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.)
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.
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