a new model characterized by two nonminimal couplings of the scalar field to both Gauss-Bonnet curvature and a U(1) gauge field (e.g. electromagnetic field). The presence of two distinct sources of tachyonic instability broadens the conditions for spontaneous scalarization. We track how the electric charge and the coupling constants govern the onset of the scalar field and derive new solution branches with nontrivial scalar profiles. Numerical integration shows multiple coexisting scalarized black hole solutions with adjustable thresholds, influenced by the relative strengths of curvature and matter couplings. We examine their scalar charge, horizon properties, and thermodynamic characteristics, demonstrating how the model can selectively activate or suppress scalarization phenomena. The matter source term modifies the scalarization onset and promotes stable solutions, as indicated by the evolution of the scalar charge and horizon quantities. These findings suggest an alternative approach to scalarization, may avoid the instabilities of curvature-only or matter-only models, and offer new ways to test strong-gravity effects in upcoming observations.

Orateur: ZAKARIA BELKHADRIA (IP2I, Université Claude Bernard Lyon 1)

6 Radial Perturbations of Black Holes in DHOST Theories

We study the gravitational waves of exotic Black Holes in modified theories of gravity (scalar tensor theories). We show that, in contrast with GR where radial perturbations are absent as a consequence of Birkhoff’s theorem, radial perturbations propagate a degree of freedom (DOF). This DOF combines both scalar and metric perturbations. We describe its propagation under the form of a Schrodinger equation in a new time and radial coordinates. We discuss the stability of the perturbations and show that this perturbation exhibits new features that should single out this signal experimentally.

Orateur: Simon Iteanu (IJClab)

Working groups sessions: Étoiles à neutrons, supernovae et synthèse des éléments lourds

Présidents de session: Anthea FANTINA (GANIL ({CNRS}UPR3266)), Matteo Bugli (UniTo - CEA Saclay), Sebastien Guillot (IRAP)

7 Discussion du GT - Étoiles à neutrons, supernovae et synthèse des éléments lourds

Orateurs: Anthea FANTINA (GANIL ({CNRS}UPR3266)), Matteo Bugli (UniTo - CEA Saclay), Sebastien Guillot (IRAP)

8 Impact of the equation of state on the evolution of rapidly rotating core-collapse supernovae

The evolution of core-collapse supernovae (CCSNe) involves the formation and evolution of a proto-neutron star (PNS), whose structure and dynamics are strongly governed by the nuclear equation of state (EOS). In rapidly rotating CCSNe, the EOS plays a key role in setting the conditions for the onset and evolution of non-axisymmetric instabilities.

We present three-dimensional neutrino-magnetohydrodynamic simulations of the collapse of a rapidly rotating, weakly magnetised massive-star progenitor, using different finite-temperature nuclear EOSs. Despite the different EOS prescriptions, all models develop two distinct phases of non-axisymmetric corotation instabilities during the post-bounce evolution, indicating that their development is a robust feature of rapidly rotating CCSNe. However, their onset, dominant azimuthal modes, duration, and characteristic frequencies vary significantly with the EOS. These differences arise from the EOS-dependent evolution of the PNS structure, compactness, and rotation profile, which determine the conditions under which the instabilities develop and evolve.

We find that the characteristic frequencies of the instabilities correlate with the PNS compactness and tidal deformability, providing a direct link between the properties of dense nuclear matter and the dynamical behaviour of the newly formed compact object. The associated large-scale spiral modes also leave characteristic imprints on the gravitational-wave and neutrino signals. Overall, our results highlight the important role of the nuclear EOS in shaping the development and evolution of rotational instabilities in rapidly rotating CCSNe.

Orateur: Dr Marco Cusinato (CEA-Saclay)

Breaks: Pause café

Talks invités: Probing nuclear physics with gravitational waves

Président de session: Lami Suleiman (Deutsches Elektronen Synchrotron)

Working groups sessions: Formes d'onde

Présidents de session: Alexandre Le Tiec (Observatoire de Paris), Eric Gourgoulhon (LUTH, Observatoire de Paris), Guillaume Faye (Institut d'Astrophysique de Paris)

9 Logarithmic divergence of the fluxes at the light ring for unstable circular orbits

At first self-force order, we consider the energy flux emitted by a particle orbiting a Schwarzschild black hole on an unstable circular orbit just outside the light ring. Both the flux to infinity and the flux down the horizon diverge as the orbit approaches the light ring, growing like the inverse of the distance to it, times a logarithm of that distance. This logarithmic divergence arises from an infinite sum over $m$-modes and is therefore out of reach of numerical methods. We determine the coefficient of the logarithmic divergence analytically using WKB methods; it is universal, i.e., the same for both fluxes. We then obtain the remaining coefficients (one for each flux) by a combination of numerical and analytical methods. We expect these results to be useful, e.g., to inform resummations and study ultrarelativistic scattering. They highlight the potential of analytical methods to address problems in self-force in regions of parameter space where traditional numerical methods fail.

