The Experts below are selected from a list of 117819 Experts worldwide ranked by ideXlab platform
B P Abbott - One of the best experts on this subject based on the ideXlab platform.
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a Gravitational Wave standard siren measurement of the hubble constant
2017Co-Authors: B P Abbott, Paolo Addesso, T D Abbott, Fausto Acernese, C Adams, T Adams, K Ackley, R Abbott, R AdhikariAbstract:On 17 August 2017, the Advanced LIGO1 and Virgo2 detectors observed the Gravitational-Wave event GW170817—a strong signal from the merger of a binary neutron-star system3. Less than two seconds after the merger, a γ-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO–Virgo-derived location of the Gravitational-Wave source4, 5, 6. This sky region was subsequently observed by optical astronomy facilities7, resulting in the identification8, 9, 10, 11, 12, 13 of an optical transient signal within about ten arcseconds of the galaxy NGC 4993. This detection of GW170817 in both Gravitational Waves and electromagnetic Waves represents the first ‘multi-messenger’ astronomical observation. Such observations enable GW170817 to be used as a ‘standard siren’14, 15, 16, 17, 18 (meaning that the absolute distance to the source can be determined directly from the Gravitational-Wave measurements) to measure the Hubble constant. This quantity represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Here we report a measurement of the Hubble constant that combines the distance to the source inferred purely from the Gravitational-Wave signal with the recession velocity inferred from measurements of the redshift using the electromagnetic data. In contrast to previous measurements, ours does not require the use of a cosmic ‘distance ladder’19: the Gravitational-Wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be about 70 kilometres per second per megaparsec. This value is consistent with existing measurements20, 21, while being completely independent of them. Additional standard siren measurements from future Gravitational-Wave sources will enable the Hubble constant to be constrained to high precision.
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exploring the sensitivity of next generation Gravitational Wave detectors
2017Co-Authors: B P Abbott, Paolo Addesso, R Adhikari, V B Adya, T D Abbott, Matthew R Abernathy, C Adams, K Ackley, R Abbott, C AffeldtAbstract:The second-generation of Gravitational-Wave detectors are just starting operation, and have already yielding their first detections. Research is now concentrated on how to maximize the scientific potential of Gravitational-Wave astronomy. To support this effort, we present here design targets for a new generation of detectors, which will be capable of observing compact binary sources with high signal-to-noise ratio throughout the Universe.
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all sky search for long duration Gravitational Wave transients with initial ligo
2016Co-Authors: B P Abbott, M A Bizouard, V Brisson, Casanueva J Diaz, F Cavalier, M Davier, S Franco, P Hello, D Huet, M KasprzackAbstract:We present the results of a search for long-duration Gravitational Wave transients in two sets of data collected by the LIGO Hanford and LIGO Livingston detectors between November 5, 2005 and September 30, 2007, and July 7, 2009 and October 20, 2010, with a total observational time of 283.0 days and 132.9 days, respectively. The search targets Gravitational Wave transients of duration 10 - 500 seconds in a frequency band of 40 - 1000 Hz, with minimal assumptions about the signal Waveform, polarization, source direction, or time of occurrence. All candidate triggers were consistent with the expected background; as a result we set 90% confidence upper limits on the rate of long-duration Gravitational Wave transients for different types of Gravitational Wave signals. We also report upper limits on the source rate density per year per Mpc^3 for specific signal models. These are the first results from an all-sky search for unmodeled long-duration transient Gravitational Waves.
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ligo the laser interferometer Gravitational Wave observatory
2009Co-Authors: B P Abbott, Parameswaran Ajith, R Adhikari, R. S. Amin, G Allen, S. B. Anderson, R Abbott, W.g. AndersonAbstract:The goal of the Laser Interferometric Gravitational-Wave Observatory (LIGO) is to detect and study Gravitational Waves (GWs) of astrophysical origin. Direct detection of GWs holds the promise of testing general relativity in the strong-field regime, of providing a new probe of exotic objects such as black holes and neutron stars and of uncovering unanticipated new astrophysics. LIGO, a joint Caltech?MIT project supported by the National Science Foundation, operates three multi-kilometer interferometers at two widely separated sites in the United States. These detectors are the result of decades of worldwide technology development, design, construction and commissioning. They are now operating at their design sensitivity, and are sensitive to Gravitational Wave strains smaller than one part in 1021. With this unprecedented sensitivity, the data are being analyzed to detect or place limits on GWs from a variety of potential astrophysical sources.
