Conveners
Poster Session
- Jessica Steinlechner
- Andrew Spencer
- Anna Green (Nikhef)
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simone Lombardi (INAF Padova)Opticsposter
The ETIC-ADONI optical bench is an experiment carried out within the PNRR
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ETIC project (Einstein Telescope Infrastructure Consortium). It is located at the
Astrophysical Observatory of Arcetri in Florence, and its objective is to investi-
gate the application of a deformable mirror (DM)—already employed by INAF in
adaptive optics (AO) for ground-based astronomical observations—to the... -
Aurelie Mailliet, Nicola Canale (University of Ferrara - INFN Ferrara)Opticsposter
To reach the sensitivity requirement of Einstein Telescope for gravitational waves detection, the birefringence of optic substrates must be optimised. The intrinsic birefringence of such substrates mainly comes from internal stress within the material, but can also be induced externally (by optical mounts for instance).
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The Ferrara ET Research Unit has been working on 2D birefringence maps... -
Tomislav AndricSuspensionsposter
GEMINI is an underground research and development facility dedicated to advancing seismic isolation and control technologies for future gravitational-wave observatories. Its primary mission is to support the Einstein Telescope (ET) by providing a testbed for inter-platform control strategies, essential for stabilizing auxiliary interferometer degrees of freedom. The facility consists of...
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Qian HuDiv10poster
Bayesian inference with stochastic sampling has been widely used to obtain the properties of gravitational wave (GW) sources. Although computationally intensive, its cost remains manageable for current second-generation GW detectors because of the relatively low event rate and signal-to-noise ratio (SNR). The third-generation (3G) GW detectors are expected to detect hundreds of thousands of...
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Valeria Milotti (University of Padova, INFN PD)ISB - Otherposter
A major limiting factor in improving sensitivity of Gravitational Wave (GW) detectors is thermal noise in the amorphous mirror coatings of interferometric gravitational-wave detectors. This is especially true for the crucial frequency range around 100 Hz in room-temperature detectors. Mirror coatings are deposited by Ion-Beam Sputtering and designed as thickness-optimized Bragg’s...
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Dr Joris van Heijningen (VU Amsterdam)Suspensionsposter
Future gravitational-wave (GW) detectors such as Einstein Telescope (ET) will be cryogenic to decrease thermal noise to be sensitive to low-frequency GWs. In addition to this thermal noise reduction, there is an opportunity for superconductive technology introduction. We can just make our current interferometric sensing and coil-magnet actuation cryo-compatible, but superconductivity solutions...
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Christophe ColletteSuspensionsposter
This talk will present the latest achievements in active seismic isolation on the E-TEST prototype. The E-TEST prototype is a facility for the Einstein Telescope. It serves as a unique full-scale test bench designed to suspend a 100 kg test mass, cooled down to cryogenic temperatures through radiative cooling, and isolated using an inverted pendulum mounted on an active platform. This...
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Riccardo De Salvo (California State University of Los Angeles)Infrastructuresposter
We propose to replace the large underground halls with a short tunnel section above the main one, connected by vertical wells that host the seismic attenuation chains. This solution has substantial advantages in terms of physics performance, engineering, safety and even cost.
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By placing the heads of the seismic attenuation chains on the bedrock of the upper tunnel it removes them from the... -
Stefano Mais (DICAAR, Università degli Studi di Cagliari)Infrastructuresposter
The Einstein Telescope project belongs to an unprecedented infrastructural dimension: a system of underground tunnels forming a triangular layout with 10 km-long sides, located about 300 meters below the surface. It is set to redefine not only the paradigms of scientific research, but also the settlement patterns, cultural frameworks, and landscapes of the territories chosen to host this...
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Matteo Di Giovanni (La Sapienza Università di Roma - INFN Roma)Vacuum and Cryogenicsposter
In this talk we present the summary of a set of environmental noise measurements conducted on cryogenic facilities at CERN and at the University of Tokyo. The goal is to assess the impact on the background noise levels of these facilities and to provide valuable information for the design of noise suppression systems in Einstein Telescope. In fact, one of the key features of Einstein Telescope...
