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Table 3.

Best-fit results of this work.

Source α* h(Rg) m ˙ Edd ( % ) $ \dot{m}_{\mathrm{Edd}}(\%) $ χ2/d.o.f.
Mrk 509 0 10–22 0.5–2.2
13.8 [10–37] 0.5 [0.5–6] 5.9/3
1 8–18 0.5–4
11.4 [8–37] 0.5 [0.5–2.2] 4.5/3
NGC 4151α 0 11–23 0.5–1.4
14.5 [11–93] 0.5 [0.5–19] 3.1/3
1 8–22 0.5–7
10.8 [8–63] 0.5 [0.5–44] 2/3
NGC 2617 0 11–19 0.5–1.1
13.5 [11–22] 0.5 [0.5–2.2] 5.5/4
1 11–13 6.5–8
9 [6–24] 0.85 [0.5–19] 5/4
Mrk 142 0 71–100 18–32
31.6 [15–100] 4 [0.5–32] 5.8/5
3.6 [2.5–100] 52 [18–56] 4/8
1 90–100 53–62
50.4 [17–100] 18 [0.5–62] 5.7/5
3.9 [2.5–100] 87 [53–91] 4/8

Notes. The third and the fourth columns list the 1σ confidence range of h and ṁEdd (in percentage), based on the width of the common area between the two 1σ confidence regions plotted in Fig. 5. Values listed in the line below these results indicate the model variance best-fit h and ṁEdd values and the corresponding 1σ confidence regions. The last column lists the best-fit χ2/degrees of freedom (d.o.f.) values. For Mrk 142, we also list our best-fit results to the time lags below the model variance best-fits (see Sect. 6.6).

(a)

For the variance models of this source, we assumed host galaxy absorption with E(B − V) = 0.35.

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