R Abbott - One of the best experts on this subject based on the ideXlab platform.
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a Gravitational Wave standard siren measurement of the hubble constant
2017Co-Authors: B P Abbott, Paolo Addesso, T D Abbott, Fausto Acernese, C Adams, T Adams, K Ackley, R Abbott, R AdhikariAbstract:On 17 August 2017, the Advanced LIGO1 and Virgo2 detectors observed the Gravitational-Wave event GW170817—a strong signal from the merger of a binary neutron-star system3. Less than two seconds after the merger, a γ-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO–Virgo-derived location of the Gravitational-Wave source4, 5, 6. This sky region was subsequently observed by optical astronomy facilities7, resulting in the identification8, 9, 10, 11, 12, 13 of an optical transient signal within about ten arcseconds of the galaxy NGC 4993. This detection of GW170817 in both Gravitational Waves and electromagnetic Waves represents the first ‘multi-messenger’ astronomical observation. Such observations enable GW170817 to be used as a ‘standard siren’14, 15, 16, 17, 18 (meaning that the absolute distance to the source can be determined directly from the Gravitational-Wave measurements) to measure the Hubble constant. This quantity represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Here we report a measurement of the Hubble constant that combines the distance to the source inferred purely from the Gravitational-Wave signal with the recession velocity inferred from measurements of the redshift using the electromagnetic data. In contrast to previous measurements, ours does not require the use of a cosmic ‘distance ladder’19: the Gravitational-Wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be about 70 kilometres per second per megaparsec. This value is consistent with existing measurements20, 21, while being completely independent of them. Additional standard siren measurements from future Gravitational-Wave sources will enable the Hubble constant to be constrained to high precision.
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exploring the sensitivity of next generation Gravitational Wave detectors
2017Co-Authors: B P Abbott, Paolo Addesso, R Adhikari, V B Adya, T D Abbott, Matthew R Abernathy, C Adams, K Ackley, R Abbott, C AffeldtAbstract:The second-generation of Gravitational-Wave detectors are just starting operation, and have already yielding their first detections. Research is now concentrated on how to maximize the scientific potential of Gravitational-Wave astronomy. To support this effort, we present here design targets for a new generation of detectors, which will be capable of observing compact binary sources with high signal-to-noise ratio throughout the Universe.
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prospects for observing and localizing Gravitational Wave transients with advanced ligo and advanced virgo
2013Co-Authors: B Abbott, Paolo Addesso, T D Abbott, Fausto Acernese, C Adams, T Adams, K Ackley, R Abbott, M R Abernathy, R X AdhikariAbstract:We present a possible observing scenario for the Advanced LIGO and Advanced Virgo Gravitational-Wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with Gravitational Waves. We determine the expected sensitivity of the network to transient Gravitational-Wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for Gravitational-Wave transients, with particular focus on Gravitational-Wave signals from the inspiral of binary neutron-star systems, which are considered the most promising for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90% credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5 to 20 square degrees will require at least three detectors of sensitivity within a factor of ~2 of each other and with a broad frequency bandwidth. Should the third LIGO detector be relocated to India as expected, a significant fraction of Gravitational-Wave signals will be localized to a few square degrees by Gravitational-Wave observations alone.
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beating the spin down limit on Gravitational Wave emission from the vela pulsar
2011Co-Authors: Jerome Abadie, R X Adhikari, B Abbott, Matthew R Abernathy, T Accadia, Fausto Acernese, C Adams, R Abbott, C AffeldtAbstract:We present direct upper limits on Gravitational Wave emission from the Crab pulsar using data from the first 9 months of the fifth science run of the Laser Interferometer Gravitational-Wave Observatory (LIGO). These limits are based on two searches. In the first we assume that the Gravitational Wave emission follows the observed radio timing, giving an upper limit on Gravitational Wave emission that beats indirect limits inferred from the spin-down and braking index of the pulsar and the energetics of the nebula. In the second we allow for a small mismatch between the Gravitational and radio signal frequencies and interpret our results in the context of two possible Gravitational Wave emission mechanisms.
