XMM-Newton long-look observation of the narrow-line Seyfert 1 galaxy PKS 0558–504 - II. Timing analysis

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Table 2:

PSD model fitting results.
PSD	Model	A^a	$\alpha$	C	$\nu_{\rm b}$	$\alpha_l$	$\alpha_h$	$f_{\rm L}$	R	$\chi^2/$ d.o.f.
		(Hz^-1)		(Hz^-1)	( $\times 10^{-6}$ Hz)			( $\times 10^{-5}$ Hz)	(%)
XMM/soft	PL	$18^{\rm +4}_{-3}$	$2.30\pm 0.14$	$0.14\pm 0.01$	-	-	-	-	-	43.6/42
XMM/soft	PL+L	$13^{\rm +7}_{-6}$	$2.24\pm 0.20$	$0.14\pm 0.01$	-	-	-	$8.2^{\rm +4.9}_{-2.1}$	$4.9\pm 2.5$	34.9/40
XMM/hard	PL	$19^{\rm +4}_{-3}$	$2.11\pm 0.18$	$0.94\pm 0.05$	-	-	-	-	-	41.2/42
RXTE+ XMM	BPL	$64^{\rm +24}_{-8}$	-	0.94^b /906^c	$6.7^{\rm +4.4}_{-2.9}$	$0.40\pm 0.17$	$2.21^{\rm +0.24}_{-0.20}$	-	-	51.7/53

Notes. Following Lampton et al. (1976), all errors indicate the 68% confidence intervals, for 3, 5 and 4 parameters of interest in the case of the PL, BPL and PL+L models, respectively.
^(a) PL normalization which is equal to the PSD value at 10^-4 Hz. In the case of the BPL model, A is defined as in Eq. (2). ^(b) Poisson noise level for the ``high-frequency'' part of the PSD. This value is equal to the best-fit value of the PL model fit to the XMM-Newton hard band PSD, and it was kept constant during the model fit. ^(c) Expected Possion noise level for the low-frequency, RXTE part of the PSD.

Source LaTeX | All tables | In the text

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