Detecting the cosmic gravitational wave background with the Big Bang Observer

By V. Corbin, N. Cornish. 2005

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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 the BBO could detect a background with Ωgw > 2.2 × 10−17.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/73a851bb49c52a9530bce6d6cb9f1f1dc731113b

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In Astronomy and Astrophysics

Citations in the corpus

Science with the space-based interferometer LISA. IV: probing inflation with gravitational waves (2016, background): “This tiny amplitude remains therefore only potentially interesting for some next-to-next-generation of space-based observatories, like Big Bang Observatory (BBO) [61] and maybe Deci-hertz Interferometer Gravitational wave Observatory (DECIGO) [62].”
Gravitational wave production by collisions: more bubbles (2008, background): “This result is especially interesting in the light of recent investigations [7, 8] that indicate that in the case of a first-order electroweak phase transition (obtained by a singlet sector [14, 15] or higher dimensional operators [16]–[18]) the peak frequency of the radiation produced is below the ”