List of Tables

Table 1:
Noise power spectral densities Sh(f) of various interferometers in operation and under construction: GEO600, Initial LIGO (ILIGO), TAMA, VIRGO, Advanced LIGO (ALIGO), Einstein Telescope (ET) and LISA (instrumental noise only). For each detector the noise PSD is given in terms of a dimensionless frequency x = f∕f0 and rises steeply above a lower cutoff fs. The parameters in the ET design sensitivity curve are α = − 4.1, β = − 0.69, a0 = 186, b0 = 233, b1 = 31, b2 = − 65, b3 = 52, b4 = − 42, b5 = 10, b6 = 12, c1 = 14, c2 = − 37, c3 = 19, c4 = 27. (See also Figure 5View Image.)
Table 2:
The value of the (squared) distance dℓ2 = r2∕ρ2 for several values of P and the corresponding smallest match that can be expected between templates and the signal at different values of the SNR.