X-ray and UV observations of nova V598 Puppis between 147 and 255 days after outburst

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Volume 507 / No 2 (November IV 2009)

A&A, 507 2 (2009) 923-927

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Table 2:

WD atmosphere model plus MEKAL fits to V598 Pup spectra at three epochs.
Satellite	Day since	No. of counts	Atmos. kT	Atmos. flux^a	MEKAL kT	MEKAL kT	MEKAL flux^a	C-stat/d.o.f.
	Optical peak	in spectrum	(eV)	(erg cm^-2 s^-1)	(eV)	(eV)	(erg cm^-2 s^-1)
XMM	147	MOS1: 653	35 $\pm$ 1^b	(8.1 $\pm$ 0.3) $\times$ 10^-12	$\rm 187^{+14}_{-12}$	$\rm 788^{+92}_{-86}$	(3.0 $\pm$ 0.4) $\times$ 10^-13	383/342
		MOS2: 641
		pn: 3458
Swift	172	117	$\rm 63^{+5}_{-4}$	$\rm 8.9^{+3.2}_{-2.2}$ $\times$ 10^-13	$\rm 636^{+218}_{-335}$	-	$\rm 1.7^{+0.7}_{-0.5}$ $\times$ 10^-13	76/56
Swift	247	88	$\rm 68^{+>18}_{-5}$	$\rm 2.0^{+0.7}_{-0.5}$ $\times$ 10^-13	$\rm 608^{+153}_{-144}$	-	$\rm 8.3^{+2.6}_{-3.1}$ $\times$ 10^-14	39/54

The day since peak corresponds to the mid-time of the spectrum. The absorbing column was fixed at 4.8 $\times$ 10²⁰ cm^-2 (Read et al. 2008). The XMM-Newton EPIC MOS1, MOS2 and pn spectra were fitted simultaneously, with a free constant of normalisation between them: with the pn constant fixed to unity, MOS 1 and MOS 2 have constants of 0.91 $\pm$ 0.08 and 0.96 $\pm$ 0.08 respectively. The temperature of the WD atmosphere component for the day 247 observation is constrained by the upper limit allowed by the model.
^a Unabsorbed, over 0.3-10 keV.
^b A systematic error of up to 25% may be required in addition; see text for details.

Source LaTeX | All tables | In the text

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