Table 1: Noise power spectral densities 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 and rises steeply above a lower
cutoff . The parameters in the ET design sensitivity curve are , ,
, , , , , , , ,
, , , . (See also Figure 5.)
Table 2: The value of the (squared) distance for several values of and the
corresponding smallest match that can be expected between templates and the signal at different
values of the SNR.