Advanced Virgo: a second-generation interferometric gravitational wave detector

Acernese, F.; Agathos, M.; Agatsuma, K.; Aisa, D.; Allemandou, N.; Allocca, A.; Amarni, J.; Astone, P.; Balestri, G.; Ballardin, G.; Barone, F.; Baronick, Jean-Pierre; Barsuglia, M.; Basti, A.; Basti, F.; Bauer, Th.; Bavigadda, V.; Bejger, M.; Beker, M. G.; Belczynski, C.; Bersanetti, D.; Bertolini, A.; Bitossi, M.; Bizouard, M. A.; Bloemen, S.; Blom, M.; Boër, M.; Bogaert, G.; Bondi, D.; Bondu, F.; Bonelli, L.; Bonnand, R.; Boschi, V.; Bosi, L.; Bouedo, T.; Bradaschia, C.; Branchesi, M.; Briant, T.; Brillet, A.; Brisson, V.; Bulik, T.; Bulten, H.; Buskulic, D.; Lesvigne-Buy, Christelle; Cagnoli, G.; Calloni, E.; Campeggi, C.; Canuela, B.; Carbognani, F.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cesarini, E.; Chassande–Mottin, E.; Chincarini, A.; Chiummo, A.; Chua, S.; Cleva, F.; Coccia, E.; Cohadon, P.-F.; Colla, A.; Colombini, M.; Conte, A.; Coulon, J.‐P.; Cuoco, E.; Dalmaz, A.; D’Antonio, S.; Dattilo, V.; Davier, M.; Day, R.; Debreczeni, G.; Degallaix, J.; Deléglise, S.; Pozzo, W. Del; Dereli, H.; Rosa, R. De; Fiore, L. Di; Lieto, A. Di; Virgilio, A. Di; Doets, M.; Dolique, V.; Drago, M.; Ducrot, M.; Endrőczi, G.; Fafone, V.; Farinon, S.; Ferrante, I.; Ferrini, F.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Fournier, J.-D.; Franco, S.; Frasca, S.; Frasconi, F.; Gammaitoni, L.; Garu_, F.; Gaspard, M.; Gatto, Alberto; Gemme, G.; Gendre, B.; Genin, É.; Gennai, A.; Ghosh, S.; Giacobone, L.; Giazotto, A.; Gouaty, R.; Granata, M.; Greco, G.; Groot, P.; Guidi, G. M.; Harms, J.; Heidmann, A.; Heitmann, H.; Hello, P.; Hemming, G.; Hennes, E.; Hofman, D.; Jonker, R. J. G.; Kasprzack, M.; Kraan, M.; Królak, A.; Kutynia, A.; Lazzaro, C.; Leonardi, M.; Leroy, N.; Letendre, N.; Li, T. G. F.; Lieunard, B.; Lorenzini, M.; Loriette, V.; Losurdo, G.; Majorana, E.; Maksimovic, I.; Malvezzi, V.; Man, N.; Mangano, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Marque, J.; Martelli, F.; Martinelli, L.; Masserot, A.; Meacher, D.; Meidam, J.; Mezzani, F.; Michel, C.; Milano, L.; Minenkov, Y.; Moggi, A.; Mohan, M.; Montani, M.; Mours, B.; Mul, F.; Nagy, M. F.; Nardecchia, I.; Naticchioni, L.; Nelemans, G.; Neri, I.; Néri, M.; Nocera, F.; Pacaud, E.; Palomba, C.; Paoletti, F.; Paoli, A.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Perciballi, M.; Petit, S.; Pichot, M.; Piergiovanni, F.; Pillant, G.; Piluso, A.; Pinard, L.; Poggiani, R.; Prijatelj, M.; Prodi, G. A.; Punturo, M.; Puppo, P.; Rabeling, D. S.; Rácz, István; Rapagnani, P.; Razzano, M.; Re, V.; Regimbau, T.; Ricci, F.; Robinet, F.; Rocchi, A.; Rolland, L.; Romano, R.; Ruggi, P.; Saracco, E.; Sassolas, B.; Schimmel, F.; Sentenac, D.; Sequino, V.; Shah, S.; Siellez, K.; Straniero, N.; Swinkels, B. L.; Tacca, M.; Tonelli, M.; Travasso, F.; Turconi, M.; Vajente, G.; Bakel, N. van; Beuzekom, M. van; Brand, J. van den; Broeck, C. Van Den; Sluys, Monique Van; Heijningen, J. V. van; Vasúth, M.; Vedovato, G.; Veitch, J.; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinet, J.-Y.; Visser, G.; Vocca, H.; Ward, R. L.; Was, M.; Wei, L.-W.; Yvert, M.; Zadrożny, A.; Zendri, J.-P.; Kéfélian, F.

doi:10.1088/0264-9381/32/2/024001

Cited by 3,337 publications

(2,711 citation statements)

