We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ... more We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ray repeater (SGR) bursts. This is the first search sensitive to neutron star f modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806À20 and 190 lesser events from SGR 1806À20 and SGR 1900þ14. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on transient GW amplitudes published to date. We find upper limit estimates on the model-dependent isotropic GW emission energies (at a nominal distance of 10 kpc) between 3 Â 10 45 and 9 Â 10 52 erg depending on waveform type, detector antenna factors and noise characteristics at the time of the burst. These upper limits are within the theoretically predicted range of some SGR models.
We report on a search for gravitational-wave bursts in data from the three LIGO interferometric d... more We report on a search for gravitational-wave bursts in data from the three LIGO interferometric detectors during their third science run. The search targets subsecond bursts in the frequency range 100-1100 Hz for which no waveform model is assumed and has a sensitivity in terms of the root-sum-square (rss) strain amplitude of h rss ∼ 10 −20 Hz −1/2. No gravitational-wave signals were detected in the eight days of analysed data.
Gravitational wave bursts are short duration perturbations of the spacetime metric due to such ca... more Gravitational wave bursts are short duration perturbations of the spacetime metric due to such catastrophic astrophysical events as supernova core collapses [1] or the merger and ringdown phases of binary black hole coalescences [2, 3]. Over the past decade, the search for these signals has been independently performed by individual detectors or by homogeneous networks of resonant bars [4] or laser interferometers [5–9]. The first coincident burst analysis between interferometers with different broadband sensitivity and ...
Currently, there is a worldwide network of kilometer scale interferometric gravitational wave det... more Currently, there is a worldwide network of kilometer scale interferometric gravitational wave detectors that are either at or approaching their respective design sensitivities. The network includes the US Laser Interferometer Gravitational-wave Observatory (LIGO)[1, 2], the British-German GEO600 [3], and the French-Italian Virgo [4]. The radiation emitted during the inspiral stage of a stellar mass compact binary system is thought to be a likely candidate for the first direct detection of gravitational waves using these interferometers [5, 6]. The initial ...
One of the signals targeted by the current generation of ground-based gravitational-wave (GW) det... more One of the signals targeted by the current generation of ground-based gravitational-wave (GW) detectors is a stochastic gravitational-wave background (SGWB)[1–3]. Such a background is analogous to the cosmic microwave background, although the dominant contribution is unlikely to have a blackbody spectrum. A SGWB can be characterized as cosmological or astrophysical in origin. Cosmological backgrounds can arise from, for example, pre-big-bang models [4–6], amplification of quantum vacuum fluctuations during ...
We search for coincident gravitational wave signals from inspiralling neutron star binaries using... more We search for coincident gravitational wave signals from inspiralling neutron star binaries using LIGO and TAMA300 data taken during early 2003. Using a simple trigger exchange method, we perform an intercollaboration coincidence search during times when TAMA300 and only one of the LIGO sites were operational. We find no evidence of any gravitational wave signals. We place an observational upper limit on the rate of binary neutron star coalescence with component masses between 1 and 3M of 49 per year uCurrently at ...
Continuous gravitational signals emitted by rotating neutron stars are promising sources for inte... more Continuous gravitational signals emitted by rotating neutron stars are promising sources for interferometric gravitational-wave detectors such as GEO600 [1, 2], the Laser Interferometer Gravitational-Wave Observatory (LIGO)[3, 4], TAMA300 [5] and VIRGO [6]. There are several physical mechanisms which might cause a neutron star to emit periodic gravitational waves. The main possibilities considered in the literature are (i) nonaxisymmetric distortions of the solid part of the star [7–10],(ii) unstable r modes in the fluid [7, 11, 12], and (iii) free ...
We report on a search for gravitational-wave bursts in data from the three LIGO interferometric d... more We report on a search for gravitational-wave bursts in data from the three LIGO interferometric detectors during their third science run. The search targets subsecond bursts in the frequency range 100–1100 Hz for which no waveform model is assumed and has a sensitivity in terms of the root-sum-square (rss) strain amplitude of hrss∼ 10− 20 Hz− 1/2. No gravitational-wave signals were detected in the eight days of analysed data.
We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ... more We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ray repeater (SGR) bursts. This is the first search sensitive to neutron star f modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806À20 and 190 lesser events from SGR 1806À20 and SGR 1900þ14. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on ...
The Laser Interferometer Gravitational-Wave Observatory has performed a third science run with mu... more The Laser Interferometer Gravitational-Wave Observatory has performed a third science run with much improved sensitivities of all three interferometers. We present an analysis of approximately 200 hours of data acquired during this run, used to search for a stochastic background of gravitational radiation. We place upper bounds on the energy density stored as gravitational radiation for three different spectral power laws. For the flat spectrum, our limit of 0< 8: 4 10ÿ4 in the 69–156 Hz band is 105 times lower than the previous result in ...
