Detecting the Cosmic Gravitational Wave Background with the Big Bang Observer

Details Detecting the Cosmic Gravitational Wave Background with the Big Bang Observer Detecting the Cosmic Gravitational Wave Background with the Big Bang Observer

Publishing date

2005-12-06

URL

arxiv.org/abs/gr-qc/0512039v1

Journals

Class.Quant.Grav. 23 (2006) 2435-2446

Science

Astronomy and Astrophysics

Field

Astrophysics

SubField

General Relativity and Quantum Cosmology

Additional info

15 pages, 12 Figures

Type

Scientific paper

Abstract

The detection of the Cosmic Microwave Background Radiation (CMB) was one of the most important cosmological discoveries of the last century. With the development of interferometric gravitational wave detectors, we may be in a position to detect the gravitational equivalent of the CMB in this century. The Cosmic Gravitational Background (CGB) is likely to be isotropic and stochastic, making it difficult to distinguish from instrument noise. The contribution from the CGB can be isolated by cross-correlating the signals from two or more independent detectors. Here we extend previous studies that considered the cross-correlation of two Michelson channels by calculating the optimal signal to noise ratio that can be achieved by combining the full set of interferometry variables that are available with a six link triangular interferometer. In contrast to the two channel case, we find that the relative orientation of a pair of coplanar detectors does not affect the signal to noise ratio. We apply our results to the detector design described in the Big Bang Observer (BBO) mission concept study and find that BBO could detect a background with $\Omega_{gw} > 2.2 \times 10^{-17}$.

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