Orateur: David Trestini (University of Southampton)

10 Radiation reaction in massless scalar-tensor theories to third post-Newtonian order

With the advent of third-generation gravitational-wave detectors, it has become crucial to extend analytical frameworks used to model waveforms from compact binary systems to alternative theories of gravity. In this talk, I will present recent results on radiation-reaction effects in a large class of scalar–tensor theories. Using the post-Newtonian multipolar post-Minkowskian (PN–MPM) formalism, we compute the dissipative contributions to the ten binding quantities, which can be classified into two types: Schott and pseudo-Schott terms. In contrast to general relativity, where only pseudo-Schott terms contribute to the waveform phasing at 4.5PN order for quasi-circular orbits, we find that Schott terms begin to contribute already at 3PN order, even in the quasi-circular case. These contributions must therefore be consistently included in the future when extending the energy flux and waveform, currently known up to 2.5PN order, to 3PN order.

Orateur: Eve Dones (IBS CTPU-CGA)

11 Next-to-next-to-leading gravitational radiation-reaction corrections to quasi-elliptic and quasi-hyperbolic compact binary orbits

Compact binaries are the primary sources of gravitational waves, and an accurate description of their dynamics is essential for constructing waveform templates for future gravitational-wave detectors. Recently, the gravitational radiation-reaction force for non-spinning compact binaries on generic orbits has been derived in harmonic coordinates at the fourth-and-a-half post-Newtonian (4.5PN) order of general relativity.
Using this result, together with the Keplerian parametrization of the motion and Lagrange's method of variation of constants, I will present the computation of the corresponding radiation-reaction corrections to eccentric quasi-elliptic and quasi-hyperbolic orbits of two compact bodies at 4.5PN order.
This requires consistently incorporating the nonlocal-in-time tail contributions arising at 4PN order, together with the gravitational-wave recoil in the center-of-mass frame at 4.5PN order. I will also discuss how the results for bound and unbound orbits are explicitly related through analytic continuation.

Orateur: Emeric Seraille (LPENS)

12 Charges aspects of BMS symmetries as opposed to a stress-energy tensor

The BMS group is the symmetry group at infinity of asymptotically flat spacetimes. In the presence of gravitationnal radiation, the associated Noether currents at null infinity are linked through flux-balance laws to variations of global quantities of the system, such as energy and angular momentum. I will present how, using the Noether currents fixed through a specific Wald-Zoupas prescription, which already enabled the obtention of background independent BMS charges, the charge integrands were obtained. Being obtained as 2-forms, those integrands, referred to as charge aspects, enable integration of the charges over a generic cross-section of null infinity, and not simply one at a constant retarded-time coordinate. I will then show why the shape of those aspects, which correspond to charge densities, suggest that the notion of a stress-energy tensor at infinity is not appropriate. Finally I will discuss the background dependence of the aspects, and notably the central extension that they exhibit.

Orateur: Pierre Piovesan (CPT, Aix-Marseille Université)

Talks invités: Talk Invité

Président de session: Sylvain MARSAT (Laboratoire des deux Infinis – Toulouse(L2IT))

General: Environnement transversal group

Président de session: Matteo Barsuglia

Poster session: Poster session and cocktail

mar. 6 octobre

Working groups sessions: Développement des détecteurs

Présidents de session: Angélique Lartaux (IJCLab), Eleonora POLINI (CNRS / OCA / ARTEMIS), Michal Was (LAPP/CNRS)

13 Probing gravitational waves using the orbital dynamics of binary systems

The internal dynamics of a binary system can be affected by the passage of gravitational waves (GWs). This effect is significantly enhanced when the GW frequency is in resonance with the orbital frequency of the binary system. Recently, this phenomenon has been proposed as a novel approach to detecting GWs in the largely unexplored microhertz frequency band, using precise measurements of the orbital dynamics of the Moon and artificial satellites.

In this contribution, we will discuss the signatures induced by GWs in the orbital dynamics of a binary system, with particular emphasis on the resonant case. We will then show how these signatures could be detected through laser ranging measurements of the Moon and artificial satellites. We will present sensitivity estimates for such measurements and briefly discuss the concept of the GUEST space mission, recently submitted to the ESA F-3 call.

