Calibration of Advanced Virgo and reconstruction of detector strain h(t) during the Observing Run O3

Acernese, F.; Agathos, M.; Ain, A.; Albanesi, S.; Allocca, A.; Amato, A.; Andrade, T.; Andres, N.; Andrić, T.; Ansoldi, S.; Antier, S.; Arène, M.; Arnaud, N.; Assiduo, M.; Astone, P.; Aubin, F.; Babak, S.; Badaracco, F.; Bader, M. K. M.; Bagnasco, S.; Baird, J.; Ballardin, G.; Baltus, G.; Barbieri, C.; Barneo, P.; Barone, F.; Barsuglia, M.; Barta, D.; Basti, A.; Bawaj, M.; Bazzan, M.; Bejger, M.; Belahcene, I.; Benedetto, V.; Bernuzzi, S.; Bersanetti, D.; Bertolini, A.; Bhardwaj, U.; Bini, S.; Bischi, M.; Bitossi, M.; Bizouard, M. -A.; Bobba, F.; Boer, M.; Bogaert, G.; Boldrini, M.; Bonavena, L. D.; Bondu, F.; Bonnand, R.; Boom, B. A.; Boschi, V.; Boudart, V.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Branchesi, M.; Breschi, M.; Briant, T.; Brillet, A.; Brooks, J.; Bruno, G.; Bulik, T.; Bulten, H. J.; Buskulic, D.; Buy, C.; Cagnoli, G.; Calloni, E.; Canepa, M.; Canevarolo, S.; Cannavacciuolo, M.; Carapella, G.; Carbognani, F.; Carpinelli, M.; Carullo, G.; Diaz, J. Casanueva; Casentini, C.; Caudill, S.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cerdá-Durán, P.; Cesarini, E.; Chaibi, W.; Chanial, P.; Chassande-Mottin, E.; Chaty, S.; Chiadini, F.; Chiarini, G.; Chierici, R.; Chincarini, A.; Chiofalo, M. L.; Chiummo, A.; Christensen, N.; Ciani, G.; Cieślar, M.; Ciecielag, P.; Cifaldi, M.; Ciolfi, R.; Cipriano, F.; Cirone, A.; Clesse, S.; Cleva, F.; Coccia, E.; Codazzo, E.; Cohadon, P. -F.; Cohen, D. E.; Colombo, A.; Colpi, M.; Conti, L.; Cordero-Carrión, I.; Corezzi, S.; Corre, D.; Cortese, S.; Coulon, J. -P.; Croquette, M.; Cudell, J. R.; Cuoco, E.; Curyło, M.; Dabadie, P.; Canton, T. Dal; Dall'Osso, S.; D'Angelo, B.; Danilishin, S.; D'Antonio, S.; Dattilo, V.; Davier, M.; De Laurentis, M.; De Lillo, F.; De Matteis, F.; De Pietri, R.; De Rosa, R.; De Rossi, C.; De Simone, R.; Degallaix, J.; Deléglise, S.; Del Pozzo, W.; Depasse, A.; Di Fiore, L.; Di Giorgio, C.; Di Giovanni, F.; Di Giovanni, M.; Di Girolamo, T.; Di Lieto, A.; Di Pace, S.; Di Palma, I.; Di Renzo, F.; Dietrich, T.; D'Onofrio, L.; Drago, M.; Ducoin, J. -G.; Durante, O.; D'Urso, D.; Duverne, P. -A.; Eisenmann, M.; Errico, L.; Estevez, D.; Fafone, V.; Farinon, S.; Favaro, G.; Fays, M.; Fenyvesi, E.; Ferrante, I.; Fidecaro, F.; Figura, P.; Fiori, I.; Fittipaldi, R.; Fiumara, V.; Flaminio, R.; Font, J. A.; Frasca, S.; Frasconi, F.; Fronzé, G. G.; Gamba, R.; Garaventa, B.; Garufi, F.; Gemme, G.; Gennai, A.; Ghosh, Archisman; Giacomazzo, B.; Giacoppo, L.; Giri, P.; Gissi, F.; Goncharov, B.; Gosselin, M.; Gouaty, R.; Grado, A.; Granata, M.; Granata, V.; Greco, G.; Grignani, G.; Grimaldi, A.; Grimm, S. J.; Gruning, P.; Guerra, D.; Guidi, G. M.; Guixé, G.; Guo, Y.; Gupta, P.; Haegel, L.; Halim, O.; Hannuksela, O.; Harder, T.; Haris, K.; Harms, J.; Haskell, B.; Heidmann, A.; Heitmann, H.; Hello, P.; Hemming, G.; Hennes, E.; Hild, S.; Hofman, D.; Hui, V.; Idzkowski, B.; Iess, A.; Jacqmin, T.; Janquart, J.; Janssens, K.; Jaranowski, P.; Jonker, R. J. G.; Juste, V.; Kéfélian, F.; Kalaghatgi, C.; Karathanasis, C.; Katsanevas, S.; Khetan, N.; Koekoek, G.; Koley, S.; Kolstein, M.; Królak, A.; Kuijer, P.; La