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Giuseppe GrecoCommunicationsposter
ETIC (Einstein Telescope Infrastructure Consortium) project, an initiative by the Italian Ministry of University and Research, led by the National Institute for Nuclear Physics (INFN). Launched in 2023, the project has two main objectives: conducting a feasibility and site characterization study in Sos Enattos, and developing a national network of laboratories within INFN, universities, and...
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Paul Ophardt (Helmut-Schimidt-Universität)Active Noise Mitigationposter
Newtonian noise (NN) induced by seismic density fluctuations limits the sensitivity of current and future gravitational-wave detectors. In particular, it poses a significant challenge to achieving the low-frequency benchmark sensitivity of the upcoming third-generation detector Einstein Telescope (ET). Several mitigation strategies for NN in ET have been proposed, all of which rely on arrays...
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Markus WaltherActive Noise Mitigationposter
Radiation pressure noise at low frequencies remains a key challenge for the Einstein Telescope (ET). One approach is active stabilization using ultralight micromirrors suspended by extremely soft springs, providing large displacement response to fluctuating photon pressure. These devices are fabricated on silicon-on-insulator wafers and released by vapor HF etching, yielding mechanically...
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Tim Kuhlbusch (RWTH Aachen University)Active Noise Mitigationposter
Predicting specific noise realizations from witness sensors will be an essential technique to improve the sensitivity of the Einstein Telescope. Different techniques, like classical or deep learning filters, can be employed to reduce the Newtonian noise level. We are presenting a Python framework that automates the evaluation of multiple noise cancellation techniques on a set of simulated or...
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Mohamed Elbashbishy (Forschungszentrum Jülich GmbH)Vacuum and Cryogenicsposter
Ultra-high vacuum (UHV) systems are critical in experimental physics and engineering, particularly in projects like the Einstein Telescope (ET), where even minor leaks can affect precision measurements and large leaks can destroy the setup. For this reason, mechanical components such as fast shutters can be used to protect the system. Large leaks can generate pressure fronts propagating at...
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Thomas SiefkeOpticsposter
The thermal noise of the end-test-mass mirrors in gravitational-wave detectors remains a major sensitivity limitation, largely due to the multi-layer Bragg-mirror-stacks required to achieve ultra-high reflectance. For the next-generation Einstein Telescope (ET), we propose a stacked-mirror approach that combines the complementary advantages of metasurfaces and Bragg mirrors, while mitigating...
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Dr Iryna Buchovska (Leibniz-Institut für Kristallzüchtung)Suspensionsposter
Monocrystalline silicon fibers are a promising candidate for suspending silicon test masses in gravitational-wave detectors. The excellent thermal and mechanical properties of crystalline silicon enable stable support of heavy mirrors and efficient extraction of laser-induced heat. Moreover, silicon's exceptional material behavior at cryogenic temperatures aligns well with the operational...
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Lucia TrozzoSuspensionsposter
The era of third-generation gravitational wave detectors is approaching, and the Einstein Telescope (ET) a large size interferometer, is becoming a concrete reality. The underground installation of the instrument offers significant advantages from seismic and local disturbances point of views: seismic noise level, indeed, is reduced by a factor of 100 compared to surface locations. In...
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Elisabet Vallejo (IFAE)Vacuum and Cryogenicsposter
The Einstein Telescope (ET), a next-generation underground gravitational-wave observatory, aims to extend sensitivity to lower frequencies through cryogenic cooling of its main optics. A critical challenge in this design is the cryoarea, where baffles must operate under extreme cryogenic conditions that alter material, thermal, optical, and vibrational properties. Building on previous studies...
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Abhay Karia (Nikhef)Active Noise Mitigationposter
The detection of low-frequency gravitational waves (below 10 Hz) is critical for probing the astrophysical origins of black holes and for expanding the observable frequency range of next-generation interferometers. However, current detectors are fundamentally limited in this regime by seismic noise and tilt-to-horizontal coupling. The Omnisens project: a 6D interferometric inertial isolation...
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Ismail El Ouedghiri-IdrissiOpticsposter
The next generation of gravitational wave detectors, such as the Einstein Telescope and LIGO Voyager, requires unprecedented sensitivity. A key limitation to this sensitivity is thermal noise from mirror coatings, particularly within their most sensitive frequency range. To address this, next-generation detectors are shifting toward cryogenic low-frequency interferometers, with silicon serving...