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ligo the laser interferometer Gravitational Wave observatory
2009Co-Authors: B P Abbott, Parameswaran Ajith, R Adhikari, R. S. Amin, G Allen, S. B. Anderson, R Abbott, W.g. AndersonAbstract:The goal of the Laser Interferometric Gravitational-Wave Observatory (LIGO) is to detect and study Gravitational Waves (GWs) of astrophysical origin. Direct detection of GWs holds the promise of testing general relativity in the strong-field regime, of providing a new probe of exotic objects such as black holes and neutron stars and of uncovering unanticipated new astrophysics. LIGO, a joint Caltech?MIT project supported by the National Science Foundation, operates three multi-kilometer interferometers at two widely separated sites in the United States. These detectors are the result of decades of worldwide technology development, design, construction and commissioning. They are now operating at their design sensitivity, and are sensitive to Gravitational Wave strains smaller than one part in 1021. With this unprecedented sensitivity, the data are being analyzed to detect or place limits on GWs from a variety of potential astrophysical sources.
Fausto Acernese - One of the best experts on this subject based on the ideXlab platform.
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a Gravitational Wave standard siren measurement of the hubble constant
2017Co-Authors: B P Abbott, Paolo Addesso, T D Abbott, Fausto Acernese, C Adams, T Adams, K Ackley, R Abbott, R AdhikariAbstract:On 17 August 2017, the Advanced LIGO1 and Virgo2 detectors observed the Gravitational-Wave event GW170817—a strong signal from the merger of a binary neutron-star system3. Less than two seconds after the merger, a γ-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO–Virgo-derived location of the Gravitational-Wave source4, 5, 6. This sky region was subsequently observed by optical astronomy facilities7, resulting in the identification8, 9, 10, 11, 12, 13 of an optical transient signal within about ten arcseconds of the galaxy NGC 4993. This detection of GW170817 in both Gravitational Waves and electromagnetic Waves represents the first ‘multi-messenger’ astronomical observation. Such observations enable GW170817 to be used as a ‘standard siren’14, 15, 16, 17, 18 (meaning that the absolute distance to the source can be determined directly from the Gravitational-Wave measurements) to measure the Hubble constant. This quantity represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Here we report a measurement of the Hubble constant that combines the distance to the source inferred purely from the Gravitational-Wave signal with the recession velocity inferred from measurements of the redshift using the electromagnetic data. In contrast to previous measurements, ours does not require the use of a cosmic ‘distance ladder’19: the Gravitational-Wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be about 70 kilometres per second per megaparsec. This value is consistent with existing measurements20, 21, while being completely independent of them. Additional standard siren measurements from future Gravitational-Wave sources will enable the Hubble constant to be constrained to high precision.
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prospects for observing and localizing Gravitational Wave transients with advanced ligo and advanced virgo
2013Co-Authors: B Abbott, Paolo Addesso, T D Abbott, Fausto Acernese, C Adams, T Adams, K Ackley, R Abbott, M R Abernathy, R X AdhikariAbstract:We present a possible observing scenario for the Advanced LIGO and Advanced Virgo Gravitational-Wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with Gravitational Waves. We determine the expected sensitivity of the network to transient Gravitational-Wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for Gravitational-Wave transients, with particular focus on Gravitational-Wave signals from the inspiral of binary neutron-star systems, which are considered the most promising for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90% credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5 to 20 square degrees will require at least three detectors of sensitivity within a factor of ~2 of each other and with a broad frequency bandwidth. Should the third LIGO detector be relocated to India as expected, a significant fraction of Gravitational-Wave signals will be localized to a few square degrees by Gravitational-Wave observations alone.
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beating the spin down limit on Gravitational Wave emission from the vela pulsar
2011Co-Authors: Jerome Abadie, R X Adhikari, B Abbott, Matthew R Abernathy, T Accadia, Fausto Acernese, C Adams, R Abbott, C AffeldtAbstract:We present direct upper limits on Gravitational Wave emission from the Crab pulsar using data from the first 9 months of the fifth science run of the Laser Interferometer Gravitational-Wave Observatory (LIGO). These limits are based on two searches. In the first we assume that the Gravitational Wave emission follows the observed radio timing, giving an upper limit on Gravitational Wave emission that beats indirect limits inferred from the spin-down and braking index of the pulsar and the energetics of the nebula. In the second we allow for a small mismatch between the Gravitational and radio signal frequencies and interpret our results in the context of two possible Gravitational Wave emission mechanisms.