Rosa, I.; Lagabbe, P.; Laghi, D.; Lamberts, A.; Lartaux-Vollard, A.; Lazzaro, C.; Leaci, P.; Lemaître, A.; Leroy, N.; Letendre, N.; Leyde, K.; Linde, F.; Llorens-Monteagudo, M.; Longo, A.; Portilla, M. Lopez; Lorenzini, M.; Loriette, V.; Losurdo, G.; Lumaca, D.; Macquet, A.; Magazzù, C.; Magnozzi, M.; Majorana, E.; Maksimovic, I.; Man, N.; Mangano, V.; Mantovani, M.; Mapelli, M.; Marchesoni, F.; Marion, F.; Marquina, A.; Marsat, S.; Martelli, F.; Martinez, M.; Martinez, V.; Masserot, A.; Mastrogiovanni, S.; Meijer, Q.; Menendez-Vazquez, A.; Mereni, L.; Merzougui, M.; Miani, A.; Michel, C.; Milano, L.; Miller, A.; Miller, B.; Milotti, E.; Minazzoli, O.; Minenkov, Y.; Mir, Ll. M.; Miravet-Tenés, M.; Montani, M.; Morawski, F.; Mours, B.; Muciaccia, F.; Mukherjee, Suvodip; Musenich, R.; Nagar, A.; Napolano, V.; Nardecchia, I.; Naticchioni, L.; Neilson, J.; Nelemans, G.; Nguyen, C.; Nissanke, S.; Nitoglia, E.; Nocera, F.; Oganesyan, G.; Olivetto, C.; Périgois, C.; Pagano, G.; Pagliaroli, G.; Palomba, C.; Pang, P. T. H.; Pannarale, F.; Paoletti, F.; Paoli, A.; Paolone, A.; Pascucci, D.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patricelli, B.; Pegoraro, M.; Perego, A.; Pereira, A.; Perreca, A.; Perriès, S.; Phukon, K. S.; Piccinni, O. J.; Pichot, M.; Piendibene, M.; Piergiovanni, F.; Pierini, L.; Pierro, V.; Pillant, G.; Pillas, M.; Pilo, F.; Pinard, L.; Pinto, I. M.; Pinto, M.; Piotrzkowski, K.; Placidi, E.; Plastino, W.; Poggiani, R.; Polini, E.; Popolizio, P.; Porter, E. K.; Poulton, R.; Pracchia, M.; Pradier, T.; Principe, M.; Prodi, G. A.; Prosposito, P.; Puecher, A.; Punturo, M.; Puosi, F.; Puppo, P.; Raaijmakers, G.; Radulesco, N.; Rapagnani, P.; Razzano, M.; Regimbau, T.; Rei, L.; Rettegno, P.; Ricci, F.; Riemenschneider, G.; Rinaldi, S.; Robinet, F.; Rocchi, A.; Rolland, L.; Romanelli, M.; Romano, R.; Romero-Rodríguez, A.; Ronchini, S.; Rosa, L.; Rosińska, D.; Roy, S.; Rozza, D.; Ruggi, P.; Salafia, O. S.; Salconi, L.; Salemi, F.; Samajdar, A.; Sanchis-Gual, N.; Sanuy, A.; Sassolas, B.; Sayah, S.; Schmidt, S.; Seglar-Arroyo, M.; Sentenac, D.; Sequino, V.; Setyawati, Y.; Sharma, A.; Shcheblanov, N. S.; Sieniawska, M.; Singh, N.; Singha, A.; Sipala, V.; Soldateschi, J.; Sordini, V.; Sorrentino, F.; Sorrentino, N.; Soulard, R.; Spagnuolo, V.; Spera, M.; Srinivasan, R.; Stachie, C.; Steer, D. A.; Steinlechner, J.; Steinlechner, S.; Stratta, G.; Sur, A.; Swinkels, B. L.; Szewczyk, P.; Tacca, M.; Tanasijczuk, A. J.; Martín, E. N. Tapia San; Taranto, C.; Tonelli, M.; Torres-Forné, A.; Melo, I. Tosta e; Trapananti, A.; Travasso, F.; Tringali, M. C.; Troiano, L.; Trovato, A.; Trozzo, L.; Tsang, K. W.; Turbang, K.; Turconi, M.; Utina, A.; Valentini, M.; van Bakel, N.; van Beuzekom, M.; Brand, J. F. J. van den; Broeck, C. Van Den; van der Schaaf, L.; van Heijningen, J. V.; van Remortel, N.; Vardaro, M.; Vasúth, M.; Vedovato, G.; Verkindt, D.; Verma, P.; Vetrano, F.; Viceré, A.; Vinet, J. -Y.; Virtuoso, A.; Vocca, H.; Walet, R. C.; Was, M.; Zadrożny, A.; Zelenova, T.; Zendri, J. -P.

