Figure 45: Examples of the sum noise power (double-sided) spectral densities of the detuned
interferometer. ‘Broadband’: double optimization of the Advanced LIGO interferometer for NS-NS
inspiraling and burst sources in presence of the classical noises [93] ( ,
, , ). ‘High-frequency’: low-power configuration
suitable for detection of the GW signals from the millisecond pulsars, similar to one planned for
GEO HF [169] [ , , , ]. ‘Second-order
pole’: the regime close to the second-order pole one, which provides a maximum of the SNR
for the GW burst sources given that technical noise is smaller than the SQL [ ,
, , , ]. In all cases, and the
losses part of the bandwidth (which corresponds to the losses per
bounce in the 4 km long arms).
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