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

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dc.contributor.authorAbbott, R.
dc.contributor.authorAbbott, T.D.
dc.contributor.authorAbraham, S.
dc.contributor.authorAcernese, F.
dc.contributor.authorAckley, K.
dc.contributor.authorAdams, A.
dc.contributor.authorAdams, C.
dc.contributor.authorAdhikari, R.X.
dc.contributor.authorAdya, V.B.
dc.contributor.authorAffeldt, C.
dc.contributor.authorAgarwal, D.
dc.contributor.authorAgathos, M.
dc.contributor.authorAgatsuma, K.
dc.contributor.authorAggarwal, N.
dc.contributor.authorAguiar, O.D.
dc.contributor.authorAiello, L.
dc.contributor.authorAin, A.
dc.contributor.authorAkutsu, T.
dc.contributor.authorAleman, K.M.
dc.contributor.authorAllen, G.
dc.contributor.authoret al.
dc.date.issued2021
dc.descriptionLIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration
dc.description.abstractWe 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 Ω(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 20– 76.6 Hz; Ω(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 Ω(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 datadriven 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.statementofresponsibilityR. Abbott ... J. Cao ... A. A. Ciobanu ... Z. J. Holmes ... C. Ingram ... J. Munch ... S.W. S. Ng ... D. J. Ottaway ... P. J. Veitch ... et al.
dc.identifier.citationPhysical Review D: Particles, Fields, Gravitation and Cosmology, 2021; 104(2):022004-1-022004-27
dc.identifier.doi10.1103/PhysRevD.104.022004
dc.identifier.issn1550-2368
dc.identifier.issn2470-0029
dc.identifier.orcidBrown, D.D. [0000-0001-7851-3939]
dc.identifier.orcidCao, H. [0000-0001-6583-6907]
dc.identifier.orcidHolmes, Z.J. [0000-0003-1311-4691]
dc.identifier.orcidIngram, C. [0000-0003-0152-3279]
dc.identifier.orcidJanssens, K. [0000-0001-8760-4429]
dc.identifier.orcidKijbunchoo, N. [0000-0002-2874-1228]
dc.identifier.orcidNg, S.W.S. [0000-0001-5843-1434]
dc.identifier.orcidOttaway, D.J. [0000-0001-6794-1591]
dc.identifier.orcidVeitch, P.J. [0000-0002-2597-435X]
dc.identifier.urihttps://hdl.handle.net/2440/132670
dc.language.isoen
dc.publisherAmerican Physical Society
dc.relation.grantARC
dc.rights© 2021 American Physical Society
dc.source.urihttps://doi.org/10.1103/physrevd.104.022004
dc.titleUpper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo's third observing run
dc.typeJournal article
pubs.publication-statusPublished

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