Journal
PHYSICAL REVIEW D
Volume 104, Issue 2, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.104.022004
Keywords
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Funding
- NSF 's LIGO Laboratory - National Science Foundation
- Science and Technology Facilities Council (STFC) of the United Kingdom
- Max-Planck-Society (MPS)
- State of Niedersachsen/Germany
- Australian Research Council
- Italian Istituto Nazionale di Fisica Nucleare (INFN)
- French Centre National de la Recherche Scientifique (CNRS)
- Netherlands Organization for Scientific Research
- EGO consortium
- Council of Scientific and Industrial Research of India
- Department of Science and Technology, India
- ScienceAMP
- Engineering Research Board (SERB), India
- Ministry of Human Resource Development, India
- Spanish Agencia Estatal de Investigacion
- Vicepresidencia i Conselleria d'Innovacio, Recerca i Turisme
- Conselleria d'Educacio i Universitat del Govern de les Illes Balears
- Conselleria d'Innovacio, Universitats, Ciencia i Societat Digital de la Generalitat Valenciana
- National Science Centre of Poland
- Foundation for Polish Science (FNP)
- Swiss National Science Foundation (SNSF)
- Russian Foundation for Basic Research
- Russian Science Foundation
- European Commission
- European Regional Development Funds (ERDF)
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- Hungarian Scientific Research Fund (OTKA)
- French Lyon Institute of Origins (LIO)
- Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertees (ARC)
- Fonds Wetenschappelijk Onderzoek Vlaanderen (FWO), Belgium
- Paris Ile-de-France Region
- National Research, Development and Innovation Office Hungary (NKFIH)
- National Research Foundation of Korea
- Natural Science and Engineering Research Council Canada
- Canadian Foundation for Innovation (CFI)
- Brazilian Ministry of Science, Technology
- International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR)
- Research Grants Council of Hong Kong
- National Natural Science Foundation of China (NSFC)
- Leverhulme Trust
- Ministry of Science and Technology (MOST), Taiwan
- United States Department of Energy
- Kavli Foundation
- NSF
- STFC
- CNRS
- MEXT
- JSPS Leading-edge Research Infrastructure Program
- JSPS [20A203: JP20H05854]
- JSPS Core-to-Core Program A. Advanced Research Networks
- National Research Foundation (NRF) and Computing Infrastructure Project of KISTI-GSDC in Korea
- AS Grid Center (ASGC)
- Ministry of Science and Technology (MoST) in Taiwan [AS-CDA-105-M06]
- STFC [ST/V001396/1] Funding Source: UKRI
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This study reports the results of a search for an isotropic gravitational-wave background using data from advanced detectors, placing upper limits on the strength of different types of gravitational-wave backgrounds. The study also explores the potential sources of correlated noise and compares the results to a fiducial model for the gravitational-wave background. Additionally, the study demonstrates the potential of combining results from individual mergers to provide stronger constraints on the merger rate of binary black holes.
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 Omega(GW) <= 5.8 x 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; Omega(GW)(f) <= 3.4 x 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 Omega(GW)(f) <= 3.9 x 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 greater than or similar to 2 than can be achieved with individually resolved mergers alone.
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