期刊
SCIENCE
卷 342, 期 6156, 页码 334-337出版社
AMER ASSOC ADVANCEMENT SCIENCE
DOI: 10.1126/science.1238012
关键词
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资金
- Commonwealth of Australia for operation
- R.N.M.'s Australian Research Council (ARC) Federation Fellowship [FF0348478]
- CSIRO
- ARC [DP0985272]
- John Stocker Postgraduate Scholarship from the Science and Industry Endowment Fund
- ARC QEII Fellowship [DP0878388]
- Australian Research Council Laureate Fellowship
- NASA
- European Research Council (ERC) for the ERC Starting Grant Beacon [279202]
- Australian Research Council [DP0985272, FF0348478] Funding Source: Australian Research Council
The formation and growth processes of supermassive black holes (SMBHs) are not well constrained. SMBH population models, however, provide specific predictions for the properties of the gravitational-wave background (GWB) from binary SMBHs in merging galaxies throughout the universe. Using observations from the Parkes Pulsar Timing Array, we constrain the fractional GWB energy density (Omega(GW)) with 95% confidence to be Omega(GW)(H-0/73 kilometers per second per megaparsec)(2) < 1.3 x 10(-9) (where H-0 is the Hubble constant) at a frequency of 2.8 nanohertz, which is approximately a factor of 6 more stringent than previous limits. We compare our limit to models of the SMBH population and find inconsistencies at confidence levels between 46 and 91%. For example, the standard galaxy formation model implemented in the Millennium Simulation Project is inconsistent with our limit with 50% probability.
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