TY - JOUR
T1 - Calibration of advanced Virgo and reconstruction of the detector strain h(t) during the observing run O3
AU - Acernese, F.
AU - Agathos, M.
AU - Ain, A.
AU - Albanesi, S.
AU - Allocca, A.
AU - Amato, A.
AU - Andrade, T.
AU - Andres, N.
AU - Andric, T.
AU - Ansoldi, S.
AU - Antier, S.
AU - Arene, M.
AU - Arnaud, N.
AU - Assiduo, M.
AU - Astone, P.
AU - Aubin, F.
AU - Babak, S.
AU - Badaracco, F.
AU - Bader, M.K.M.
AU - Bagnasco, S.
AU - Baird, J.
AU - Ballardin, G.
AU - Baltus, G.
AU - Barbieri, C.
AU - Barneo, P.
AU - Barone, F.
AU - Barsuglia, M.
AU - Barta, D.
AU - Basti, A.
AU - Bawaj, M.
AU - Bazzan, M.
AU - Bejger, M.
AU - Belahcene, I.
AU - Benedetto, V.
AU - Bernuzzi, S.
AU - Bersanetti, D.
AU - Bertolini, A.
AU - Bhardwaj, U.
AU - Bini, S.
AU - Bischi, M.
AU - Bitossi, M.
AU - Virgo Collaboration
AU - Danilishin, S.
AU - Hild, S.
AU - Koekoek, G.
AU - Singha, A.
AU - Spagnuolo, V.
AU - Steinlechner, J.
AU - Steinlechner, S.
AU - Utina, A.
AU - van den Brand, J.F.J.
N1 - Funding Information:
The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Netherlands Organization for Scientific Research (NWO), for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Spanish Agencia Estatal de Investigación, the Consellera d’Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the European Union-European Regional Development Fund; Foundation for Polish Science (FNP), the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertées (ARC) and Fonds Wetenschappelijk Onderzoek–Vlaanderen (FWO), Belgium, the European Commission. The authors gratefully acknowledge the support of the NSF, STFC, INFN, CNRS and Nikhef for provision of computational resources. We would like to thank all of the essential workers who put their health at risk during the COVID-19 pandemic, without whom we would not have been able to complete this work.
Publisher Copyright:
© 2022 IOP Publishing Ltd.
PY - 2022/2/17
Y1 - 2022/2/17
N2 - The three advanced Virgo and LIGO gravitational wave detectors participated to the third observing run (O3) between 1 April 2019 15:00 UTC and 27 March 2020 17:00 UTC, leading to several gravitational wave detections per month. This paper describes the advanced Virgo detector calibration and the reconstruction of the detector strain h(t) during O3, as well as the estimation of the associated uncertainties. For the first time, the photon calibration technique as been used as reference for Virgo calibration, which allowed to cross-calibrate the strain amplitude of the Virgo and LIGO detectors. The previous reference, so-called free swinging Michelson technique, has still been used but as an independent cross-check. h(t) reconstruction and noise subtraction were processed online, with good enough quality to prevent the need for offline reprocessing, except for the two last weeks of September 2019. The uncertainties for the reconstructed h(t) strain, estimated in this paper in a 20-2000 Hz frequency band, are frequency independent: 5% in amplitude, 35 mrad in phase and 10 mu s in timing, with the exception of larger uncertainties around 50 Hz.
AB - The three advanced Virgo and LIGO gravitational wave detectors participated to the third observing run (O3) between 1 April 2019 15:00 UTC and 27 March 2020 17:00 UTC, leading to several gravitational wave detections per month. This paper describes the advanced Virgo detector calibration and the reconstruction of the detector strain h(t) during O3, as well as the estimation of the associated uncertainties. For the first time, the photon calibration technique as been used as reference for Virgo calibration, which allowed to cross-calibrate the strain amplitude of the Virgo and LIGO detectors. The previous reference, so-called free swinging Michelson technique, has still been used but as an independent cross-check. h(t) reconstruction and noise subtraction were processed online, with good enough quality to prevent the need for offline reprocessing, except for the two last weeks of September 2019. The uncertainties for the reconstructed h(t) strain, estimated in this paper in a 20-2000 Hz frequency band, are frequency independent: 5% in amplitude, 35 mrad in phase and 10 mu s in timing, with the exception of larger uncertainties around 50 Hz.
KW - gravitational wave
KW - strain reconstruction
KW - Virgo
KW - O3 observing run
KW - calibration
KW - strain uncertainties
U2 - 10.1088/1361-6382/ac3c8e
DO - 10.1088/1361-6382/ac3c8e
M3 - Article
SN - 0264-9381
VL - 39
JO - Classical and Quantum Gravity
JF - Classical and Quantum Gravity
IS - 4
M1 - 045006
ER -