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07/10/2026, 13:00
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07/10/2026, 13:30
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Artem Basalaev (AEI), Artem Basalaev (AEI Hannover)07/10/2026, 14:00
Future ground-based gravitational wave detectors, such as the Einstein Telescope and the Cosmic Explorer, will reveal the universe in gravitational waves throughout cosmic history. However, their realisation presents a set of unprecedented challenges. In this talk, I will focus on low-frequency gravitational waves, from a few Hz to a couple of dozen Hz. I will discuss the unique discovery...
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07/10/2026, 15:30
General overview of news in Ligo-Virgo-KAGRA Collaboration
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07/10/2026, 16:00
General overview of nieuws in LISA.
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07/10/2026, 16:30
General news from the Einstein Telescope collaboration
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Thibeau Wouters (Utrecht University/Nikhef)07/10/2026, 17:00
Future gravitational wave observatories, such as the Einstein Telescope, will detect thousands of mergers between compact objects annually. By detecting the effects of tidal deformation in binary neutron star mergers, these detectors will be the dominant way to study the equation of state of ultradense nuclear matter in the coming decades. However, this requires a scalable Bayesian...
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Martin Gerini07/10/2026, 17:20
Third-Generation (3G) observatories will observe Binary Neutron Star coalescences for hours before merger. Over these extended windows, Earth's motion induces signal modulations that render standard approaches computationally prohibitive for low-latency searches. To overcome this, we propose a 2D Convolutional Neural Network (CNN) processing multi-detector, complex Short Fourier Transform...
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Leonardo Ricca (CP3)07/10/2026, 17:40
We present a method to search for coincident gravitational-wave and high-energy neutrino emissions from binary black holes (BBHs) embedded in the accretion disks of active galactic nuclei (AGNs). Such environments are promising sites for multimessenger emission from BBHs, as the surrounding matter and radiation fields can enable electromagnetic and neutrino emission in addition to GWs....
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Luca D'Onofrio08/10/2026, 09:00
The low-frequency sensitivity of the Einstein Telescope depends on the seismic environment of its site, both through the mechanical coupling of ground motion to the test masses and through Newtonian noise.
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We present the first results of the seismic characterization of the Euregio Meuse-Rhine candidate site based on a network of recently instrumented boreholes covering the first seven months... -
Brieux Thibaut (Uliege)08/10/2026, 09:20
Seismic noise remains one of the principal challenges to extending the detection bandwidth of gravitational-wave detectors toward lower frequencies. As the Einstein Telescope aims to achieve unprecedented low-frequency sensitivity, the seismic isolation of its test masses must be significantly improved.
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A major difficulty in active isolation at very low frequencies arises from the strong... -
Morgane Zeoli (Université de Liège)08/10/2026, 09:40
Technology validation for the ET-LF must be conducted in an extremely low-vibration, cryogenic environment to simulate adequate operational conditions. This harsh environment calls for a highly sensitive, cryogenic-compatible inertial sensor for vibration monitoring and reduction in the test facilities. To that end, cryogenic, vacuum-compatible, horizontal and vertical inertial sensors with a...
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Ricardo Cabrita08/10/2026, 10:00
Detector upgrades typically include increasing circulating power in the interferometer. In particular, next-generation detectors plan to have circulating powers in the MW range. Meanwhile, current detectors have achieved a few hundreds of kWs of circulating power, well below the intended design values. High power operation comes with a particular set of challenges, due to optical absorption at...
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Francesco De Marco (Ghent University)08/10/2026, 10:50
Gravitational-wave detectors require a purely Gaussian beam in output, which ensures a smooth distribution of the optical power across the transversal plane, and the lowest angular divergence. For this reason, an Output Mode Cleaner (OMC) optical cavity is placed before the detection photodiode, to filter out the control sidebands created with phase modulation, and spurious higher-order modes...
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Daniela Pascucci (Ghent University)08/10/2026, 11:10
The Virgo gravitational-wave detector is calibrated using two independent methods: the Photon Calibrator (PCal) and Newtonian Calibrator (NCal), that can validate h(t) with an accuracy of ~1% up to 2 kHz. A new independent technique that uses scattered light as a signal for the detector calibration was recently proposed and it is planned to be installed in Virgo for its fifth observing...
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Swapnil Dhage (UCLouvain)08/10/2026, 11:30
The proposed Einstein Telescope (ET), a third generational European gravitational-wave (GW) detector, plans to extend the frequency band below 10 Hz and achieve a broadband sensitivity improvement by at least an order of magnitude over current ground-based detectors such LIGO, Virgo and KAGRA. ET will have 10 km underground interferometers in a triangular configuration with each arm consisting...
