On the Rate of Detectability of IntermediateMass Black Hole Binaries Using LISA
Abstract
We estimate the rate at which the proposed space gravitationalwave interferometer LISA could detect intermediatemass black hole (IMBH) binaries, that is, binaries containing a black hole in the mass range 10100 M_{solar} orbiting a black hole in the mass range 1001000 M_{solar}. For 1 yr integrations leading up to the innermost stable circular orbit and a signaltonoise ratio of 10, we estimate a detection rate of only 1 per million years for 10 M_{solar}/100 M_{solar} binaries. The estimate uses the method of parameter estimation via matched filtering, incorporates a noise curve for LISA established by the LISA Science Team that is available online, and employs an IMBH formation rate model used by Miller in 2002. We find that the detectable distance is relatively insensitive to LISA arm lengths or acceleration noise but is roughly inversely proportional to LISA position errors and varies roughly as T^{1/2}, where T is the integration time in years. We also show that while all IMBH systems in this mass range may be detected in the Virgo cluster up to 40 yr before merger, none can be detected there earlier than 400 yr before merger. An extended LISA mission that enabled 10 yr integrations could detect IMBH systems at the Virgo cluster 1000 yr before merger, and systems in Galactic globular clusters 1 million yr before merger. We compare and contrast these estimates with earlier estimates by Miller.
 Publication:

The Astrophysical Journal
 Pub Date:
 August 2004
 DOI:
 10.1086/422387
 arXiv:
 arXiv:astroph/0403644
 Bibcode:
 2004ApJ...611.1080W
 Keywords:

 Black Hole Physics;
 Gravitation;
 Gravitational Waves;
 Astrophysics;
 General Relativity and Quantum Cosmology
 EPrint:
 6 pages, 3 figures, added discussion of implications of 10year LISA mission, accepted for publication in The Astrophysical Journal