Noise from scattered light in Virgo's second science run data

Accadia, T.; Acernese, F.; Antonucci, F.; Astone, P.; Ballardin, G.; Barone, F.; Barsuglia, M.; Bauer, Th.; Beker, M. G.; Belĺetoile, A.; Birindelli, S.; Bitossi, M.; Bizouard, M. A.; Blom, M.; Bondu, F.; Bonelli, L.; Bonnand, R.; Boschi, V.; Bosi, L.; Bouhou, B.; Braccini, S.; Bradaschia, C.; Brillet, A.; Brisson, V.; Budzyński, R.; Bulik, T.; Bulten, H.; Buskulic, D.; Buy, C.; Cagnoli, G.; Calloni, E.; Campagna, E.; Canuel, B.; Carbognani, F.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cesarini, E.; Mottin, Eric; Chincarini, A.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.; Corsi, A.; Coulon, J.-P.; Cuoco, E.; D’Antonio, S.; Dattilo, V.; Davier, M.; Day, R.; Rosa, R. De; Debreczeni, G.; Prete, M. Del; Fiore, L. Di; Lieto, A. Di; Emilio, M. Di Paolo; Virgilio, A. Di; Dietz, A.; Drago, M.; Fafone, V.; Ferrante, I.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Fournier, J.-D.; Franc, J.; Frasca, S.; Frasconi, F.; Freise, A.; Galimberti, M.; Gammaitoni, L.; Garufi, F.; Gáspár, M. E.; Gemme, G.; Genin, É.; Gennai, A.; Giazotto, A.; Gouaty, R.; Granata, M.; Greverie, C.; Guidi, G. M.; Hayau, J.-F.; Heitmann, H.; Hello, P.; Hild, S.; Huet, D.; Jaranowski, P.; Kowalska, I.; Królak, A.; Leroy, N.; Letendre, N.; Li, T. G. F.; Lorenzini, M.; Loriette, V.; Losurdo, G.; Majorana, E.; Maksimovic, I.; Man, N.; Mantovani, M.; Marchesoni, F.; Marion, F.; Marque, J.; Martelli, F.; Masserot, A.; Michel, C.; Milano, L.; Minenkov, Y.; Mohan, M.; Morgado, N.; Morgia, A.; Mosca, S.; Moscatelli, V.; Mours, B.; Neri, I.; Nocera, F.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Paoletti, F.; Pardi, S.; Parisi, M.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Persichetti, G.; Pichot, M.; Piergiovanni, F.; Piȩtka, M.; Pinard, L.; Poggiani, R.; Prato, Mirko; Prodi, G. A.; Punturo, M.; Puppo, P.; Rabeling, D. S.; Rácz, István; Rapagnani, P.; Re, V.; Regimbau, T.; Ricci, F.; Robinet, F.; Rocchi, A.; Rolland, L.; Romano, R.; Rosińska, D.; Ruggi, P.; Sassolas, B.; Sentenac, D.; Sperandio, L.; Sturani, R.; Swinkels, B. L.; Toncelli, A.; Tonelli, M.; Torre, O.; Tournefier, E.; Travasso, F.; Vajente, G.; Brand, J. van den; Putten, S. van der; Vasúth, M.; Vavoulidis, M.; Vedovato, G.; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinet, J.-Y.; Vocca, H.; Was, M.; Yvert, M.

doi:10.1088/0264-9381/27/19/194011

Cited by 83 publications

(71 citation statements)

References 9 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Scattered light is a common source of noise in the LIGO and Virgo detectors. Stray light is reflected back into the main interferometer path, resulting in excess power in the data [91,229,230]. Motion of the reflective surface, such as optic mounts, phase shift the reflected light.…”

Section: Scattered Lightmentioning

confidence: 99%

See 1 more Smart Citation

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

Abbott¹,

Abbott²,

Abbott³

et al. 2019

View full text Add to dashboard Cite

We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1 M ⊙ during the first and second observing runs of the advanced gravitationalwave detector network. During the first observing run (O1), from September 12, 2015 to January 19, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November 30, 2016 to August 25, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818, and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between 18.6 þ3.2 −0.7 M ⊙ and 84.4 þ15.8 −11.1 M ⊙ and range in distance between 320 þ120 −110 and 2840 þ1400 −1360 Mpc. No neutron star-black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false-alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of 110 − 3840 Gpc −3 y −1 for binary neutron stars and 9.7 − 101 Gpc −3 y −1 for binary black holes assuming fixed population distributions and determine a neutron star-black hole merger rate 90% upper limit of 610 Gpc −3 y −1 .

