Picoradiant tiltmeter and direct ground tilt measurements at the Sos Enattos site

Allocca, A.; Avino, S.; Calloni, E.; Caprara, S.; Carpinelli, M.; D’Urso, D.; Laurentis, M. De; Rosa, R. De; Errico, L.; Gagliardi, G.; Grilli, M.; Mangano, V.; Marsella, Maria; Naticchioni, L.; Pasqualetti, A.; Pepe, G. P.; Perciballi, M.; Pesenti, Luca; Puppo, P.; Rapagnani, P.; Ricci, F.; Rosa, Luigi; Rovelli, Carlo; Rozza, D.; Ruggi, P.; Saini, N. L.; Sipala, V.; Stornaiuolo, Daniela; Tafuri, F.

doi:10.1140/epjp/s13360-021-01993-w

Cited by 9 publications

(7 citation statements)

References 29 publications

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“…Despite the efforts performed by different experimental groups [20,21] in the development of a suited sensor for high precision ground-tilt measurements, we do not have any experimental measurements supporting our simulation model investigation, and we can only give a lower limit evaluation of it by using the following empirical formula:…”

Section: Sos Enattos Site: Ground Tilt Lower Limit Estimationmentioning

confidence: 99%

New Generation of Superattenuator for Einstein Telescope: preliminary studies

Bertocco,

Bruno,

De Rosa

et al. 2024

Class. Quantum Grav.

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Seismic noise and local disturbances are dominant noise sources for ground-based Gravitational Waves detectors in the low frequency region (0.1 to 10 Hz) limiting their sensitivity and duty cycle. With the introduction of high-performance seismic isolation systems based on mechanical pendula, the 2nd generation laser interferometric detectors have reached the scientific goal of the first direct observation of GW signals thanks to the extension of the detection bandwidth down to 10 Hz.Now, the 3rd generation instrument era is approaching, and the Einstein Telescope giant interferometer is becoming a reality with the possibility to install the detector in an underground site where seismic noise is 100 times smaller than on surface. Moreover, new available technologies as well as the experience acquired in operating advanced detectors are key points to further extend the detection bandwidth down to 2 Hz with the possibility to suspend cryogenic payload and then mitigating Thermal Noise too. Here, we present a preliminary study devoted to improving seismic attenuation performance of the Advanced VIRGO Superattenuator in the low frequency region of about five orders of magnitude. Particular care has been carried on in analyzing the possibility to improve the vertical attenuation performance with a multi-stage pendulum chain equipped with magnetic anti-springs that is hung to a double Inverted Pendulum in nested configuration. The feedback control requirements and possible strategies to be adopted for this last element will be presented.

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Section: Sos Enattos Site: Ground Tilt Lower Limit Estimationmentioning

confidence: 99%

New Generation of Superattenuator for Einstein Telescope: preliminary studies

Bertocco,

Bruno,

De Rosa

et al. 2024

Class. Quantum Grav.

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“…It is an immense benefit for NNC to deal with only one type of seismic wave [33], and so the choice of vertical geophones measuring Rayleigh-wave displacement is justified. As a note, a tiltmeter was deployed at the NEB to investigate a potential utilization for NNC [24,26]. It must be emphasized that the discussion so far is accurate only if the surface is flat, which is not the case at Virgo around its test masses [15].…”

Section: Instrumentationmentioning

confidence: 99%

“…It is equipped with two different optical readout systems comprising a Michelson interferometer for higher sensitivities and an auxiliary optical lever capable of handling a larger dynamic range. A detailed description of the tiltmeter and an assessment of its sensitivity in a quiet seismic environment can be found in [40] and [26], respectively. Figure 11(a) shows the 10 th , 50 th , and 90 th percentiles of the PSDs of the tilt signal.…”

Section: Proof Of Principlementioning

confidence: 99%

Design and implementation of a seismic Newtonian-noise cancellation system for the Virgo gravitational-wave detector

Koley,

Harms,

Badaracco

et al. 2023

Preprint

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Terrestrial gravity perturbations caused by seismic fields produce the so-called Newtonian noise in gravitational-wave detectors, which is predicted to limit their sensitivity in the upcoming observing runs. In the past, this noise was seen as an infrastructural limitation, i.e., something that cannot be overcome without major investments to improve a detector's infrastructure. However, it is possible to have at least an indirect estimate of this noise by using the data from a large number of seismometers deployed around a detector's suspended test masses. The noise estimate can be subtracted from the gravitational-wave data; a process called Newtonian-noise cancellation (NNC). In this article, we present the design and implementation of the first NNC system at the Virgo detector as part of its AdV+ upgrade. It uses data from 110 vertical geophones deployed inside the Virgo buildings in optimized array configurations. We use a separate tiltmeter channel to test the pipeline in a proof-of-principle. The system has been running with good performance over months.

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“…After few months of updates, devoted to the optical delay line installation and to the amplitude noise subtraction implementation described above, the site tilt was measured in the NN frequency region (2-20 Hz). The results are reported in [90].…”

Section: First Tilt Measurements At Virgo and Sos-enattosmentioning

confidence: 99%

Research Facilities for Europe’s Next Generation Gravitational-Wave Detector Einstein Telescope

et al. 2022

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The Einstein Telescope is Europe’s next generation gravitational-wave detector. To develop all necessary technology, four research facilities have emerged across Europe: The Amaldi Research Center (ARC) in Rome (Italy), ETpathfinder in Maastricht (The Netherlands), SarGrav in the Sos Enattos mines on Sardinia (Italy) and E-TEST in Liége (Belgium) and its surroundings. The ARC pursues the investigation of a large cryostat, equipped with dedicated low-vibration cooling lines, to test full-scale cryogenic payloads. The installation will be gradual and interlaced with the payload development. ETpathfinder aims to provide a low-noise facility that allows the testing of full interferometer configurations and the interplay of their subsystems in an ET-like environment. ETpathfinder will focus amongst others on cryogenic technologies, silicon mirrors, lasers and optics at 1550 and 2090 nm and advanced quantum noise reduction schemes. The SarGrav laboratory has a surface lab and an underground operation. On the surface, the Archimedes experiment investigates the interaction of vacuum fluctuations with gravity and is developing (tilt) sensor technology for the Einstein Telescope. In an underground laboratory, seismic characterisation campaigns are undertaken for the Sardinian site characterisation. Lastly, the Einstein Telecope Euregio meuse-rhine Site & Technology (E-TEST) is a single cryogenic suspension of an ET-sized silicon mirror. Additionally, E-TEST investigates the Belgian–Dutch–German border region that is the other candidate site for Einstein Telescope using boreholes and seismic arrays and hydrogeological characterisation. In this article, we describe the Einstein Telescope, the low-frequency part of its science case and the four research facilities.

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Picoradiant tiltmeter and direct ground tilt measurements at the Sos Enattos site

Cited by 9 publications

References 29 publications

New Generation of Superattenuator for Einstein Telescope: preliminary studies

New Generation of Superattenuator for Einstein Telescope: preliminary studies

Design and implementation of a seismic Newtonian-noise cancellation system for the Virgo gravitational-wave detector

Research Facilities for Europe’s Next Generation Gravitational-Wave Detector Einstein Telescope

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