The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

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Volume 500 / No 2 (June III 2009)

A&A, 500 2 (2009) 769-779

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Table 3:

Comparison of SS1 spectral best fit parameters and derived parameters for blackbody and WD atmosphere models with halo and solar abundances.
Model	Blackbody	WD halo	WD solar
(energy range [keV])	(0.2-0.8)	(0.2-0.6)	(0.2-0.6)
kT (eV)	48⁺²_-3	$61\pm1$	$70\pm1$
$N_{\rm H}$ (10²¹ cm^-2)	$2.3\pm0.1$	$1.0\pm0.2$	$1.0\pm0.2$
$\chi^{2}_{r}$	1.39	1.01	1.06
d.o.f.	53	44	48
L_x (10³⁸ erg s^-1)	$10.6 \pm 0.2$	$1.00 \pm 0.02$	$0.88 \pm 0.02$
L_bol (10³⁸ erg s^-1)	$\rm 28.7^{+0.2}_{-0.1}$	$2.7 \pm 0.1$	$1.5 \pm 0.1$
R (10⁹ cm)	$\rm 7.0^{+1.6}_{-0.7}$	$1.21 \pm 0.07$	$0.70 \pm 0.04$
ecf $_{\rm PN}$ (ct cm² erg^-1)	5.0 $\times~10^{9}$	5.5 $\times~10^{10}$	6.1 $\times~10^{10}$
ecf $_{\rm HRC-I}$ (ct cm² erg^-1)	2.6 $\times~10^{9}$	3.2 $\times~10^{10}$	3.7 $\times~10^{10}$
ecf $_{\rm XRT}$ (ct cm² erg^-1)	7.4 $\times~10^{8}$	8.7 $\times~10^{9}$	9.9 $\times~10^{9}$

Notes: Luminosities and WD radii refer to the XMM-Newton observation 0511380201. The unabsorbed X-ray luminosity L_x is for the 0.2-1.0 keV range. Bolometric luminosities and WD radii for the WD atmosphere model are upper limits (see Sect. 2.1 for details).

Source LaTeX | All tables | In the text

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