Orateur: Aurelien Hees (LTE - Observatoire de Paris)

14 A landscape of possible higher-resolution mHz gravitational-wave missions

As we prepare for LISA to open observations in the mHz gravitational wave observational band in the next decade, it is also time to begin considering what could come next? One goal for a future mHz-band observatory, or a network of observatories, would be to enhance the ability to localize sources. We discuss possible design strategies for architectures of future LISA-like missions to improve sky-localization, their relative capabilities for localizing mHz-band sources, and potential science opportunities for such missions.

Orateur: John Baker (L2I Toulouse, CNRS/IN2P3, Université de Toulouse)

General: Presentations of other GdR efforts and discussion on possible joint activities (GdR DI2I)

Présidents de session: Giulia HULL (Université Paris-Saclay, CNRS/IN2P3, IJCLab), Viola Sordini (IP2I Lyon)

Talks invités: Current status and future perspectives of Virgo in the worldwide GW network

Président de session: Loïc Rolland (CNRS/LAPP)

Breaks: Pause café

Working groups sessions: Méthodes d'analyse des données

Présidents de session: Alba ROMERO RODRIGUEZ (Laboratoire D'Annecy de Physique de Particules (LAPP)), Florian Aubin (IPHC), Yves Lemiere (LPCCaen, ENSICAEN, Unuiversité de Caen, CNRS/IN2P3, Caen, France)

15 Les défis pour LVK et ET

Orateur: Dr Tania Regimbau ({CNRS}UMR5814)

16 Les défis pour LISA et PTA

Orateur: Stanislav BABAK (APC)

17 Separating the GW background components with LISA through anisotropies and time-frequency techniques

LISA will observe a superposition of astrophysical and cosmological stochastic backgrounds, whose disentanglement represents a major challenge for the data analysis. The talk is meant to give an overview on the ongoing research of GW background searches with LISA, and on how anisotropies can help in that direction. I then discuss what angular information adds to component separation, including the annual modulation of the Galactic foreground, the kinematic dipole, and cross-correlation with galaxy catalogues. In the end I will show why time-frequency techniques turn out to be promising in analyzing such non-stationary backgrounds.

Orateur: Giorgio Mentasti (APC Paris)

18 Tfwaves: a time-frequency approach to long-lived LISA signals — from EMRIs to stellar-mass black hole binaries

We present tfwaves, a Python package that represents long-lived gravitational-wave signals directly in the time-frequency domain. From the amplitude and phase of a time-domain waveform, it computes an analytical approximation of the Short-Time Fourier Transform, together with an approximate LISA response. The resulting representation is sparse: each harmonic occupies only a few frequency bins per time segment. Two consequences follow. First, non-stationarity is taken into account naturally, since the noise is described locally in each time-frequency pixel rather than by a single stationary spectrum over the whole observation. Second, the likelihood becomes cheap enough that parameter estimation with MCMC methods is practical for signals that stay in the LISA band for months to years, such as those from extreme mass-ratio inspirals (EMRIs) and stellar-mass black hole binaries.
We focus on the EMRI case. The analytical time-frequency waveform and response reproduce the numerically computed STFT of FEW waveforms passed through the full LISA response, with overlaps greater than 95% for the EMRI sources of the Mojito Lite simulated dataset, and its accuracy depends on the time-frequency resolution and on the set of retained harmonics, together with injection-recovery MCMC results on those sources. Results obtained from the frequency-domain framework of the package for stellar-mass black hole binaries will be shown briefly for comparison.

Orateur: Saptarshi GHOSH (Astroparticule et Cosmologie, Université Paris Cité)

Breaks: Repas de midi

General: Table ronde (precision era et effets systématiques)

Working groups sessions: Cosmologie et Population des sources

Présidents de session: Astrid Lamberts (Observatoire de la Côte d'Azur), Aurélien Chalumeau (LPC2E/OSUC), Giulia Cusin (IAP), Irina Dvorkin (Institut d'Astrophysique de Paris), Michele Mancarella (Aix-Marseille Université), Tania Regimbau (LAPP)

19 A weakly modelled view of the joint compact-binary mass plane: population structure and spectral-siren cosmology

In this contribution, I will present a novel approach for reconstructing the compact-binary mass spectrum and exploiting its population features for gravitational-wave cosmology. We infer the population in the joint source-frame component-mass plane using a flexible mixture model, and introduce a model-independent procedure to identify structures directly from the reconstructed density and quantify their robustness and prominence.
Applied to GWTC-5, the joint reconstruction clarifies the morphology of several familiar mass-spectrum features. In particular, the structure near $\sim35 M_\odot$ is a stable near-equal-mass peak whose projection can appear ambiguously as a peak or shoulder, clarifying differing one-dimensional interpretations. We also find tentative evidence for a weaker unequal-mass feature near $(21,12),M_\odot$. Using the joint component-mass distribution improves the $H_0$ constraint by $33%$ compared with a flexible one-dimensional analysis. While the $\sim10M_\odot$ and $\sim35M_\odot$ features constrain $H_0$ primarily through coherent mass scales, the intermediate unequal-mass structure carries additional information through its intrinsically two-dimensional geometry.
These results highlight the joint mass plane as a useful space both for characterizing compact-binary population structure and for identifying the features that drive spectral-siren cosmology.

