Seto, Naoki and Cooray, Asantha (2004) Search for small-mass black-hole dark matter with space-based gravitational wave detectors. Physical Review D, 70 (6). Art. No. 063512. ISSN 0556-2821 http://resolver.caltech.edu/CaltechAUTHORS:SETprd04b
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If the halo dark matter were composed of primordial black holes (PBHs) with mass between 10^16 and 10^20 g, their gravitational interaction with test masses of laser interferometer may lead to a detectable pulselike signal during the fly-by. If a proof-mass noise of 3×10-15 m/s^2/Hz^1/2 down to ~10^-5 Hz is achieved by the Laser Interferometer Space Antenna, the event rate, with signal-to-noise ratios greater than 5, could become ~0.1 per decade, involving black holes of mass ~10^17 g. The detection rate could improve significantly for future space-based interferometers, though these events must be distinguished from those involving perturbations due to near-Earth asteroids. While the presence of primordial black holes below a mass of ~10^16 g is now constrained based on the radiation released during their evaporation, the gravitational-wave detectors could potentially extend the search for PBHs to several orders of magnitude higher masses.
|Additional Information:||©2004 The American Physical Society (Received 11 May 2004; published 15 September 2004) We thank members of the Caltech TAPIR group for helpful comments. This work has been supported by the Sherman Fairchild Foundation, DOE DE-FG 03-92-ER40701 at Caltech (A.C.) and NASA Grant No. NAG5-10707 (N.S.). Note added.—While this paper was under editorial review, we became aware of a similar paper on the same topic . Their results are consistent with our calculations.|
|Subject Keywords:||black holes; gravitation; gravitational wave detectors; dark matter; galaxies; gravitational waves; light interferometry|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Archive Administrator|
|Deposited On:||01 Dec 2006|
|Last Modified:||26 Dec 2012 09:20|
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