The VIRGO Project: A wide band antenna for gravitational wave detection

Bradaschia, C.; Fabbro, R. Del; Virgilio, A. Di; Giazotto, A.; Kautzky, H.; Montelatici, V.; Passuello, D.; Brillet, A.; Crégut, O.; Hello, P.; Man, C. N.; Manh, P. T.; Marraud, A.; Shoemaker, D.; Vinet, J.-Y.; Barone, F.; Fiore, L. Di; Milano, L.; Russo, G.; Aguirregabiria, J. M.; Bel, H.; Duruisseau, J. P.; Denmat, G. Le; Tourrenc, P.; Capozzi, M.; Longo, M.; Lops, Marco; Pinto, I. M.; Rotoli, G.; Damour, Thibault; Bonazzola, S.; Marck, J. A.; Gourghoulon, Y.; Holloway, L.; Fuligni, F.; Iafolla, V.; Natale, Giovan G.

doi:10.1016/0168-9002(90)91525-g

Cited by 463 publications

(280 citation statements)

References 5 publications

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“…f o = 0.976 × 10 −20 s −3 , and (3) f o = −0.615 × 10 −30 s −4 . We see that in many cases the value of the rms error of a certain parameter does not change if we go from a model with k spindowns to a model with k + 1 spindowns.…”

Section: Dependence Of the Covariance Matrix On The Observational Parmentioning

confidence: 96%

“…Detection of gravitational waves from spinning neutron stars by currently constructed long-arm laser interferometers [1,2,3,4] is expected to provide a wealth of astrophysical information about these objects. In the first paper of this series [5] (hereafter Paper I) we introduced a model of the gravitationalwave signal from a spinning neutron star.…”

Section: Introductionmentioning

confidence: 99%

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Data analysis of gravitational-wave signals from spinning neutron stars. II. Accuracy of estimation of parameters

Jaranowski

Królak

1999

Phys. Rev. D

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We examine the accuracy of estimation of parameters of the gravitational-wave signals from spinning neutron stars that can be achieved from observations by Earth-based laser interferometers. We consider a model of the signal consisting of two narrowband components and including both phase and amplitude modulation. We calculate approximate values of the rms errors of the parameter estimators using the Fisher information matrix. We carry out extensive Monte Carlo simulations and obtain cumulative distribution functions of rms errors of astrophysically interesting parameters: amplitude of the signal, wobble angle, position of the source in the sky, frequency, and spindown coefficients. We consider both all-sky searches and directed searches. We also examine the possibility of determination of neutron star proper motion. We perform simulations for all laser-interferometric detectors that are currently under construction and for several possible lengths of the observation time and sizes of the parameter space. We find that observations of continuous gravitational-wave signals from neutron stars by laser-interferometric detectors will provide a very accurate information about their astrophysical properties. We derive several simplified models of the signal that can be used in the theoretical investigations of the data analysis schemes independently of the physical mechanisms generating the gravitational-wave signal.

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Section: Dependence Of the Covariance Matrix On The Observational Parmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

Data analysis of gravitational-wave signals from spinning neutron stars. II. Accuracy of estimation of parameters

Jaranowski

Królak

1999

Phys. Rev. D

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“…Compact object mergers are one of the most promising sources of gravitational waves for ground-based interferometric detectors like LIGO (Laser Interferometer Gravitational-wave Observatory; Abramovici et al 1992) and VIRGO (Variability of Irradiance and Gravity Oscillations; Bradaschia et al 1990). So far, most of the theoretical papers on the properties of these sources related to the gravitational-wave detections have concentrated on calculating the predicted rates (Narayan, Piran, & Shemi 1991;Phinney 1991;Kalogera et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the Binary Evolution from Chirp Mass Measurements

Bulik

Belczyński

2003

ApJ

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We estimate the observed distribution of chirp masses of compact object binaries for gravitational-wave detectors. The stellar binary evolution is modeled using the StarTrack population synthesis code. The distribution of the predicted "observed" chirp masses varies with the variation of the different parameters describing stellar binary evolution. We estimate the sensitivity of the observed distribution to the variation of these parameters, and we show which of the parameters can be constrained after observing 20, 100, and 500 compact object mergers. As a general feature of all our models, we find that the population of observed binaries is dominated by the double black hole mergers.

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“…Coalescing NS binaries are also important sources of gravitational waves that may be directly detectable by the large laser interferometers currently under construction, such as LIGO (Abramovici et al 1992; see Barish & Weiss 1999 for a recent pedagogical introduction) and VIRGO (Bradaschia et al 1990). In addition to providing a major new confirmation of Einstein's theory of general relativity (GR), including the first direct proof of the existence of black holes (see, e.g., Flanagan & Hughes 1998;Lipunov, Postnov, & Prokhorov 1997), the detection of gravitational waves from coalescing binaries at cosmological distances could provide accurate independent measurements of the Hubble constant and mean density of the Universe (Schutz 1986;Chernoff & Finn 1993;Marković 1993).…”

Section: Double Neutron Starsmentioning

confidence: 99%

The Final Fate of Coalescing Compact Binaries: From Black Hole to Planet Formation

Rasio

2001

The Neutron Star—Black Hole Connection

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Abstract. Coalescing compact binaries are thought to be involved in a wide variety of astrophysical phenomena. In particular, they are important sources of gravitational radiation for both ground-based and space-based laser-interferometer detectors, and they may be sources of supernova explosions or gamma-ray bursts. Mergers of two white dwarfs may produce neutron stars with peculiar properties, including perhaps millisecond radio pulsars sometimes accompanied by planets (as observed in PSR 1257+12). According to a widely held belief, the coalescence of two neutron stars should produce a rapidly rotating black hole surrounded by an accretion disk or torus, but this is by no means certain. This review paper focuses on the final hydrodynamic coalescence and merger of double neutron stars and double white dwarfs, and addresses the question of the nature of the final merger products.

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The VIRGO Project: A wide band antenna for gravitational wave detection

Cited by 463 publications

References 5 publications

Data analysis of gravitational-wave signals from spinning neutron stars. II. Accuracy of estimation of parameters

Data analysis of gravitational-wave signals from spinning neutron stars. II. Accuracy of estimation of parameters

Constraints on the Binary Evolution from Chirp Mass Measurements

The Final Fate of Coalescing Compact Binaries: From Black Hole to Planet Formation

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