We report on a search for gravitational waves from the coalescence of compact binaries during the... more We report on a search for gravitational waves from the coalescence of compact binaries during the third and fourth LIGO science runs. The search focused on gravitational waves generated during the inspiral phase of the binary evolution. In our analysis, we considered three categories of compact binary systems, ordered by mass:(i) primordial black hole binaries with masses in the range 0: 35M< m1, m2< 1: 0M,(ii) binary neutron stars with masses in the range 1: 0M< m1, m2< 3: 0M, and (iii) binary black holes with masses in the ...
The Laser Interferometer Gravitational-Wave Observatory (LIGO) has performed the fourth science r... more The Laser Interferometer Gravitational-Wave Observatory (LIGO) has performed the fourth science run, S4, with significantly improved interferometer sensitivities with respect to previous runs. Using data acquired during this science run, we place a limit on the amplitude of a stochastic background of gravitational waves. For a frequency independent spectrum, the new Bayesian 90% upper limit is Ω GW× 2< 6.5× 10-5. This is currently the most sensitive result in the frequency range 51–150 Hz, with a factor of 13 improvement ...
The fourth science run of the LIGO and GEO 600 gravitational-wave detectors, carried out in early... more The fourth science run of the LIGO and GEO 600 gravitational-wave detectors, carried out in early 2005, collected data with significantly lower noise than previous science runs. We report on a search for short-duration gravitationalwave bursts with arbitrary waveform in the 64-1600 Hz frequency range appearing in all three LIGO interferometers. Signal consistency tests, data quality cuts, and auxiliary-channel vetoes are applied to reduce the rate of spurious triggers. No gravitational-wave signals are detected in 15.5 days of live observation time; we set a frequentist upper limit of 0.15 per day (at 90% confidence level) on the rate of bursts with large enough amplitudes to be detected reliably. The amplitude sensitivity of the search, characterized using Monte Carlo simulations, is several times better than that of previous searches. We also provide rough estimates of the distances at which representative supernova and binary black hole merger signals could be detected with 50% efficiency by this analysis.
We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ... more We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ray repeater (SGR) bursts. This is the first search sensitive to neutron star f modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806À20 and 190 lesser events from SGR 1806À20 and SGR 1900þ14. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on transient GW amplitudes published to date. We find upper limit estimates on the model-dependent isotropic GW emission energies (at a nominal distance of 10 kpc) between 3 Â 10 45 and 9 Â 10 52 erg depending on waveform type, detector antenna factors and noise characteristics at the time of the burst. These upper limits are within the theoretically predicted range of some SGR models.
We report on a search for gravitational-wave bursts in data from the three LIGO interferometric d... more We report on a search for gravitational-wave bursts in data from the three LIGO interferometric detectors during their third science run. The search targets subsecond bursts in the frequency range 100-1100 Hz for which no waveform model is assumed and has a sensitivity in terms of the root-sum-square (rss) strain amplitude of h rss ∼ 10 −20 Hz −1/2. No gravitational-wave signals were detected in the eight days of analysed data.
Gravitational wave bursts are short duration perturbations of the spacetime metric due to such ca... more Gravitational wave bursts are short duration perturbations of the spacetime metric due to such catastrophic astrophysical events as supernova core collapses [1] or the merger and ringdown phases of binary black hole coalescences [2, 3]. Over the past decade, the search for these signals has been independently performed by individual detectors or by homogeneous networks of resonant bars [4] or laser interferometers [5–9]. The first coincident burst analysis between interferometers with different broadband sensitivity and ...
Currently, there is a worldwide network of kilometer scale interferometric gravitational wave det... more Currently, there is a worldwide network of kilometer scale interferometric gravitational wave detectors that are either at or approaching their respective design sensitivities. The network includes the US Laser Interferometer Gravitational-wave Observatory (LIGO)[1, 2], the British-German GEO600 [3], and the French-Italian Virgo [4]. The radiation emitted during the inspiral stage of a stellar mass compact binary system is thought to be a likely candidate for the first direct detection of gravitational waves using these interferometers [5, 6]. The initial ...
One of the signals targeted by the current generation of ground-based gravitational-wave (GW) det... more One of the signals targeted by the current generation of ground-based gravitational-wave (GW) detectors is a stochastic gravitational-wave background (SGWB)[1–3]. Such a background is analogous to the cosmic microwave background, although the dominant contribution is unlikely to have a blackbody spectrum. A SGWB can be characterized as cosmological or astrophysical in origin. Cosmological backgrounds can arise from, for example, pre-big-bang models [4–6], amplification of quantum vacuum fluctuations during ...
