Suzaku observation of the Phoenix galaxy | Astronomy & Astrophysics (A&A)

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Table 3:

Best fit parameters for the broand band ${\it Suzaku}$ (photoionization scenario) and XMM-*Newton* spectra.
	$\Gamma_{\rm s}$	$\Gamma_{\rm h}$	$N_{\rm H}$	R	$E_{\rm line}$	EW	$\chi^2_r$ /d.o.f.
			(10²³ cm^-2)		(keV)	(eV)
${\it Suzaku}$	$1.71\pm0.12$	(= $\Gamma_{\rm s}$ )	$\rm 3.33^{+0.17}_{-0.15}$	$\rm 1.28^{+0.81}_{-0.56}$	$6.397\pm0.009$	$218\pm 24$	1.16/219
XMM-Newton	$2.49\pm0.23$	$\rm 1.62^{+0.11}_{-0.23}$	$\rm 1.76^{+0.13}_{-0.21}$	<2.1	$6.44\pm0.05$	$133\pm 63$	1.21/70

Note: from left to right: the indices of the soft ( $\Gamma_{\rm s}$ ) and hard ( $\Gamma_{\rm h}$ ) power laws; the column density of the intrinsic absorber; the relative normalization of the Compton reflection component, R; the centroid energy, $E_{\rm line}$ and equivalent width (EW) of the iron line; the reduced $\chi^2$ and the d.o.f.

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