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sensitivity studies for third generation Gravitational Wave observatories
2011Co-Authors: Stefan Hild, M Barsuglia, Pau Amaroseoane, Nils Andersson, K G Arun, F Barone, B Barr, Matthew R Abernathy, Fausto Acernese, M G BekerAbstract:Advanced Gravitational Wave detectors, currently under construction, are expected to directly observe Gravitational Wave signals of astrophysical origin. The Einstein Telescope (ET), a third-generation Gravitational Wave detector, has been proposed in order to fully open up the emerging field of Gravitational Wave astronomy. In this paper we describe sensitivity models for ET and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10 Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.
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sensitivity studies for third generation Gravitational Wave observatories
2011Co-Authors: Stefan Hild, M Barsuglia, Pau Amaroseoane, Nils Andersson, K G Arun, F Barone, B Barr, Matthew R Abernathy, Fausto Acernese, M G BekerAbstract:Advanced Gravitational Wave detectors, currently under construction, are expected to directly observe Gravitational Wave signals of astrophysical origin. The Einstein Telescope (ET), a third-generation Gravitational Wave detector, has been proposed in order to fully open up the emerging field of Gravitational Wave astronomy. In this paper we describe sensitivity models for ET and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10 Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.
Florent Robinet - One of the best experts on this subject based on the ideXlab platform.
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Omicron: a tool to characterize transient noise in Gravitational-Wave detectors
2020Co-Authors: Florent Robinet, Nicolas Arnaud, Nicolas Leroy, Andrew Lundgren, Duncan Macleod, Jessica MciverAbstract:The Omicron software is a tool developed to perform a multi-resolution time-frequency analysis of data from Gravitational-Wave detectors: the LIGO, Virgo, and KAGRA detectors. Omicron generates spectrograms from whitened data streams, offering a visual representation of transient detector noises and Gravitational-Wave events. In addition, these events can be parameterized with an optimized resolution. They can be written to disk to conduct offline noise characterization and Gravitational-Wave event validation studies. Omicron is optimized to process, in parallel, thousands of data streams recorded by Gravitational-Wave detectors. The Omicron software plays an important role in vetting Gravitational-Wave detection candidates and characterization of transient noise.
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information theoretic approach to the Gravitational Wave burst detection problem
2017Co-Authors: R Lynch, R C Essick, E Katsavounidis, S Vitale, Florent RobinetAbstract:The observational era of Gravitational-Wave astronomy began in the Fall of 2015 with the detection of GW150914. One potential type of detectable Gravitational Wave is short-duration Gravitational-Wave bursts, whose Waveforms can be difficult to predict. We present the framework for a new detection algorithm for such burst events -- \textit{oLIB} -- that can be used in low-latency to identify Gravitational-Wave transients independently of other search algorithms. This algorithm consists of 1) an excess-power event generator based on the Q-transform -- \textit{Omicron} --, 2) coincidence of these events across a detector network, and 3) an analysis of the coincident events using a Markov chain Monte Carlo Bayesian evidence calculator -- \textit{LALInferenceBurst}. These steps compress the full data streams into a set of Bayes factors for each event; through this process, we use elements from information theory to minimize the amount of information regarding the signal-versus-noise hypothesis that is lost. We optimally extract this information using a likelihood-ratio test to estimate a detection significance for each event. Using representative archival LIGO data, we show that the algorithm can detect Gravitational-Wave burst events of astrophysical strength in realistic instrumental noise across different burst Waveform morphologies. We also demonstrate that the combination of Bayes factors by means of a likelihood-ratio test can improve the detection efficiency of a Gravitational-Wave burst search. Finally, we show that oLIB's performance is robust against the choice of Gravitational-Wave populations used to model the likelihood-ratio test likelihoods.
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information theoretic approach to the Gravitational Wave burst detection problem
2017Co-Authors: R Lynch, R C Essick, E Katsavounidis, S Vitale, Florent RobinetAbstract:The observational era of Gravitational-Wave astronomy began in the fall of 2015 with the detection of GW150914. One potential type of detectable Gravitational Wave is short-duration Gravitational-Wave bursts, whose Waveforms can be difficult to predict. We present the framework for a detection algorithm for such burst events---oLIB---that can be used in low latency to identify Gravitational-Wave transients. This algorithm consists of (1) an excess-power event generator based on the Q transform---Omicron---, (2) coincidence of these events across a detector network, and (3) an analysis of the coincident events using a Markov chain Monte Carlo Bayesian evidence calculator---LALInferenceBurst. These steps compress the full data streams into a set of Bayes factors for each event. Through this process, we use elements from information theory to minimize the amount of information regarding the signal-versus-noise hypothesis that is lost. We optimally extract this information using a likelihood-ratio test to estimate a detection significance for each event. Using representative archival LIGO data across different burst Waveform morphologies, we show that the algorithm can detect Gravitational-Wave burst events of astrophysical strength in realistic instrumental noise. We also demonstrate that the combination of Bayes factors by means of a likelihood-ratio test can improve the detection efficiency of a Gravitational-Wave burst search. Finally, we show that oLIB's performance is robust against the choice of Gravitational-Wave populations used to model the likelihood-ratio test likelihoods.
