The present status of the VIRGO Central Interferometer*

Acernese, F.; Amico, P.; Arnaud, N.; Arnault, C.; Babusci, D.; Ballardin, G.; Barone, F.; Barsuglia, M.; Bellachia, F.; Béney, J.L.; Bilhaut, R.; Bizouard, M. A.; Boccara, Claude; Boget, D.; Bondu, F.; Bourgoin, C.; Bozzi, A.; Bracci, L.; Braccini, S.; Bradaschia, C.; Brillet, A.; Brisson, V.; Buskulic, D.; Cachenaut, J.; Calamai, G.; Calloni, E.; Canitrot, P.; Caron, Bernard; Casciano, C.; Cattuto, Ciro; Cavalier, F.; Cavaliere, Sergio; Cavalieri, R.; Cecchi, Roberto; Cella, G.; Chiche, R.; Chollet, F.; Cleva, F.; Cokelaer, Thomas; Cortese, S.; Coulon, J.‐P.; Cuoco, E.; Cuzon, S.; Dattilo, V.; David, P.Y.; Davier, M.; Rosa, M. De; Rosa, R. De; Dehamme, M.; Fiore, L. Di; Virgilio, A. Di; Dominici, P.; Dufournaud, D.; Eder, C.; Eleuteri, A.; Enard, D.; Errico, Angela; Evangelista, Gianpaolo; Fabbroni, L.; Fang, Hua; Ferrante, I.; Fidecaro, F.; Flaminio, R.; Fournier, J.-D.; Fournier, L.; Frasca, S.; Frasconi, F.; Gammaitoni, L.; Ganau, P.; Garufi, F.; Gaspard, M.; Gennaro, G. Di; Giacobone, L.; Giazotto, A.; Giordano, G.; Girard, C.; Guidi, G. M.; Heitmann, H.; Hello, P.; Hermel, R.; Heusse, P.; Holloway, L.; Iannarelli, M.; Innocent, J. M.; Jules, E.; Penna, P. La; Lacotte, J.C.; Lagrange, B.; Leliboux, M.; Lieunard, B.; Lodygenski, O.; Lomtadze, T.; Loriette, V.; Losurdo, G.; Loupias, M.; Mackowski, J.‐M.; Majorana, E.; Man, C. N.; Mansoux, B.; Marchesoni, F.; Marin, Pierre; Marion, F.; Marrucho, J. C.; Martelli, F.; Masserot, A.; Massonnet, L.; Mataguez, S.; Mazzoni, M.; Mencik, M.; Michel, C.; Milano, L.; Montorio, J.-L.; Morgado, N.; Mours, B.; Mugnier, P.; Nicolosi, L.; Pacheco, José Antonio Freitas; Palomba, C.; Paoletti, F.; Paoli, A.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Perciballi, M.; Pinard, L.; Poggiani, R.; Popolizio, P.; Pradier, T.; Punturo, M.; Puppo, P.; Qipiani, K.; Ramonet, J.; Rapagnani, P.; Reboux, A.; Regimbau, T.; Reita, V.; Remillieux, A.; Ricci, F.; Richard, Frédéric; Ripepe, Maurizio; Rivoirard, P.; Roger, Jean Paul; Scheidecker, J. P.; Solimeno, S.; Sottile, R.; Stanga, R.; Taddei, R.; Taurigna, M.; Teuler, J. M.; Tourrenc, P.; Trinquet, H.; Turri, E.; Varvella, M.; Verkindt, D.; Vetrano, F.; Véziant, O.; Viceré, A.; Vinet, J.-Y.; Vocca, H.; Yvert, M.; Zhang, Z.

doi:10.1088/0264-9381/19/7/325

Cited by 85 publications

(31 citation statements)

References 9 publications

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“…We show in appendix B (to lowest order in the uncertainties of C lm and D lm ) that the overlaps quoted in table 2 are upper bounds. We also derive lower bounds for these overlaps there, which are smaller than the values given in table 2 by about 12/(π N cyc ) 2 . So these lower bounds are about 0.02 smaller than the table 2 values for the m = 2 modes, and 0.002 smaller for the m = 6 modes.…”