doi:10.48550/arxiv.2107.03294

Cited by 8 publications

(15 citation statements)

References 14 publications

(34 reference statements)

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“…The duty factors for this run were 76%, 71%, and 76% for L1, H1, and V1, respectively. The uncertainties on the amplitude and phase calibration of the detectors for O2 can be found in Cahillane et al (2017); Acernese et al (2018) and those for O3 can be found in Sun et al (2020Sun et al ( , 2021; Acernese et al (2021). For O2, the maximum 1σ amplitude uncertainties over the range 10-2000 Hz were between about [−2.5, +7.5]% and [−8, +4]% for H1 and L1, respectively, and for Virgo the the maximum uncertainty was 5.1%.…”

Section: Gravitational-wave Datamentioning

confidence: 98%

“…The data used underwent cleaning processes (Davis et al 2019;Viets & Wade 2021;Acernese et al 2021), specifically the removal of narrowband spectral artifacts at the calibration line frequencies and power line frequencies. A discussion on the consequences of performing a search using LIGO data with the narrowband cleaning of Viets & Wade (2021) applied compared to that without it applied can be found in Appendix A.…”

Section: Gravitational-wave Datamentioning

confidence: 99%

See 1 more Smart Citation

Searches for Gravitational Waves from Known Pulsars at Two Harmonics in the Second and Third LIGO-Virgo Observing Runs

Abbott¹,

Abe²,

Acernese³

et al. 2021

Preprint

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We present a targeted search for continuous gravitational waves (GWs) from 236 pulsars using data from the third observing run of LIGO and Virgo (O3) combined with data from the second observing run (O2). Searches were for emission from the l = m = 2 mass quadrupole mode with a frequency at only twice the pulsar rotation frequency (single harmonic) and the l = 2, m = 1, 2 modes with a frequency of both once and twice the rotation frequency (dual harmonic). No evidence of GWs was found so we present 95% credible upper limits on the strain amplitudes h 0 for the single harmonic search along with limits on the pulsars' mass quadrupole moments Q 22 and ellipticities ε. Of the pulsars studied, 23 have strain amplitudes that are lower than the limits calculated from their electromagnetically measured spin-down rates. These pulsars include the millisecond pulsars J0437−4715 and J0711−6830 which have spin-down ratios of 0.87 and 0.57 respectively. For nine pulsars, their spin-down limits have been surpassed for the first time. For the Crab and Vela pulsars our limits are factors of ∼ 100 and ∼ 20 more constraining than their spin-down limits, respectively. For the dual harmonic searches, new limits are placed on the strain amplitudes C 21 and C 22 . For 23 pulsars we also present limits on the emission amplitude assuming dipole radiation as predicted by Brans-Dicke theory.

