Status of Virgo

Acernese, F.; Amico, P.; Alshourbagy, M.; Aoudia, S.; Avino, S.; Babusci, D.; Ballardin, G.; Barille, Régis; Barone, F.; Barsotti, L.; Barsuglia, M.; Beauville, F.; Bizouard, M. A.; Boccara, Claude; Bondu, F.; Bosi, L.; Bradaschia, C.; Braccini, S.; Brillet, A.; Brisson, V.; Brocco, L.; Buskulic, D.; Calloni, E.; Campagna, E.; Cavalier, F.; Cavalieri, R.; Cella, G.; Chassande–Mottin, E.; Corda, Christian; Clapson, A. C.; Cleva, F.; Coulon, J.‐P.; Cuoco, E.; Dattilo, V.; Davier, M.; Rosa, R. De; Fiore, L. Di; Virgilio, A. Di; Dujardin, B.; Eleuteri, A.; Enard, D.; Ferrante, I.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Fournier, J.-D.; Frasca, S.; Frasconi, F.; Freise, A.; Gammaitoni, L.; Gennai, A.; Giazotto, A.; Giordano, G.; Giordano, L.; Gouaty, R.; Grosjean, Daniel; Guidi, G. M.; Hebri, S.; Heitmann, H.; Hello, P.; Holloway, L.; Kreckelbergh, S.; Penna, P. La; Loriette, V.; Loupias, M.; Losurdo, G.; Mackowski, J.‐M.; Majorana, E.; Man, C. N.; Mantovani, M.; Marchesoni, F.; Marion, F.; Marque, J.; Martelli, F.; Masserot, A.; Mazzoni, M.; Milano, L.; Moins, C.; Moreau, Julien; Morgado, N.; Mours, B.; Pai, A.; Palomba, C.; Paoletti, F.; Pardi, S.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Perniola, B.; Piergiovanni, F.; Pinard, L.; Poggiani, R.; Punturo, M.; Puppo, P.; Qipiani, K.; Rapagnani, P.; Reita, V.; Remillieux, A.; Ricci, F.; Ricciardi, I.; Ruggi, P.; Russo, G.; Solimeno, S.; Spallicci, A.; Stanga, R.; Taddei, R.; Tombolato, D.; Tonelli, M.; Toncelli, A.; Tournefier, E.; Travasso, F.; Vajente, G.; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinet, J.-Y.; Vocca, H.; Yvert, M.; Zhang, Zhen

doi:10.1088/0264-9381/25/11/114045

Cited by 162 publications

(130 citation statements)

References 8 publications

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“…2 If we consider h e to be the exact waveform, and h to be the difference between the model and the exact waveforms, then the model waveform will be indistinguishable from the exact if and only if h hj hi < 1. Our derivation of this condition is based on the simple one-parameter family of waveforms defined in Eq.…”

Section: A Accuracy Requirements For Measurementmentioning

confidence: 99%

“…This is a timely and important subject which has received relatively little attention in the scientific literature up to this point. Several gravitational wave detectors [1][2][3] have now achieved a high enough level of sensitivity that the first astrophysical observations are expected to occur within the next few years. The numerical relativity community has also matured to the point that several groups are now computing model gravitational waveforms for the inspiral and merger of black hole and neutron star binary systems [4][5][6][7][8][9][10][11][12][13].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Model waveform accuracy standards for gravitational wave data analysis

2008

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Model waveforms are used in gravitational wave data analysis to detect and then to measure the properties of a source by matching the model waveforms to the signal from a detector. This paper derives accuracy standards for model waveforms which are sufficient to ensure that these data analysis applications are capable of extracting the full scientific content of the data, but without demanding excessive accuracy that would place undue burdens on the model waveform simulation community. These accuracy standards are intended primarily for broadband model waveforms produced by numerical simulations, but the standards are quite general and apply equally to such waveforms produced by analytical or hybrid analytical-numerical methods.

