The universal power spectrum of quasars in optical wavelengths - Break timescale scales directly with both black hole mass and the accretion rate

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Table 3.

Best-fitting parameters and figures of merit for the five better-fitting power spectrum models.

α_L	α_H	A2	B	C	D	F	fom/N
0	−2.5	1.5	0.0052	−0.65	−0.30	−0.50	2.0
−0.5	−2.5	1.4	0.0052	−0.60	−0.30	−0.45	1.9
−1	−2.5	1.1	0.0058	−0.60	−0.35	−0.40	2.3

−0.5	−3	0.71	0.0086	−0.60	−0.35	−0.40	2.4
−1	−3	0.42	0.0104	−0.55	−0.35	−0.40	1.7

Notes. The low- and high-frequency powerspectral slopes are given in the first two columns. The parameters are explained in Eqs. (1)–(4) and N is the number of power spectral points, that is, the number of timescales times the number of M − R_Edd bins. The second, finer grid run.

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