Virgo status

Acernese, F.; Alshourbagy, M.; Amico, P.; Antonucci, F.; Aoudia, S.; Arun, K. G.; Astone, P.; Avino, S.; Baggio, L; Ballardin, G.; Barone, F.; Barsotti, L.; Barsuglia, M.; Bauer, Th.; Bigotta, S.; Birindelli, S.; Bizouard, M. A.; Boccara, Claude; Bondu, F.; Bosi, L.; Braccini, S.; Bradaschia, C.; Brillet, A.; Brisson, V.; Buskulic, D.; Cagnoli, G.; Calloni, E.; Campagna, E.; Carbognani, F.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cesarini, E.; Chassande–Mottin, E.; Chatterji, S.; Cleva, F.; Coccia, E.; Corda, Christian; Corsi, A.; Cottone, F.; Coulon, J.‐P.; Cuoco, E.; D’Antonio, S.; Dari, A.; Dattilo, V.; Davier, M.; Rosa, R. De; Prete, M. Del; Fiore, L. Di; Lieto, A. Di; Emilio, M. Di Paolo; Virgilio, A. Di; Evans, M.; Fafone, V.; Ferrante, I.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Fournier, J.-D.; Frasca, S.; Frasconi, F.; Gammaitoni, L.; Garufi, F.; Genin, É.; Gennai, A.; Giazotto, A.; Granata, V.; Greverie, C.; Grosjean, Daniel; Guidi, G. M.; Hamdani, S.; Hebri, S.; Heitmann, H.; Hello, P.; Huet, D.; Penna, P. La; Laval, M.; Leroy, N.; Letendre, N.; López, B.; Lorenzini, M.; Loriette, V.; Losurdo, G.; Mackowski, J.‐M.; Majorana, E.; Man, N.; Mantovani, M.; Marchesoni, F.; Marion, F.; Marque, J.; Martelli, F.; Masserot, A.; Menzinger, F.; Milano, L.; Minenkov, Y.; Mohan, M.; Moreau, Julien; Morgado, N.; Mosca, S.; Mours, B.; Neri, I.; Nocera, F.; Pagliaroli, G.; Palomba, C.; Paoletti, F.; Pardi, S.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Piergiovanni, F.; Pinard, L.; Poggiani, R.; Punturo, M.; Puppo, P.; Rabaste, Olivier; Rapagnani, P.; Regimbau, T.; Remillieux, A.; Ricci, F.; Ricciardi, I.; Rocchi, A.; Rolland, L.; Romano, R.; Ruggi, P.; Sentenac, D.; Solimeno, S.; Swinkels, B. L.; Terenzi, R.; Toncelli, A.; Tonelli, M.; Tournefier, E.; Travasso, F.; Vajente, G.; Brand, J. van den; Putten, S. van der; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinet, J.-Y.; Vocca, H.; Yvert, M.

doi:10.1088/0264-9381/25/18/184001

Cited by 132 publications

(130 citation statements)

References 2 publications

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“…Coalescing binary compact (CBC) objects are the most promising sources of gravitational waves for the second generation of ground-based interferometric detectors, such as Advanced LIGO (AdvLIGO) [6], Advanced Virgo (AdvVIRGO) [7] and KAGRA [8], as well as for the planned third generation detectors like the Einstein Telescope (ET) [9] and the Cosmic Explorer (CE) [10]. For example, all GW150914, GW151226, GW170104 and GW170814 are coalescing binary black holes.…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave source localization for eccentric binary coalesce with a ground-based detector network

Cao

Lin

et al. 2017

Phys. Rev. D

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Gravitational wave source localization problem is important in gravitational wave astronomy. Regarding ground-based detector, almost all of the previous investigations only considered the difference of arrival time among the detector network for source localization. Within the matched filtering framework, the information beside the arrival time difference can possibly also do some help on source localization. Especially when an eccentric binary is considered, the character involved in the gravitational waveform may improve the source localization. We investigate this effect systematically in the current paper. During the investigation, the enhanced post-circular (EPC) waveform model is used to describe the eccentric binary coalesce. We find that the source localization accuracy does increase along with the eccentricity increases. But such improvement depends on the total mass of the binary. For total mass 100M binary, the source localization accuracy may be improved about 2 times in general when the eccentricity increases from 0 to 0.4. For total mass 65M binary (GW150914-like binary), the improvement factor is about 1.3 when the eccentricity increases from 0 to 0.4. For total mass 22M binary (GW151226-like binary), such improvement is ignorable.