show abstract

Section: Scattered Lightmentioning

confidence: 99%

“…The strain noise amplitude of scattered light instrumental artifacts correlates with the intensity of the corresponding ground motion. Additionally, higher velocities of optic motion lead to higher-frequency content in the scattered light [229].…”

Section: Scattered Lightmentioning

confidence: 99%

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

Abbott¹,

Abbott²,

Abbott³

et al. 2019

View full text Add to dashboard Cite

show abstract

“…Scattered light is intrinsically non-stationary, since the amplitude and maximum frequency of this noise source depend on the motion of the scattering element. 4 Scattered light has been mitigated with a careful placement of black glass absorbing baffles and beam dumps. All spurious beams from the anti-reflection coated surfaces are intercepted and dumped.…”

mentioning

confidence: 99%

“…In addition the increased seismic isolation will also help in reducing scattered light. Indeed, scattered light up-conversion is highly non-linear: 4 residual motion at few Hz will be the dominant contributor to scattered light phase noise, while the slower 100 mHz motion that we will introduce to periodically stress the cantilevers results in a negligible contribution. The second potentially problematic non-stationary noise source can be traced to the actuation chain which used to apply force on the two test cantilevers.…”

mentioning

confidence: 99%

An instrument to measure mechanical up-conversion phenomena in metals in the elastic regime

Vajente

Quintero

et al. 2016

Review of Scientific Instruments

View full text Add to dashboard Cite

Physical aging of plastoferrites under tensile stress and its effect on microwave properties J. Appl. Phys. 104, 064108 (2008) Crystalline materials, such as metals, are known to exhibit deviation from a simple linear relation between strain and stress when the latter exceeds the yield stress. In addition, it has been shown that metals respond to varying external stress in a discontinuous way in this regime, exhibiting discrete releases of energy. This crackling noise has been extensively studied both experimentally and theoretically when the metals are operating in the plastic regime. In our study, we focus on the behavior of metals in the elastic regime, where the stresses are well below the yield stress. We describe an instrument that aims to characterize non-linear mechanical noise in metals when stressed in the elastic regime. In macroscopic systems, this phenomenon is expected to manifest as a non-stationary noise modulated by external disturbances applied to the material, a form of mechanical up-conversion of noise. The main motivation for this work is for the case of maraging steel components (cantilevers and wires) in the suspension systems of terrestrial gravitational wave detectors. Such instruments are planned to reach very ambitious displacement sensitivities, and therefore mechanical noise in the cantilevers could prove to be a limiting factor for the detectors' final sensitivities, mainly due to non-linear up-conversion of low frequency residual seismic motion to the frequencies of interest for the gravitational wave observations. We describe here the experimental setup, with a target sensitivity of 10 −15 m/ √Hz in the frequency range of 10-1000 Hz, a simple phenomenological model of the non-linear mechanical noise, and the analysis method that is inspired by this model. Published by AIP Publishing. [http://dx

show abstract

“…This noise is typically not of a fundamental nature (like shot-noise for example) but coming from other technical sources like scattered light [11] or electronic noise. The contribution of this spurious coupling mechanisms to the detector sensitivity can be directly estimated by means of projection measurements, as already explained in Section 4 of [4].…”

Section: Noise Couplings To Gravitational Channelmentioning

confidence: 99%

Performance of the Virgo interferometer longitudinal control system during the second science run

Accadia

Acernese

Antonucci

et al. 2011

Astroparticle Physics

View full text Add to dashboard Cite

Noise from scattered light in Virgo's second science run data

Cited by 83 publications

References 9 publications

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

An instrument to measure mechanical up-conversion phenomena in metals in the elastic regime

Performance of the Virgo interferometer longitudinal control system during the second science run

Contact Info

Product

Resources

About