Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published September 15, 2004 | Published
Journal Article Open

Search for small-mass black-hole dark matter with space-based gravitational wave detectors

Abstract

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-FG03-92-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 [26]. Their results are consistent with our calculations.

Attached Files

Published - SETprd04b.pdf

Files

SETprd04b.pdf
Files (113.5 kB)
Name Size Download all
md5:008752613daf344bd68ee50ab8976b80
113.5 kB Preview Download

Additional details

Created:
August 22, 2023
Modified:
October 16, 2023