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Section: Gravitational-wave Datamentioning

confidence: 98%

Section: Gravitational-wave Datamentioning

confidence: 99%

Searches for Gravitational Waves from Known Pulsars at Two Harmonics in the Second and Third LIGO-Virgo Observing Runs

Abbott¹,

Abe²,

Acernese³

et al. 2021

Preprint

Self Cite

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show abstract

“…We compute the percentage of injections that have a significance higher than the best event candidate and look for the amplitude at which this percentage is above 90%, which sets the upper limit. We include O3b calibration errors (Sun et al 2021;Acernese et al 2021) by jittering the amplitude and arrival time according to a Gaussian distribution representative of the calibration uncertainties. As with the modeled search, these injection sets allow us to calculate 90% exclusion distances.…”

Section: Search For Generic Gw Transientsmentioning

confidence: 99%

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift During the LIGO-Virgo Run O3b

Abbott,

Acernese

et al. 2021

Preprint

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We search for gravitational-wave signals associated with gamma-ray bursts detected by the Fermi and Swift satellites during the second half of the third observing run of Advanced LIGO and Advanced Virgo (1 November 2019 15:00 UTC-27 March 2020 17:00 UTC). We conduct two independent searches: a generic gravitational-wave transients search to analyze 86 gamma-ray bursts and an analysis to target binary mergers with at least one neutron star as short gamma-ray burst progenitors for 17 events. We find no significant evidence for gravitational-wave signals associated with any of these gammaray bursts. A weighted binomial test of the combined results finds no evidence for sub-threshold gravitational wave signals associated with this GRB ensemble either. We use several source types and signal morphologies during the searches, resulting in lower bounds on the estimated distance to each gamma-ray burst. Finally, we constrain the population of low luminosity short gamma-ray bursts using results from the first to the third observing runs of Advanced LIGO and Advanced Virgo. The resulting population is in accordance with the local binary neutron star merger rate.

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“…Obtained results indicate that the adopted methodology, based on the pytvfemd adaptive algorithm, is suitable to monitor the onset and evolution of scattered light noise, related to environmental noise variability in GW interferometers. As the source of scattered light during O3 was known to be the West end bench, this noise was mainly removed during the online noise subtraction using the relevant photodiode as a witness channel [30]. This allowed to remove the scattered light noise so that it would not significantly affect the gravitational wave strain data.…”

Section: Discussionmentioning

confidence: 99%

Daily monitoring of scattered light noise due to microseismic variability at the Virgo interferometer

Longo,

Bianchi,

Valdes

et al. 2021

Preprint

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Data acquired by the Virgo interferometer during the second part of the O3 scientific run, referred to as O3b, were analysed with the aim of characterising the onset and time evolution of scattered light noise in connection with the variability of microseismic noise in the environment surrounding the detector. The adaptive algorithm used, called pytvfemd, is suitable for the analysis of time series which are both nonlinear and nonstationary. It allowed to obtain the first oscillatory mode of the differential arm motion degree of freedom of the detector during days affected by scattered light noise. The mode's envelope i.e., its instantaneous amplitude, is then correlated with the motion of the West end bench, a known source of scattered light during O3. The relative velocity between the West end test mass and the West end optical bench is used as a predictor of scattered light noise. Higher values of correlation are obtained in periods of higher seismic noise in the microseismic frequency band. This is also confirmed by the signal-to-noise ratio (SNR) of scattered light glitches from Grav-itySpy for the January-March 2020 period. Obtained results suggest that the adopted methodology is suited for scattered light noise characterisation and monitoring in gravitational wave interferometers.

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Calibration of Advanced Virgo and reconstruction of detector strain h(t) during the Observing Run O3

Abstract: Calibration of Advanced Virgo and reconstruction of detector strain h(t) during the Observing Run O33

Cited by 8 publications

References 14 publications

Searches for Gravitational Waves from Known Pulsars at Two Harmonics in the Second and Third LIGO-Virgo Observing Runs

Searches for Gravitational Waves from Known Pulsars at Two Harmonics in the Second and Third LIGO-Virgo Observing Runs

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift During the LIGO-Virgo Run O3b

Daily monitoring of scattered light noise due to microseismic variability at the Virgo interferometer

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