X-rays from Saturn: a study with XMM-Newton and Chandra over the years 2002–05

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Table 2:

*XMM-Newton* and *Chandra* spectral fitting results (errors are at 90% confidence).
Year	Satellite	Source	`mekal`	`mekal`	`mekal`	`mekal`	Gauss	Gauss	Gauss	Gauss	$\chi^2$	$\chi^2$	GOES-10
of	(observation	net	kT^a	norm^b	flux^c	0.2-2.0 keV	energy	norm^e	flux^f	emitted	/dof^g	/dof^g	1-8 Å
obs.	number)	counts				emitted	(keV)			power^d (MW)		no line	fluxⁱ
						power^d (MW)
2002	XMM-Newton (1)	112	0.28 $^{\rm +0.06}_{\rm -0.04}$	4.3 $^{\rm +1.2}_{\rm -1.1}$	1.04 $^{\rm +0.36}_{\rm -0.28}$	230 $^{\rm +80}_{\rm -62}$	0.48 $^{\rm +0.04}_{\rm -0.05}$	2.6 $^{\rm +1.7}_{\rm -1.8}$	0.20 $^{\rm +0.13}_{\rm -0.14}$	44 $^{\rm +29}_{\rm -30}$	0.9/5	7.0/7	1.13
2003	Chandra (1)	137	$0.65\pm{0.19}$	1.3 $\pm$ 0.4	0.37 $^{\rm +0.10}_{\rm -0.12}$	94 $^{\rm +25}_{\rm -30}$	0.55 $^{\rm +0.02}_{\rm -0.01}$	$5.9\pm{1.5}$	$0.53\pm{0.13}$	$135\pm{34}$	8.6/9	32.6/11	2.12
2004	Chandra (2)	112	0.59 $^{\rm +0.15}_{\rm -0.28}$	3.1 $^{\rm +0.7}_{\rm -0.8}$	0.90 $^{\rm +0.10}_{\rm -0.35}$	167 $^{\rm +19}_{\rm -65}$	0.57 $\pm$ 0.03	4.9 $^{\rm +2.3}_{\rm -2.1}$	0.44 $^{\rm +0.21}_{\rm -0.19}$	82 $^{\rm +38}_{\rm -35}$	12.2/10	16.7/12	3.23
2004	Chandra (3)	42	0.61 $^{\rm +0.84}_{\rm -0.36}$	0.7 $^{\rm +0.8}_{\rm -0.4}$	0.19 $^{\rm +0.15}_{\rm -0.12}$	36 $^{\rm +28}_{\rm -23}$	0.56 $^{\rm +0.05}_{\rm -0.03}$	4.3 $^{\rm +1.8}_{\rm -2.4}$	0.39 $^{\rm +0.16}_{\rm -0.22}$	74 $^{\rm +31}_{\rm -41}$	0.22/1	5.2/3	0.16
2005	XMM-Newton (2)	146	0.33 $^{\rm +0.12}_{\rm -0.08}$	$1.1\pm{0.4}$	0.27 $^{\rm +0.15}_{\rm -0.10}$	65 $^{\rm +36}_{\rm -24}$	$0.52\pm{0.02}$	$1.7\pm{0.7}$	$0.15\pm{0.06}$	$36\pm{15}$	17.4/16	33.3/18	0.22
2005	XMM-Newton (3)	<44^h	0.33	<0.3^h	<0.08^h	<19^h	0.52	<0.51^h	<0.05^h	<12^h			0.004

Notes. ^(a) mekal temperature in keV. ^(b) mekal normalisation at 1 keV in units of 10 $^{\rm -6}$ ph cm $^{\rm -2}$ s $^{\rm -1}$ keV $^{\rm -1}$ . ^(c) Total 0.2-2.0 keV energy flux in the mekal component in units of 10 $^{\rm -14}$ erg cm $^{\rm -2}$ s $^{\rm -1}$ ; the errors on the fluxes were obtained by varying the mekal temperatures and normalisations between their 90% confidence limits. ^(d) Powers and errors calculated by multiplying the values in the previous column by 4 $\pi$ d², where d is the geocentric distance of Saturn at the given epoch. ^(e) Gaussian line normalisation in units of 10 $^{\rm -6}$ ph cm $^{\rm -2}$ s $^{\rm -1}$ . ^(f) Total energy flux in the line in units of 10 $^{\rm -14}$ erg cm $^{\rm -2}$ s $^{\rm -1}$ . ^(g) $\chi^2$ value and degrees of freedom. ^(h) 3 $\sigma$ upper limit. ⁽ⁱ⁾ Solar X-ray flux (1.5-12.4 keV) in units of 10 $^{\rm -6}$ Watt m $^{\rm -2}$ , corrected for solar rotation (see text).

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