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. |

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