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Charlotte Bragard (UCLouvain)08/10/2026, 11:50
Inertial sensors are essential tools for gravitational-wave detectors.
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These detectors typically rely on Fabry-Pérot cavities that are actively stabilized to minimize mechanical noises in the frequency range of interest.
This stabilization demands precise monitoring of the mirrors motion using displacement sensors.
Various techniques have been developed for such inertial sensing,... -
Jue Zhang08/10/2026, 12:10
The current performance of the Virgo Gravitational Wave Detector is limited by an excess noise source, caused by marginally resonant higher order modes in the recycling cavity. Virgo is proposing a substantial update, to shift to a “stable cavity” geometry. This would suppress higher order modes in the recycling cavity. However, the design introduces new challenges with Astigmatism associated...
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Loïc Honet (Université libre de Bruxelles)08/10/2026, 14:00
With the upcoming third-generation gravitational-wave detectors comes the need to build complete, faithful, and fast waveform models for asymmetric-mass-ratio compact binaries. Most efforts within the self-force community have focused on modeling these binaries’ inspiral regime, but for ground-based detectors the final merger can represent the dominant part of the signal. In the multiscale...
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Guillaume Lhost (University of Mons)08/10/2026, 14:20
In the small mass ratio limit, eccentric binary systems can be modelled up to the separatrix crossing within the self-force framework by using first principles. At this stage, the timescale of the dynamics changes, and the prescription of post-adiabatic expansion ceases to be applicable. In the quasi-circular case, the development of a transition-to-plunge model, together with a post-geodesic...
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Stef Husken08/10/2026, 14:40
We present a practical algorithm for the numerical spatial projection of Kerr quasi-normal mode excitations from numerical data. We study criteria for quasinormal mode completeness. We conclude by discussing prospective applications to linear and generically nonlinear evolutions of perturbed Kerr black holes.
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Ethan Carlier (Université Libre de Bruxelles)08/10/2026, 15:00
The observation of the gravitational-wave signal GW170817 from a binary neutron-star merger marked the beginning of a new era in astrophysics. Such events offer unique opportunities to probe the properties of matter under conditions so extreme that they cannot be reproduced in terrestrial laboratories. During the inspiral phase, neutron stars undergo slight deformations induced by the tidal...
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Thomas Brabant (Université de Liège)08/10/2026, 15:20
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...
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Bert Depoorter (KU Leuven - Royal Observatory of Belgium)08/10/2026, 16:10
Extreme mass-ratio inspirals (EMRIs), the inspiral of a stellar-mass compact object into a supermassive black hole, are one of the primary targets for LISA. They are long-duration, multi-harmonic signals that capture the complicated two-body dynamics of the system, which is exactly what makes them such precise probes of the source parameters. Detecting them in realistic LISA data is a...
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Valeriya Korol (SRON Space Research Organisation Netherlands)08/10/2026, 16:30
The Laser Interferometer Space Antenna (LISA) will open the millihertz gravitational-wave window and provide a new way to survey the fossil stellar population of our Galaxy through compact binaries composed of white dwarfs, neutron stars, and black holes. This offers enormous potential for population studies, Galactic astrophysics, and multi-messenger astronomy with LISA. However, once a...
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Vincent Ernst08/10/2026, 16:50
Short-period white dwarf (WD) binaries are prime targets for LISA, where both gravitational-wave (GW) emission and dynamical tides drive the spin-orbital evolution. Previous treatments of resonance locking — in which the tidal torque and GW-driven decay evolve in concert to hold the forcing frequency constant — rely on a quasi-adiabatic description in which the tidal torque is dissipative by...
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Mick Wright (Utrecht University)08/10/2026, 17:10
Just like light, gravitational waves may be gravitationally lensed by massive objects along their travel path, however, this has not been observed so far. GW231123 is the most massive binary black-hole merger observed to-date, and standard analyses infer uncommon source properties that are unusually sensitive to the waveform model used. Here we investigate whether gravitational lensing can...
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Disha Hegde (UCLouvain)08/10/2026, 17:30
The exceptional gravitational-wave event GW231123 exhibited unusually high total mass and near-extremal spins, while revealing strong waveform-dependent variations in its inferred source properties. Several follow-up studies favored a lensed interpretation, with reduced waveform systematics,raising whether apparent lensing evidence could arise from waveform modeling systematics. Using...
