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Title:
Gravitational Wave Signal from Assembling the Lightest Supermassive Black Holes
Authors:
Holley-Bockelmann, Kelly; Micic, M.; Sigurdsson, S.
Affiliation:
AA(Vanderbilt University), AB(University of Sydney, Australia), AC(Penn State University)
Publication:
American Astronomical Society, AAS Meeting #213, #477.13; Bulletin of the American Astronomical Society, Vol. 41, p.444
Publication Date:
01/2009
Origin:
AAS
Bibliographic Code:
2009AAS...21347713H

Abstract

We use high resolution cosmological N-body simulations to study the growth of intermediate to supermassive black holes (SMBH) from redshift 49 to zero in a Local Group like volume. Our mass resolution is small enough that we can track black hole growth from the seeds of population III stars to 10 million solar mass black holes. The assembly of these lower mass black holes is particularly important because SMBHs in this mass range are the primary observable for the Laser Interferometer Space Antenna (LISA). We calculate the gravitational wave signal of each of the mergers in our volume, and find that the most common source in the LISA band from our volume consists of mergers between IMBHs and SMBHs at redshifts less than 2. This type of high mass ratio merger has not been considered before in the gravitational wave community; detection and characterization of this signal will likely require a different technique than is used for SMBH mergers or extreme mass ratio inspirals. We find that the event rate of this new LISA source depends on prescriptions for gas accretion onto the black hole as well as an accurate model of the dynamics on a galaxy scale; our best estimate yields roughly 5 events with a signal-to-noise ratio greater than 30 in the Local Group over a 5 year LISA observation -- extrapolated over the local universe yields roughly 100 events. We include preliminary results for the event rate when gravitational recoil is included.
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