6 Detection Rates

The detection of a gravitational wave signal from merging close binaries is characterized by the signal-to-noise ratio S ∕N, which depends on the binary masses, the distance to the binary, the frequency, and the noise characteristics. A pedagogical derivation of the signal-to-noise ratio and its discussion for different detectors is given, for example, in Section 8 of the review [124Jump To The Next Citation Point].

In this section we focus of two particular points: the plausible enhancement of the detection of merging binary black holes with respect to binary neutron stars and the way how absolute detection rates of binary mergings can be calculated.

 6.1 Enhancement of the detection rate for binary BH mergers
 6.2 Note on realistic calculation of the detection rates of binary mergings
 6.3 Going further

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