Matthew R Abernathy - One of the best experts on this subject based on the ideXlab platform.
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exploring the sensitivity of next generation Gravitational Wave detectors
2017Co-Authors: B P Abbott, Paolo Addesso, R Adhikari, V B Adya, T D Abbott, Matthew R Abernathy, C Adams, K Ackley, R Abbott, C AffeldtAbstract:The second-generation of Gravitational-Wave detectors are just starting operation, and have already yielding their first detections. Research is now concentrated on how to maximize the scientific potential of Gravitational-Wave astronomy. To support this effort, we present here design targets for a new generation of detectors, which will be capable of observing compact binary sources with high signal-to-noise ratio throughout the Universe.
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beating the spin down limit on Gravitational Wave emission from the vela pulsar
2011Co-Authors: Jerome Abadie, R X Adhikari, B Abbott, Matthew R Abernathy, T Accadia, Fausto Acernese, C Adams, R Abbott, C AffeldtAbstract:We present direct upper limits on Gravitational Wave emission from the Crab pulsar using data from the first 9 months of the fifth science run of the Laser Interferometer Gravitational-Wave Observatory (LIGO). These limits are based on two searches. In the first we assume that the Gravitational Wave emission follows the observed radio timing, giving an upper limit on Gravitational Wave emission that beats indirect limits inferred from the spin-down and braking index of the pulsar and the energetics of the nebula. In the second we allow for a small mismatch between the Gravitational and radio signal frequencies and interpret our results in the context of two possible Gravitational Wave emission mechanisms.
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sensitivity studies for third generation Gravitational Wave observatories
2011Co-Authors: Stefan Hild, M Barsuglia, Pau Amaroseoane, Nils Andersson, K G Arun, F Barone, B Barr, Matthew R Abernathy, Fausto Acernese, M G BekerAbstract:Advanced Gravitational Wave detectors, currently under construction, are expected to directly observe Gravitational Wave signals of astrophysical origin. The Einstein Telescope (ET), a third-generation Gravitational Wave detector, has been proposed in order to fully open up the emerging field of Gravitational Wave astronomy. In this paper we describe sensitivity models for ET and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10 Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.
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sensitivity studies for third generation Gravitational Wave observatories
2011Co-Authors: Stefan Hild, M Barsuglia, Pau Amaroseoane, Nils Andersson, K G Arun, F Barone, B Barr, Matthew R Abernathy, Fausto Acernese, M G BekerAbstract:Advanced Gravitational Wave detectors, currently under construction, are expected to directly observe Gravitational Wave signals of astrophysical origin. The Einstein Telescope (ET), a third-generation Gravitational Wave detector, has been proposed in order to fully open up the emerging field of Gravitational Wave astronomy. In this paper we describe sensitivity models for ET and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10 Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.
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the einstein telescope a third generation Gravitational Wave observatory
2010Co-Authors: Michele Punturo, M Barsuglia, Nils Andersson, K G Arun, F Barone, B Barr, Matthew R Abernathy, Fausto Acernese, M G BekerAbstract:Advanced Gravitational Wave interferometers, currently under realization, will soon permit the detection of Gravitational Waves from astronomical sources. To open the era of precision Gravitational Wave astronomy, a further substantial improvement in sensitivity is required. The future space-based Laser Interferometer Space Antenna and the third-generation ground-based observatory Einstein Telescope (ET) promise to achieve the required sensitivity improvements in frequency ranges. The vastly improved sensitivity of the third generation of Gravitational Wave observatories could permit detailed measurements of the sources' physical parameters and could complement, in a multi-messenger approach, the observation of signals emitted by cosmological sources obtained through other kinds of telescopes. This paper describes the progress of the ET project which is currently in its design study phase.