We search for coincident gravitational wave signals from inspiralling neutron star binaries using... more We search for coincident gravitational wave signals from inspiralling neutron star binaries using LIGO and TAMA300 data taken during early 2003. Using a simple trigger exchange method, we perform an intercollaboration coincidence search during times when TAMA300 and only one of the LIGO sites were operational. We find no evidence of any gravitational wave signals. We place an observational upper limit on the rate of binary neutron star coalescence with component masses between 1 and 3M of 49 per year uCurrently at ...
Continuous gravitational signals emitted by rotating neutron stars are promising sources for inte... more Continuous gravitational signals emitted by rotating neutron stars are promising sources for interferometric gravitational-wave detectors such as GEO600 [1, 2], the Laser Interferometer Gravitational-Wave Observatory (LIGO)[3, 4], TAMA300 [5] and VIRGO [6]. There are several physical mechanisms which might cause a neutron star to emit periodic gravitational waves. The main possibilities considered in the literature are (i) nonaxisymmetric distortions of the solid part of the star [7–10],(ii) unstable r modes in the fluid [7, 11, 12], and (iii) free ...
We report on a search for gravitational-wave bursts in data from the three LIGO interferometric d... more We report on a search for gravitational-wave bursts in data from the three LIGO interferometric detectors during their third science run. The search targets subsecond bursts in the frequency range 100–1100 Hz for which no waveform model is assumed and has a sensitivity in terms of the root-sum-square (rss) strain amplitude of hrss∼ 10− 20 Hz− 1/2. No gravitational-wave signals were detected in the eight days of analysed data.
We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ... more We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ray repeater (SGR) bursts. This is the first search sensitive to neutron star f modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806À20 and 190 lesser events from SGR 1806À20 and SGR 1900þ14. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on ...
The Laser Interferometer Gravitational-Wave Observatory has performed a third science run with mu... more The Laser Interferometer Gravitational-Wave Observatory has performed a third science run with much improved sensitivities of all three interferometers. We present an analysis of approximately 200 hours of data acquired during this run, used to search for a stochastic background of gravitational radiation. We place upper bounds on the energy density stored as gravitational radiation for three different spectral power laws. For the flat spectrum, our limit of 0< 8: 4 10ÿ4 in the 69–156 Hz band is 105 times lower than the previous result in ...
We report on a search for gravitational waves from the coalescence of compact binaries during the... more We report on a search for gravitational waves from the coalescence of compact binaries during the third and fourth LIGO science runs. The search focused on gravitational waves generated during the inspiral phase of the binary evolution. In our analysis, we considered three categories of compact binary systems, ordered by mass:(i) primordial black hole binaries with masses in the range 0: 35M< m1, m2< 1: 0M,(ii) binary neutron stars with masses in the range 1: 0M< m1, m2< 3: 0M, and (iii) binary black holes with masses in the ...
The Laser Interferometer Gravitational-Wave Observatory (LIGO) has performed the fourth science r... more The Laser Interferometer Gravitational-Wave Observatory (LIGO) has performed the fourth science run, S4, with significantly improved interferometer sensitivities with respect to previous runs. Using data acquired during this science run, we place a limit on the amplitude of a stochastic background of gravitational waves. For a frequency independent spectrum, the new Bayesian 90% upper limit is Ω GW× 2< 6.5× 10-5. This is currently the most sensitive result in the frequency range 51–150 Hz, with a factor of 13 improvement ...
The fourth science run of the LIGO and GEO 600 gravitational-wave detectors, carried out in early... more The fourth science run of the LIGO and GEO 600 gravitational-wave detectors, carried out in early 2005, collected data with significantly lower noise than previous science runs. We report on a search for short-duration gravitationalwave bursts with arbitrary waveform in the 64-1600 Hz frequency range appearing in all three LIGO interferometers. Signal consistency tests, data quality cuts, and auxiliary-channel vetoes are applied to reduce the rate of spurious triggers. No gravitational-wave signals are detected in 15.5 days of live observation time; we set a frequentist upper limit of 0.15 per day (at 90% confidence level) on the rate of bursts with large enough amplitudes to be detected reliably. The amplitude sensitivity of the search, characterized using Monte Carlo simulations, is several times better than that of previous searches. We also provide rough estimates of the distances at which representative supernova and binary black hole merger signals could be detected with 50% efficiency by this analysis.
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