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Section: Introductionmentioning

confidence: 99%

Gravitational wave source localization for eccentric binary coalesce with a ground-based detector network

Cao

Lin

et al. 2017

Phys. Rev. D

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“…They have been designed for the first direct detection and together with their advanced versions, presently in the preparation phase, are operated at room temperature looking at typical GW sources distant up to 100 Mpc [4], [5]. However, for an effective GW astronomy the antenna sensitivity should be increased ten-fold requesting an additional effort for the study of third generation interferometers which has just started [6].…”

Section: Introductionmentioning

confidence: 99%

A cryogenic payload for the 3rd generation of gravitational wave interferometers

Basti¹,

Frasconi²,

Majorana³

et al. 2011

Astroparticle Physics

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Thermal noise is a limiting factor of interferometric gravitational wave detectors sensitivity in the low and intermediate frequency range. A concrete possibility for beating this limit, is represented by the development of a cryogenic last stage suspension lobe integrated within a complex seismic isolation system. To this purpose a last stage payload prototype has been designed and built. It has been suspended within a dedicated cryostat with the same technique adopted for the VIRGO payload and making use of two thin wires in a cradle configuration to support a mirror made of silicon. The cooling strategy, the thermal behaviour and the system mechanical response have been deeply studied while a measurement characterization campaign has been performed both at room temperature and at cryogenic temperature. In this paper, the preliminary results obtained together with the first cooling down of the 300 kg overall mass payload at about 25 K, are reported. This study will play a driving role in the design of the third generation gravitational wave detector. (C) 2011 Elsevier B.V. All rights reserved

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“…The LIGO [2,3] and Virgo [4][5][6][7] ground-based gravitational wave observatories are currently undergoing major upgrades, and are scheduled to go back online in 2015 and 2016, respectively [8], collecting data with a sensitivity that should allow for a few up to a few tens of CBC detections per year. The exact number will depend on the actual sensitivity reached by the instrument, as well as on the formation rate of compact binary systems, which is still rather uncertain [9].…”

Section: Introductionmentioning

confidence: 99%

How serious can the stealth bias be in gravitational wave parameter estimation?

Vitale

Pozzo

2014

Phys. Rev. D

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The upcoming direct detection of gravitational waves will open a window to probing the strong-field regime of general relativity. As a consequence, waveforms that include the presence of deviations from general relativity have been developed (e.g., in the parametrized post-Einsteinian approach). TIGER, a data analysis pipeline which builds Bayesian evidence to support or question the validity of general relativity, has been written and tested. In particular, it was shown that the LIGO and Virgo detectors can probe deviations from general relativity in a regime than cannot be tested by Solar System tests or pulsar timing measurements. However, evidence from several detections is required before a deviation from general relativity can be confidently claimed. An interesting consequence is that, should general relativity not be the correct theory of gravity in its strong field regime, using standard general relativity templates for the matched filter analysis of interferometer data will introduce biases in the gravitational wave measured parameters with potentially serious consequences on the astrophysical inferences, such as the coalescence rate or the mass distribution. In this work we consider three heuristic possible deviations from general relativity and show that the biases introduced in the estimated parameters of gravitational waves emitted during the inspiral phase of spinless compact binary coalescence systems assuming the validity of general relativity manifest in various ways. The mass parameters are usually the most affected, with biases that can be as large as 30 standard deviations for the symmetric mass ratio, and nearly one percent for the chirp mass, which is usually estimated with subpercent accuracy. Other parameters do not show a significant bias. We conclude that statements about the nature of the observed sources, e.g., if both objects are neutron stars, depend critically on the explicit assumption that general relativity is the right theory of gravity in the strong field regime.

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Virgo status

Cited by 132 publications

References 2 publications

Gravitational wave source localization for eccentric binary coalesce with a ground-based detector network

Gravitational wave source localization for eccentric binary coalesce with a ground-based detector network

A cryogenic payload for the 3rd generation of gravitational wave interferometers

How serious can the stealth bias be in gravitational wave parameter estimation?

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