Paper (*cross-listing*): gr-qc/0511145
Date: Sun, 27 Nov 2005 19:24:09 GMT (116kb)

Title: Detecting a gravitational-wave background with next-generation space
interferometers

Authors: Hideaki Kudoh, Atsushi Taruya, Takashi Hiramatsu, Yoshiaki Himemoto

Comments: 19 pages, 6 figures
\\
Future missions of gravitational-wave astronomy will be operated by
space-based interferometers, covering very wide range of frequency band. Search
for stochastic gravitational-wave backgrounds (GWBs) is one of the main target
for such missions, and we here discuss the prospects for direct measurement of
isotropic and anisotropic components of (primordial) GWBs around the frequency
0.1-10 Hz. After extending the theoretical basis for correlation analysis, we
evaluate the sensitivity and the signal-to-noise ratio for the proposed future
missions of space interferometers, like Big-Bang Observer (BBO), Deci-Hertz
Interferometer Gravitational-wave Observer (DECIGO) and recently proposed
Fabry-Perot type DECIGO. The astrophysical foregrounds which are expected at
the low frequency may be a big obstacle and significantly reduce the
signal-to-noise ratio of GWBs. As a result, minimum detectable amplitude may
reach h^2 \Omega = 10^{-15} - 10^{-16}, as long as foreground point sources are
properly subtracted. Based on the correlation analysis, we also discuss
measurement of anisotropies of GWBs. As an example, sensitivity level required
for detecting the dipole moment of GWB induced by the proper motion of our
local system is closely examined.

\\ ( http://arXiv.org/abs/gr-qc/0511145 , 116kb)