Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO–Virgo Run O3a

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doi:10.3847/1538-4357/abee15

Cited by 32 publications

(24 citation statements)

References 139 publications

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“…The gamma and X-ray observations involved energies extending up to ∼ 1 TeV. The majority of high-energy searches reported no candidates [432,441,450,458,470,484,535,551,552].…”

Section: Appendix A: Low-latency Alert System and Multimessenger Foll...mentioning

confidence: 99%

GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run

Abbott,

Acernese

et al. 2021

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The third Gravitational-wave Transient Catalog (GWTC-3) describes signals detected with Advanced LIGO and Advanced Virgo up to the end of their third observing run. Updating the previous GWTC-2.1, we present candidate gravitational waves from compact binary coalescences during the second half of the third observing run (O3b) between 1 November 2019, 15:00 UTC and 27 March 2020, 17:00 UTC. There are 35 compact binary coalescence candidates identified by at least one of our search algorithms with a probability of astrophysical origin pastro > 0.5. Of these, 18 were previously reported as low-latency public alerts, and 17 are reported here for the first time. Based upon estimates for the component masses, our O3b candidates with pastro > 0.5 are consistent with gravitational-wave signals from binary black holes or neutron star-black hole binaries, and we identify none from binary neutron stars. However, from the gravitational-wave data alone, we are not able to measure matter effects that distinguish whether the binary components are neutron stars or black holes. The range of inferred component masses is similar to that found with previous catalogs, but the O3b candidates include the first confident observations of neutron star-black hole binaries. Including the 35 candidates from O3b in addition to those from GWTC-2.1, GWTC-3 contains 90 candidates found by our analysis with pastro > 0.5 across the first three observing runs. These observations of compact binary coalescences present an unprecedented view of the properties of black holes and neutron stars.

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“…The gamma and X-ray observations involved energies extending up to ∼ 1 TeV. The majority of high-energy searches reported no candidates [432,441,450,458,470,484,535,551,552].…”

Section: Appendix A: Low-latency Alert System and Multimessenger Foll...mentioning

confidence: 99%

GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run

Abbott,

Acernese

et al. 2021

Preprint

Self Cite

441

778

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“…Gating is used extensively in LVK analyses. Pre-whitening gating is currently used by several CBC search algorithms ( PyCBC [76], MBTA [78], PyGRB [150]) as well as a search for generic transients (X-pipeline [151]). This method has been used in low latency analyses [152] to manually mitigate loud glitches before localizing the source of gravitational-wave signals.…”

Section: Gating and Inpaintingmentioning

confidence: 99%

Detector Characterization and Mitigation of Noise in Ground-Based Gravitational-Wave Interferometers

Davis

Walker

2022

Galaxies

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Since the early stages of operation of ground-based gravitational-wave interferometers, careful monitoring of these detectors has been an important component of their successful operation and observations. Characterization of gravitational-wave detectors blends computational and instrumental methods of investigating the detector performance. These efforts focus both on identifying ways to improve detector sensitivity for future observations and understand the non-idealized features in data that has already been recorded. Alongside a focus on the detectors themselves, detector characterization includes careful studies of how astrophysical analyses are affected by different data quality issues. This article presents an overview of the multifaceted aspects of the characterization of interferometric gravitational-wave detectors, including investigations of instrumental performance, characterization of interferometer data quality, and the identification and mitigation of data quality issues that impact analysis of gravitational-wave events. Looking forward, we discuss efforts to adapt current detector characterization methods to meet the changing needs of gravitational-wave astronomy.

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“…It can be found from Figure 5 and Table 4 that it is not only SGRBs that are harder than LGRBs, but noncollapse GRBs are also significantly harder than core-collapsing ones. In particular, Figure 5 shows the comparison of these normal GRBs with some special GRBs including SN/GRBs 101219B, 100418A, 091127, 090618, 080319B, 050824, 050525A, and 050416 (Chandra & Frail 2012;); X-ray flashes (XRFs) including 060428B, 051109B, 050416A, and 050215B (Chandra & Frail 2012;); gravitational-wave (GW) associated GRBs 060614, 070923, and 170817A (Abbott et al 2017b(Abbott et al , 2021; fast radio burst (FRB)associated GRBs 100704A and 101011A (Bannister et al 2012); and GRB 090429B, with the highest redshift of z ∼ 9.4 (Cucchiara et al 2011). It can be easily seen that only GWassociated and short GRBs are consistently distributed in the log HR 32 -log T 90 plane and all other special bursts consisting of XRFs, FRB/SN-associated and high-redshift GRBs are distributed within the region of long GRBs.…”

Section: Hardness Ratiomentioning

confidence: 99%

Reclassifying Swift Gamma-Ray Bursts with Diverse Duration Distributions

Deng

Zhang

et al. 2022

ApJ

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We select the largest sample of Swift gamma-ray bursts (GRBs) so far to reexamine the classification in terms of time duration, hardness ratio, and physical collapse model. To analyze the sample selection effect, we divide the observed Swift GRB sample into four subsamples according to signal-to-noise level, spectral quality, and extended emission. First, we find that only the sample of Swift GRBs with well-measured peak energy can be evidently divided into two types at a boundary of ∼1 s, and other data sets are well described by three Gaussian functions. Using Swift GRBs with known redshift, a Kolmogorov–Smirnov test shows the intrinsic duration distributions of five data sets are equally distributed. Second, we ascertain in the plane of hardness ratio versus duration that the hardness ratio of short GRBs is significantly higher than those of middle classes and long GRBs, while the latter two components are the same in statistics, implying the so-called middle class to be artificial. Third, we apply a collapse model to discriminate the boundaries between collapse and noncollapse Swift bursts. It is interesting to find that a significant fraction, ≥30%, of Swift short GRBs could have originated from the collapsing progenitors, while all long GRBs are produced from the collapsars only. Finally, we point out that short GRBs with extended emission are the main contributors to the noncollapsar population with longer duration.

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Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO–Virgo Run O3a

Cited by 32 publications

References 139 publications

GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run

GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run

Detector Characterization and Mitigation of Noise in Ground-Based Gravitational-Wave Interferometers

Reclassifying Swift Gamma-Ray Bursts with Diverse Duration Distributions

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