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Shannon, R. M.; Ravi, V.; Coles, W. A.; Hobbs, G.; Keith, M. J.; Manchester, R. N.; Wyithe, J. S. B.; Bailes, M.; Bhat, N. D. R.; Burke-Spolaor, S.; Khoo, J.; Levin, Y.; Osłowski, S.; Sarkissian, J. M.; van Straten, W.; Verbiest, J. P. W.; Wang, J.-B.
Science (American Association for the Advancement of Science), 10/2013, Volume: 342, Issue: 6156Journal Article
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 (Ω GW ) with 95% confidence to be Ω GW (H₀/73 kilometers per second per megaparsec)² < 1.3 × 10⁻⁹ (where H₀ 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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