Upper limits on the isotropic gravitational-wave background from advanced LIGO and advanced Virgo's third observing run

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dc.contributor.author Roy, Soumen
dc.contributor.author Sengupta, Anand S. et al.
dc.coverage.spatial United States of America
dc.date.accessioned 2012-09-29T14:45:09Z
dc.date.available 2012-09-29T14:45:09Z
dc.date.issued 2021-07
dc.identifier.citation Roy, Soumen and Sengupta, Anand S. et al., "Upper limits on the isotropic gravitational-wave background from advanced LIGO and advanced Virgo's third observing run", Physical Review D, DOI: 10.1103/PhysRevD.104.022004, vol. 104, no. 2, Jul. 2021. en_US
dc.identifier.issn 470-0010
dc.identifier.issn 2470-0029
dc.identifier.uri https://doi.org/10.1103/PhysRevD.104.022004
dc.identifier.uri https://repository.iitgn.ac.in/handle/123456789/6785
dc.description.abstract We report results of a search for an isotropic gravitational-wave background (GWB) using data from Advanced LIGO's and Advanced Virgo's third observing run (O3) combined with upper limits from the earlier O1 and O2 runs. Unlike in previous observing runs in the advanced detector era, we include Virgo in the search for the GWB. The results of the search are consistent with uncorrelated noise, and therefore we place upper limits on the strength of the GWB. We find that the dimensionless energy density ? GW ? 5.8 � 10 ? 9 at the 95% credible level for a flat (frequency-independent) GWB, using a prior which is uniform in the log of the strength of the GWB, with 99% of the sensitivity coming from the band 200-76.6 Hz; ? GW ( f ) ? 3.4 � 10 ? 9 at 25 Hz for a power-law GWB with a spectral index of 2 / 3 (consistent with expectations for compact binary coalescences), in the band 20�90.6 Hz; and ? GW ( f ) ? 3.9 � 10 ? 10 at 25 Hz for a spectral index of 3, in the band 20�291.6 Hz. These upper limits improve over our previous results by a factor of 6.0 for a flat GWB, 8.8 for a spectral index of 2 / 3 , and 13.1 for a spectral index of 3. We also search for a GWB arising from scalar and vector modes, which are predicted by alternative theories of gravity; we do not find evidence of these, and place upper limits on the strength of GWBs with these polarizations. We demonstrate that there is no evidence of correlated noise of magnetic origin by performing a Bayesian analysis that allows for the presence of both a GWB and an effective magnetic background arising from geophysical Schumann resonances. We compare our upper limits to a fiducial model for the GWB from the merger of compact binaries, updating the model to use the most recent data-driven population inference from the systems detected during O3a. Finally, we combine our results with observations of individual mergers and show that, at design sensitivity, this joint approach may yield stronger constraints on the merger rate of binary black holes at z ? 2 than can be achieved with individually resolved mergers alone.
dc.description.statementofresponsibility by Soumen Roy and Anand S. Sengupta et al.
dc.format.extent vol. 104, no. 2
dc.language.iso en_US en_US
dc.publisher American Physical Society en_US
dc.subject Gravitational wave detection en_US
dc.subject Gravitation en_US
dc.subject Cosmology en_US
dc.subject Astrophysics en_US
dc.title Upper limits on the isotropic gravitational-wave background from advanced LIGO and advanced Virgo's third observing run en_US
dc.type Article en_US
dc.relation.journal Physical Review D


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