Fig. 2.
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Spectral index vs. amplitude posterior distributions of the power-law PSD for DMv (left) and RN (right) obtained for 12 pulsars from DR2low (blue) and DR2new+ (orange) using the standard noise models. The green vertical lines show the predicted spectral index from a Kolmogorov turbulence in the IISM for DMv (left), and from circular and GW-driven SMBHBs (right). The black crosses display the 99.7% credible intervals of posterior distributions obtained with NANOGrav-15yr and PPTA DR3, displaying the principal directions.
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