Identification of Black-Hole Dark Matter

Details Identification of Black-Hole Dark Matter Identification of Black-Hole Dark Matter

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005idm..conf..165c&link_type=abstract

THE IDENTIFICATION OF DARK MATTER. Proceedings of the Fifth International Workshop. Held 6-10 September 2004 in Edinburgh, UK. E

Computer Science

Scientific paper

The high sensitivity of upcoming space-based gravitational wave detectors suggests the possibility that if halo dark matter were composed of primordial black holes (PBHs) with mass between 1016 g and 1020 g, the gravitational interaction with detector test masses will lead to a detectable pulse-like signal during the fly-by. For an improved version of the Laser Interferometer Space Antenna with a reduced acceleration noise at the low-end of its frequency spectrum, we find an event rate, with signal-to-noise ratios greater than 5, of ~ a few per decade involving black holes of mass ~ 1017 g. The detection rate improves significantly for second generation space based interferometers that are currently envisioned, 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 ~ 1016 g is now constrained based on the radiation released during their evaporation, the gravitational wave detectors will extend the study of PBHs to a several orders of magnitude higher masses.

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