Conveners
Poster Session
- Jessica Steinlechner
- Andrew Spencer
- Anna Green (Nikhef)
The ETIC-ADONI optical bench is an experiment carried out within the PNRR
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...
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).
The Ferrara ET Research Unit has been working on 2D birefringence maps...
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...
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...
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...
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...
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...
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...
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...
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...
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...
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...
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...
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...
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...
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...
