Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 473, Issue 1, Pages 1186-1194Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx1959
Keywords
binaries: general; galaxies: statistics
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Funding
- NASA [HST-GO-12966.003-A, HST-GO-13343.009-A]
- Division Of Physics
- Direct For Mathematical & Physical Scien [1520921, 1620638] Funding Source: National Science Foundation
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We present an empirical approach for interpreting gravitational wave signals of binary black hole mergers under the assumption that the underlying black hole population is sourced by remnants of stellar evolution. Using the observed relationship between galaxy mass and stellar metallicity, we predict the black hole count as a function of galaxy stellar mass. We show, for example, that a galaxy like the Milky Way should host millions of similar to 30 M-circle dot black holes and dwarf satellite galaxies like Draco should host similar to 100 such remnants, with weak dependence on the assumed initial mass function and stellar evolution model. Most low-mass black holes (similar to 10 M-circle dot) typically reside within massive galaxies (M-* similar or equal to 10(11) M-circle dot) while massive black holes (similar to 50 M-circle dot) typically reside within dwarf galaxies (M-* similar or equal to 10(9) M-circle dot) today. If roughly 1 per cent of black holes are involved in a binary black hole merger, then the reported merger rate densities from advanced Laser Interferometer Gravitational-Wave Observatory can be accommodated for a range of merger time-scales, and the detection of mergers with > 50 M-circle dot black holes should be expected within the next decade. Identifying the host galaxy population of the mergers provides a way to constrain both the binary neutron star or black hole formation efficiencies and the merger time-scale distributions; these events would be primarily localized in dwarf galaxies if the merger time-scale is short compared to the age of the Universe and in massive galaxies otherwise. As more mergers are detected, the prospect of identifying the host galaxy population, either directly through the detection of electromagnetic counterparts of binary neutron star mergers or indirectly through the anisotropy of the events, will become a realistic possibility.
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