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Section: A Accuracy Requirements For Measurementmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Model waveform accuracy standards for gravitational wave data analysis

2008

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“…The GW detectors LIGO (Abbott et al 2009a), Virgo (Acernese et al 2008) and GEO600 (Grote & the LIGO Scientific Collaboration 2008) are designed to optimally detect merger signals. These detectors have been operational intermittently during the last few years reaching their nominal design sensitivity (Abbott et al 2009b;Sengupta et al 2010; the LIGO Scientific Collaboration & the Virgo Collaboration 2010) with detection horizons of a few dozen Mpc for NS 2 and almost a hundred Mpc for BH-NS mergers (the LIGO -Virgo collaboration adopts an optimal canonical distance of 33/70Mpc; Abadie et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Detectable radio flares following gravitational waves from mergers of binary neutron stars

Nakar

Piran

2011

Nature

393

484

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The question "what is the observable electromagnetic (EM) signature of a compact binary merger?" is an intriguing one with crucial consequences to the quest for gravitational waves (GW). Compact binary mergers are prime sources of GW, targeted by current and next generation detectors. Numerical simulations have demonstrated that these mergers eject energetic sub-relativistic (or even relativistic) outflows. This is certainly the case if the mergers produce short GRBs, but even if not, significant outflows are expected. The interaction of such outflows with the surround matter inevitably leads to a long lasting radio signal. We calculate the expected signal from these outflows (our calculations are also applicable to short GRB orphan afterglows) and we discuss their detectability. We show that the optimal search for such signal should, conveniently, take place around 1.4 GHz. Realistic estimates of the outflow parameters yield signals of a few hundred µJy, lasting a few weeks, from sources at the detection horizon of advanced GW detectors. Followup radio observations, triggered by GW detection, could reveal the radio remnant even under unfavorable conditions. Upcoming all sky surveys can detect a few dozen, and possibly even thousands, merger remnants at any give time, thereby providing robust merger rate estimates even before the advanced GW detectors become operational. In fact, the radio transient RT 19870422 fits well the overall properties predicted by our model and we suggest that its most probable origin is a compact binary merger radio remnant.

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“…Over the past decade, LIGO has built three such multi-kilometre interferometers, at two locations 2 : H1 (4 km) and H2 (2 km) share the same facility at Hanford, Washington, USA, and L1 (4 km) is located in Livingston Parish, Louisiana, USA. LIGO, together with the 3 km interferometer Virgo 19 in Italy and GEO 20 in Germany, forms a network of gravitational-wave observatories. LIGO has completed science run S5 (between 5 November 2005 and 30 September 2007), acquiring one year of data coincident among H1, H2 and L1, at the interferometer design sensitivities (Fig.…”

mentioning

confidence: 99%

An upper limit on the stochastic gravitational-wave background of cosmological origin

Abbott¹,

Abbott²,

Acernese³

et al. 2009

Nature

313

154

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A stochastic background of gravitational waves is expected to arise from a superposition of a large number of unresolved gravitational-wave sources of astrophysical and cosmological origin. It should carry unique signatures from the earliest epochs in the evolution of the Universe, inaccessible to standard astrophysical observations(1). Direct measurements of the amplitude of this background are therefore of fundamental importance for understanding the evolution of the Universe when it was younger than one minute. Here we report limits on the amplitude of the stochastic gravitational-wave background using the data from a two-year science run of the Laser Interferometer Gravitational-wave Observatory(2) (LIGO). Our result constrains the energy density of the stochastic gravitational-wave background normalized by the critical energy density of the Universe, in the frequency band around 100 Hz, to be <6.9 X 10(-6) at 95% confidence. The data rule out models of early Universe evolution with relatively large equation-of-state parameter(3), as well as cosmic (super) string models with relatively small string tension(4) that are favoured in some string theory models(5). This search for the stochastic background improves on the indirect limits from Big Bang nucleosynthesis(1,6) and cosmic microwave background(7) at 100Hz

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Status of Virgo

Cited by 162 publications

References 8 publications

Model waveform accuracy standards for gravitational wave data analysis

Model waveform accuracy standards for gravitational wave data analysis

Detectable radio flares following gravitational waves from mergers of binary neutron stars

An upper limit on the stochastic gravitational-wave background of cosmological origin

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