Figure 45

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] (J = JaLIGO ≡ (2π × 100)3 s−3, Γ = 3100 s−1, β = 0.80, ϕLO = π ∕2 − 0.44). ‘High-frequency’: low-power configuration suitable for detection of the GW signals from the millisecond pulsars, similar to one planned for GEO HF [169] [J = 0.1JaLIGO, −1 Γ = 2π × 1000 s, β = π∕2 − 0.01, ϕLO = 0]. ‘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 [Stech = 0.1SSQL, J = JaLIGO, Γ = 1050 s− 1, β = π∕2 − 0.040, ϕLO = 0.91]. In all cases, ηd = 0.95 and the losses part of the bandwidth − 1 γ2 = 1.875 s (which corresponds to the losses − 4 Aarm = 10 per bounce in the 4 km long arms).