Orateur: Viola De Renzis (University of Milano-Bicocca)

20 Probing Cosmology with Gravitational-Wave Dark Sirens using Euclid Galaxy Catalogs

We investigate the use of Euclid galaxy catalogs for gravitational-wave dark-siren cosmology using the GWTC-5 sample. We develop a framework to characterize the Euclid galaxy population, including photometric selection effects, catalog completeness, and the galaxy luminosity function through empirical Schechter fits. These ingredients are used to construct line-of-sight galaxy redshift priors and perform cosmological inference with the icarogw framework. We apply the analysis to the Euclid Q1 (public) and TR1 (internal) releases, testing different catalog selections and systematic effects. This work establishes the framework for future analyses with Euclid DR1 and its larger sky coverage to improve dark-siren cosmology.

Orateur: Sarah Ferraiuolo (CPPM at Aix-Marseille University (AMU) & Università di Roma, La Sapienza)

21 Latest LIGO-Virgo-KAGRA cosmological results from the Gravitational Wave Transient Catalogue 5.0.

Authors

Maxime Bloch bloch@subatech.in2p3.fr (Subatech (UMR 6457)) for the LVK Collaboration

Abstract

This work presents the gravitational-wave (GW) measurement of the Hubble constant (H0) using the detections from the fifth observing GW Transient Catalog (GWTC-5.0) of the LIGO-Virgo-KAGRA Collaboration (LVK). Using the combined information from the luminosity distance of the sources and their redshifts - inferred either from mass spectrum constraints or from statistical host galaxy correspondence - we draw information on the cosmological parameters. We estimate $H_0=71.7^{+9.4}_{−7.5}$ $km s^{−1} Mpc^{−1}$ (68% credible symmetric interval) using the Dark Sirens statistical framework on 236 GW signals as well as the bright siren GW170817 resulting from a binary neutron-star system coalescence with an observed electro-magnetic counterpart. The precision shows a 22.0% improvement compared to the GWTC-4.0 catalog, thanks to the inclusion of more GW sources and additional constraints using new mass models covering the full range of compact objects. We challenged modified-gravity models against the GW event dataset. No significant deviation from General Relativity was observed.

Orateur: Maxime Bloch (Subatech (UMR 6457))

22 Dark Sirens as Probes of Compact-Binary Host Galaxies

Gravitational-wave (GW) dark sirens statistically associate GW luminosity-distance measurements with galaxies consistent with the source localization. This association contains astrophysical information about how compact binaries populate galaxies and the likely hosts of individual events. To date, however, dark-siren analyses have focused primarily on cosmology, fixing the galaxy–merger relation and marginalizing over host identity. In this talk, I will instead discuss how dark-siren observations can be used as an astrophysical probe, and present an inference framework that jointly constrains the galaxy dependence of merger rates and yields the host probabilities of individual events. The framework provides a criterion for reducing the potential hosts of a well-localized, electromagnetically dark, event to a compact target list for electromagnetic follow-up, accounting for catalog incompleteness and galaxy-dependent merger probabilities. Applied blindly to GW170817, the method recovers NGC4993 as the highest-ranked host and constrains the galaxy luminosity weighting, with a mild preference for non-uniform host weights. These results illustrate how dark-siren analyses can provide information about the astrophysics of compact-binary mergers that lack an identified electromagnetic counterpart. Self-calibration of the galaxy-weighting prescription may also help reduce a potential source of systematic uncertainty in cosmological inference.

Orateur: Michele Mancarella (Aix-Marseille Université)

General: Presentations of other GdR efforts and discussion on possible joint activities (GdR CoPhy)

Présidents de session: Dr Josquin Errard (APC / CNRS), Viola Sordini (IP2I Lyon)

Fin de l'Assemblée Générale: Pause

Working groups meetings: Discussion jointe des groupes de travail développement des détecteurs et méthodes d'analyse des données

Présidents de session: Alba ROMERO RODRIGUEZ (Laboratoire D'Annecy de Physique de Particules (LAPP)), Angélique Lartaux (IJCLab), Eleonora POLINI (CNRS / OCA / ARTEMIS), Florian Aubin (IPHC), Michal Was (LAPP/CNRS), Yves Lemiere (LPCCaen, ENSICAEN, Unuiversité de Caen, CNRS/IN2P3, Caen, France)