Fig. 1: MLI output for three correlation classes.
From: Signatures of correlation of spacetime fluctuations in laser interferometers
Output signal power spectral densities (PSDs) of an MLI due to SFs. For correlation class (a), factorised ρF, the scaled PSD \({S}_{{{{\rm{NC}}}}}(\nu )=\frac{cS(f)}{{\Gamma }_{{{{\rm{S}}}}}{{{{\mathcal{L}}}}}^{3}}\) vs. \(\nu=\frac{\pi f}{2{f}_{{{{\rm{LRT}}}}}}\) is plotted. For classes (b), inverse ρIm, and (c) exponential ρEm with m = S, ST, the scaled PSD \({S}_{{{{\rm{C}}}}}(\nu )=\frac{cS(f)}{{\Gamma }_{{{{\rm{S}}}}}{\ell }_{r}{{{{\mathcal{L}}}}}^{2}}\) vs ν is plotted. Here, m = S (m = ST) denotes correlations depending on spatial (spacetime) separation. In (c), PSDs corresponding to ρES for \(\kappa={\ell }_{r}/{{{\mathcal{L}}}}=0.025\) (red solid), κ = 0.01 (green dashed), κ = 0.005 (brown dot-dashed), and κ = 0.0025 (pink dotted), demonstrate dependence on κ. The PSD corresponding to ρEST for κ = 0.025 (blue points) is also plotted in (c). Small and large ν trends are as indicated by black dashed/dotted lines in (a)−(c). The black vertical line marks ν = 1.