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Jef Heynen (UC Louvain)08/10/2026, 17:50
As the rate of gravitational wave detections continues to grow, the probability of observing a gravitationally lensed gravitational wave also increases. When the Schwarzschild radius of the lens is comparable in size to the gravitational wave wavelength, wave-optics effects induce a frequency-dependent modulation on the signal. CPU-based parameter estimation analyses for wave-optics lensing...
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Thomas Giordano (University of Liège)09/10/2026, 10:30
In order to reach the targeted low-frequency sensitivity of the Einstein Telescope, large cryogenic mirrors will have to be mounted on ultralow-frequency seismic isolation stages. In this context, ET-CRISTAL is developing a full-scale prototype suspending a 100 kg silicon test mass cooled to cryogenic temperatures by radiative cooling and isolated at low frequency from seismic noise. The...
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Elise Van den Bossche (Vrije Universiteit Brussel)09/10/2026, 10:50
The European third generation gravitational-wave detector Einstein Telescope will rely on cryogenics and silicon as mirror and suspension material to achieve unprecedented low-frequency sensitivity. Prototyping and characterisation of these new technologies on a system-level is needed to inform the design and future upgrades of the large-scale observatory. This is the mission of ETpathfinder,...
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Aaron Goodwin-Jones (UCLouvain)09/10/2026, 11:10
The proposed Einstein Telescope high-frequency interferometers (ET-HF) in their nominal configuration are limited by coating Brownian thermal noise (CBTN) and quantum shot noise. Achieving the target sensitivity requires up to 3 MW of laser power with advanced optical coatings. At these power levels, thermo-elastic and thermo-optic effects induce wavefront distortions, causing transverse mode...
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Seppe Staelens (University of Cambridge)09/10/2026, 11:30
The gravitational-wave detections reported by the LVK collaboration have so far been consistent with quasi-circular compact binary coalescences. Nevertheless, a small fraction of binaries may retain measurable orbital eccentricity in the LVK frequency band. Confident measurement of eccentricity would provide strong evidence for dynamically driven mergers; however, eccentric...
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Robin Chan (UGent | Royal Observatory of Belgium)09/10/2026, 11:50
Gravitational wave parameter estimation demands millions of waveform evaluations per event, a bottleneck set to worsen as next-generation detectors like the Einstein Telescope and Cosmic Explorer increase detection rates and signal duration. We present a major expansion of ripple, a JAX-based waveform package offering GPU acceleration and exact autodifferentiation, which now covers...
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Chun-Fung Wong (KU Leuven)09/10/2026, 13:40
Fisher-matrix forecasts are the standard tool for comparing proposed gravitational-wave detector networks, such as the triangular and double-L designs of the Einstein Telescope. When the likelihood is nearly flat in some direction and only the prior constrains it, the Fisher interval overstates the uncertainty — and because the size of this bias depends on detector geometry, it need not cancel...
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Luca Negri (Utrecht University & Nikhef)09/10/2026, 14:00
The Fisher Information Matrix is the most widely used tool to forecast and compare the parameter estimation capabilities of future gravitational waves detectors. This method relies on a linear approximation of the detectors' response which speeds up computation of confidence intervals by millions of times with respect to stochastic sampling methods. However, neglecting higher orders terms,...
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Antonin Oswald (UCLouvain)09/10/2026, 14:20
The geometrical configuration of the Einstein Telescope (ET) gravitational-wave observatory is one the most important design choices to be made for this future scientific facility. Two baseline configurations are currently being considered, a single triangle or 2 distant L-shaped detectors tilted by about 45◦. In this document we present a study of the scientific performance of the ET baseline...
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Jo van den Brand09/10/2026, 14:40
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Frederic Nguyen (ULiège)09/10/2026, 15:10
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Tjonnie Li (KU Leuven)09/10/2026, 15:40
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Kelly Holley-Bockelmann (SRON)
Astronomers now know that massive black holes are in nearly every galaxy.
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Though these black holes are an observational certainty, nearly every aspect of their evolution -- from their birth, to their fuel source, to their basic dynamics -- is a matter of lively debate. Fortunately, LISA, a space-based gravitational wave observatory set to launch in 2035, will revolutionize this field by... -
Future gravitational wave observatories, such as the Einstein Telescope, will detect thousands of mergers between compact objects annually. By detecting the effects of tidal deformation in binary neutron star mergers, these detectors will be the dominant way to study the equation of state of ultradense nuclear matter in the coming decades. However, this requires a scalable Bayesian...
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