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1826217484927107072
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MIT
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| description |
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 are consistent with uncorrelated noise, and
therefore we place upper limits on the strength of the GWB. We find that the
dimensionless energy density $\Omega_{\rm GW}\leq 5.8\times 10^{-9}$ 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; $\leq 3.4 \times 10^{-9}$ 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 $\leq 3.9 \times
10^{-10}$ 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. We also search for a GWB arising from scalar and vector modes, which are
predicted by alternative theories of gravity; we 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.
Finally, we combine our results with observations of individual mergers andshow
that, at design sensitivity, this joint approach may yield stronger constraints
on the merger rate of binary black holes at $z \lesssim 2$ than can be achieved
with individually resolved mergers alone. [abridged]
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| first_indexed |
2024-09-23T17:04:23Z
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Article
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| id |
mit-1721.1/139690
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| institution |
Massachusetts Institute of Technology
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| language |
English
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| last_indexed |
2024-09-23T17:04:23Z
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| publishDate |
2022
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| publisher |
American Physical Society (APS)
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| record_format |
dspace
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| spelling |
mit-1721.1/1396902022-09-29T23:30:45Z Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run 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 are consistent with uncorrelated noise, and therefore we place upper limits on the strength of the GWB. We find that the dimensionless energy density $\Omega_{\rm GW}\leq 5.8\times 10^{-9}$ 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; $\leq 3.4 \times 10^{-9}$ 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 $\leq 3.9 \times 10^{-10}$ 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. We also search for a GWB arising from scalar and vector modes, which are predicted by alternative theories of gravity; we 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. Finally, we combine our results with observations of individual mergers andshow that, at design sensitivity, this joint approach may yield stronger constraints on the merger rate of binary black holes at $z \lesssim 2$ than can be achieved with individually resolved mergers alone. [abridged] 2022-01-25T14:36:04Z 2022-01-25T14:36:04Z 2021 2022-01-25T14:31:54Z Article http://purl.org/eprint/type/JournalArticle https://hdl.handle.net/1721.1/139690 2021. "Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run." Physical Review D, 104 (2). en 10.1103/PHYSREVD.104.022004 Physical Review D Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf American Physical Society (APS) APS
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| spellingShingle |
Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run
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| title |
Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run
|
| title_full |
Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run
|
| title_fullStr |
Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run
|
| title_full_unstemmed |
Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run
|
| title_short |
Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run
|
| title_sort |
upper limits on the isotropic gravitational wave background from advanced ligo and advanced virgo s third observing run
|
| url |
https://hdl.handle.net/1721.1/139690
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