References 70 publications

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“…Advanced LIGO recently completed its first observing period, from September 2015 to January 2016. Advanced LIGO is among a generation of planned instruments that includes GEO 600, Advanced Virgo, and KAGRA; the capabilities of this global gravitational-wave network should quickly grow over the next few years [5][6][7][8].…”

Section: Introductionmentioning

confidence: 99%

Observing gravitational-wave transient GW150914 with minimal assumptions

Abbott¹,

Cagnoli²,

Degallaix³

et al. 2016

Phys. Rev. D

155

111

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The gravitational-wave signal GW150914 was first identified on September 14, 2015, by searches for short-duration gravitational-wave transients. These searches identify time-correlated transients in multiple detectors with minimal assumptions about the signal morphology, allowing them to be sensitive to gravitational waves emitted by a wide range of sources including binary black hole mergers. Over the observational period from September 12 to October 20, 2015, these transient searches were sensitive to binary black hole mergers similar to GW150914 to an average distance of ∼600 Mpc. In this paper, we describe the analyses that first detected GW150914 as well as the parameter estimation and waveform reconstruction techniques that initially identified GW150914 as the merger of two black holes. We find that the reconstructed waveform is consistent with the signal from a binary black hole merger with a chirp mass of ∼30 M ⊙ and a total mass before merger of ∼70 M ⊙ in the detector frame.

show abstract

Section: Introductionmentioning

confidence: 99%

Observing gravitational-wave transient GW150914 with minimal assumptions

Abbott¹,

Cagnoli²,

Degallaix³

et al. 2016

Phys. Rev. D

155

111

View full text Add to dashboard Cite

show abstract

“…Recently, the LIGO Scientific Collaboration and Virgo Collaboration, based on data acquired by the Advanced LIGO [2] and Advanced Virgo [3] detectors, have announced detections of gravitational waves from coalescing stellar mass black hole binaries [4][5][6][7][8][9] and a neutron star binary [10]. This opened up the era of gravitational wave astronomy.…”

Section: Introductionmentioning

confidence: 99%

Investigating the Poor Match among Different Precessing Gravitational Waveforms

et al. 2018

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Abstract:The sixfold direct detection of gravitational waves opened the era of gravitational wave astronomy. All of these gravitational waves were emitted by black hole or neutron star binaries. The determination of the parameters characterizing compact binaries requires the accurate knowledge of waveforms. Three different waveforms (Spin Dominated, SpinTaylorT4 and Spinning Effective One Body fitted to Numerical Relativity, SEOBNR) are considered in the spin-aligned and precessing cases, in the parameter ranges where the larger spin dominates over the orbital angular momentum. The degeneracy in the parameter space of each waveform is analyzed, then the matches among the waveforms are investigated. Our results show that in the spin-aligned case only the inspiral Spin-dominated and SpinTaylorT4 waveforms agree well with each other. The highest matches of these with SEOBNR are at different parameters as compared to where SEOBNR shows the best match with itself, reflecting SEOBNR being full inspiral-merger-ringdown waveform, with coefficients fitted to numerical relativity, rather than arising from post-Newtonian (PN) calculations. In the precessing case, the matches between the pairs of all waveforms are significantly lower. We identify possible causes of this in (1) the implementation of the angular dynamics carried out at different levels of accuracy for different waveforms; (2) differences in the inclusiveness of the merger process and in the PN coefficients of the inspiral waveforms (Spin-Dominated, SpinTaylorT4) and the full SEOBNR waveform.

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“…The current network of gravitational wave detectors, comprises the two Advanced LIGO instruments [1], and GEO 600 [2] currently operating with Advanced Virgo [3] due to come on-line soon and KAGRA [4] due to start observing the next few years. These detectors are expected to be limited over most of their bandwidth by quantum noise.…”

Section: Introductionmentioning

confidence: 99%

Experimental demonstration of coupled optical springs

Gordon

Barr

Bell

et al. 2017

Class. Quantum Grav.

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Abstract. Optical rigidity will play an important role in improving the sensitivity of future generations of gravitational wave (GW) interferometers which employ high laser power in order to reach and exceed the standard quantum limit. Several experiments have demonstrated the combined effect of two optical springs on a single system for very low-weight mirror masses or membranes. In this paper we investigate the complex interactions between multiple optical springs and the surrounding apparatus in a system of comparable dynamics to a largescale GW detector. Using three 100 g mirrors to form a coupled cavity system capable of sustaining two or more optical springs, we demonstrate a number of different regimes of opto-mechanical rigidity and measurement techniques. Our measurements reveal couplings between each optical spring and the control loops that can affect both the achievable increase in sensitivity and the stability of the system. Hence this work establishes a better understanding of the realisation of the these techniques and paves the way to their application future GW observatories, such as upgrades to Advanced LIGO.

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Advanced Virgo: a second-generation interferometric gravitational wave detector

Cited by 3,337 publications

References 70 publications

Observing gravitational-wave transient GW150914 with minimal assumptions

Observing gravitational-wave transient GW150914 with minimal assumptions

Investigating the Poor Match among Different Precessing Gravitational Waveforms

Experimental demonstration of coupled optical springs

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