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Nicole BusdonOpticsposter
One of the most critical components of gravitational wave interferometers is their mirror test masses, as coating thermal noise is a primary limiting factor in the 20–2000 Hz frequency range. For this reason, one of the two nested interferometers composing the Einstein Telescope (ET-LF) is designed to operate at cryogenic temperatures. However, characterizing both mechanical and optical losses...
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Francesco BianchiVacuum and Cryogenicsposter
The ET layout provides space for the vacuum towers of the LF and HF interferometers. The towers will be housed in caverns designed to facilitate manoeuvring operations and ensure correct spacing between the components of the interferometers. Both LF and HF towers will need to be installed on a basement to make use of the space underneath them for manoeuvring. Furthermore, the cryogenic towers...
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Lorenzo AspreaEIBposter
The increasing data volume from gravitational-wave observatories presents both an opportunity for new discoveries and a significant challenge for existing analysis methods. While deep learning models, particularly those designed for image processing, are powerful tools for analyzing 2D time-frequency representations of transient signals, their application has been limited by a fundamental...
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Barbara GaraventaISB - Otherposter
The Einstein Telescope Infrastructure Consortium (ETIC), coordinated by INFN, has developed laboratories to support the future Einstein Telescope and to carry out site characterization at Sos-Enattos, in Sardinia (Italy). This poster presents the GALILEO project at INFN and the University of Genoa. The initiative includes a new quantum optics laboratory, equipped with two 1550 nm laser...
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Tatevik ChalyanOpticsposter
One of the limiting factors for gravitational wave detection sensitivity to date is the coating thermal noise in the lower audio-band. The use of cryogenically cooled crystalline silicon in combination with high-quality silicon-based coatings for the test mass mirrors will allow tackling the thermal noise problem. In the gravitational wave interferometry, moving the laser wavelengths to 2 µm...
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Andrea MoscatelloOpticsposter
High-sensitivity optical measurements, such as those carried out in interferometric gravitational-wave detectors, are highly susceptible to stray light noise. Because of the exceptional quality of the optics employed, scattering is often dominated by residual particulate contamination. This represents a critical challenge not only for the next-generation Einstein Telescope but also for current...
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Roberto CiminoVacuum and Cryogenicsposter
In the upcoming generation of gravitational wave detectors (GWDs), the use of cryogenic mirrors is a great technological challenge and may present potentially new noise sources limiting the desired sensitivity. As shown in KAGRA, frost formation on cold optics is a known severe issue for cryogenic GWDs. Also, the mirror charging, as observed in LIGO, may severely affect sensitivity, and the...
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A. Erbanni, A. Pasqualetti, B. Piffre, G. Gargiulo, L. Francescon (EGO), T. ZelenovaVacuum and Cryogenicsposter
The ET cryogenic tower will host the test mass (TM) operating at 10–20 K, where key challenges are attaining the exceptionally low vacuum level (normally the lowest in the entire ET system) and realizing the cryostat with ultra-low noise technology.Large-scale prototype initiatives have been launched by major laboratories to investigate cryostat design and cooling strategies, and dedicated...
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Mariusz SuchenekISB - Otherposter
The Einstein Telescope (ET), as a next-generation underground gravitational wave observatory, requires a comprehensive environmental monitoring system to achieve its ambitious sensitivity goals. Dense arrays of seismic and infrasound sensors must operate continuously to track local and global disturbances and to support advanced noise mitigation strategies. Given the large number of sensors...
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Jan-Niklas Feldhusen (University of Hamburg)Active Noise Mitigationposter
Deep Frequency Modulation Interferometry (DFMI) offers a powerful approach to achieve precise displacement readout as well as absolute ranging with reduced complexity and compact sensing heads. Minimizing local sensing noise is crucial to reduce controls noise in e.g. active suspension damping and therefore DFMI will be a crucial technology to achieve the low-frequency sensitivity of future...
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Simone MarchettiOpticsposter
The detection of gravitational waves (GWs) depends upon interferometers that use mirrors specifically designed to reduce both optical absorption and mechanical dissipation, thus meeting the high sensitivity demands necessary for detection. Advanced mirror coatings are made up of alternating thin layers of dielectrics such as tantalum oxide (Ta₂O₅), doped with TiO₂, and silicon dioxide (SiO₂)....
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