Section: Waveform Comparisonsmentioning

confidence: 72%

Reducing Orbital Eccentricity in Binary Black Hole Simulations

Pfeiffer

Brown

Kidder

et al. 2008

The Eleventh Marcel Grossmann Meeting

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Binary black hole simulations starting from quasi-circular (i.e., zero radial velocity) initial data have orbits with small but nonzero orbital eccentricities. In this paper, the quasi-equilibrium initial-data method is extended to allow nonzero radial velocities to be specified in binary black hole initial data. New low-eccentricity initial data are obtained by adjusting the orbital frequency and radial velocities to minimize the orbital eccentricity, and the resulting (∼5 orbit) evolutions are compared with those of quasi-circular initial data. Evolutions of the quasi-circular data clearly show eccentric orbits, with eccentricity that decays over time. The precise decay rate depends on the definition of eccentricity; if defined in terms of variations in the orbital frequency, the decay rate agrees well with the prediction of Peters (1964 Phys. Rev. 136 1224. The gravitational waveforms, which contain ∼8 cycles in the dominant l = m = 2 mode, are largely unaffected by the eccentricity of the quasi-circular initial data. The overlap between the dominant mode in the quasi-circular evolution and the same mode in the low-eccentricity evolution is about 0.99.

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Section: Waveform Comparisonsmentioning

confidence: 72%

Reducing Orbital Eccentricity in Binary Black Hole Simulations

Pfeiffer

Brown

Kidder

et al. 2008

The Eleventh Marcel Grossmann Meeting

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show abstract

“…The first generation interferometric gravitational-wave detectors, such as LIGO [43,44], GEO600 [45], and VIRGO [46,47], are now operating at or near their design sensitivities. Furthermore, the advanced generation of detectors are entering their construction phases.…”

Section: Introductionmentioning

confidence: 99%

High-accuracy comparison of numerical relativity simulations with post-Newtonian expansions

et al. 2007

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Numerical simulations of 15 orbits of an equal-mass binary black-hole system are presented. Gravitational waveforms from these simulations, covering more than 30 cycles and ending about 1.5 cycles before merger, are compared with those from quasicircular zero-spin post-Newtonian (PN) formulae. The cumulative phase uncertainty of these comparisons is about 0.05 radians, dominated by effects arising from the small residual spins of the black holes and the small residual orbital eccentricity in the simulations. Matching numerical results to PN waveforms early in the run yields excellent agreement (within 0.05 radians) over the first 15 cycles, thus validating the numerical simulation and establishing a regime where PN theory is accurate. In the last 15 cycles to merger, however, generic time-domain Taylor approximants build up phase differences of several radians. But, apparently by coincidence, one specific post-Newtonian approximant, TaylorT4 at 3.5PN order, agrees much better with the numerical simulations, with accumulated phase differences of less than 0.05 radians over the 30-cycle waveform. Gravitational-wave amplitude comparisons are also done between numerical simulations and postNewtonian, and the agreement depends on the post-Newtonian order of the amplitude expansion: the amplitude difference is about 6%-7% for zeroth order and becomes smaller for increasing order. A newly derived 3.0PN amplitude correction improves agreement significantly ( < 1% amplitude difference throughout most of the run, increasing to 4% near merger) over the previously known 2.5PN amplitude terms.

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“…There is one four kilometer instrument at each of the LIGO-Hanford site in Washington State [54] and LIGO-Livingston site in Louisiana [55] (H1 and L1 respectively), and a two kilometer instrument, housed in the same enclosure, at the LIGO-Hanford Observatory (H2). The other interferometers are the three kilometer Virgo instrument, built in Italy by a French-Italian collaboration [56], the 600 meter German-English Observatory (GEO600) in Germany [57], and the TAMA observatory, a 300 meter instrument located in and funded by Japan [58].…”

Section: Gravitational Wave Detectorsmentioning

confidence: 99%

Searches for Gravitational Waves from Binary Neutron Stars: A Review

Anderson

Creighton

2008

Astrophysics and Space Science Library

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Summary.A new generation of observatories is looking for gravitational waves. These waves, emitted by highly relativistic systems, will open a new window for observation of the cosmos when they are detected. Among the most promising sources of gravitational waves for these observatories are compact binaries in the final minutes before coalescence. In this article, we review in brief interferometric searches for gravitational waves emitted by neutron star binaries, including the theory, instrumentation and methods. No detections have been made to date. However, the best direct observational limits on coalescence rates have been set, and instrumentation and analysis methods continue to be refined toward the ultimate goal of defining the new field of gravitational wave astronomy.

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The present status of the VIRGO Central Interferometer*

Cited by 85 publications

References 9 publications

Reducing Orbital Eccentricity in Binary Black Hole Simulations

Reducing Orbital Eccentricity in Binary Black Hole Simulations

High-accuracy comparison of numerical relativity simulations with post-Newtonian expansions

Searches for Gravitational Waves from Binary Neutron Stars: A Review

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