A ionized reflecting skin above the accretion disk of GX 349+2

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Table 5:

Best-fit values of the parameters obtained fitting the emission features with relativistic smeared lines (diskline in XSPEC). The Fe-K $\alpha$ feature is modelled with one diskline component.
Aver. spectrum	Spectrum 1+3	Spectrum 2
$N_{\rm H}$ (10²² cm^-2)	$0.735 \pm 0.004$	0.735 (fixed)	0.735 (fixed)
$kT_{\rm BB}$ (keV)	$1.797^{\rm +0.016}_{-0.007}$	$1.780^{\rm +0.023}_{-0.009}$	$1.818^{\rm +0.013}_{-0.010}$
$N_{\rm BB}$ (10^-1)	$1.048^{\rm +0.004}_{-0.013}$	$0.924^{\rm +0.013}_{-0.017}$	$1.126^{\rm +0.007}_{-0.009}$
$kT_{\rm DIS~KBB}$ (keV)	$1.049^{\rm +0.028}_{-0.014}$	$1.08^{\rm +0.03}_{-0.02}$	$1.05 \pm 0.02$
$N_{\rm DIS~KBB}$	$207^{\rm +9}_{-20}$	$213^{\rm +14}_{-18}$	$190^{\rm +5}_{-12}$
$E_{1~{\rm keV}}$ (keV)	$1.052^{\rm +0.006}_{-0.009}$	$1.030^{\rm +0.009}_{-0.016}$	$1.062^{\rm +0.004}_{-0.009}$
$\sigma_{1~{\rm keV}}$ (eV)	$85^{\rm +13}_{-7}$	$120^{\rm +20}_{-8}$	$66^{\rm +10}_{-7}$
$I_{1~{\rm keV}}$	$24^{\rm +4}_{-2}$	$42^{\rm +8}_{-4}$	$17.0^{\rm +2.1}_{-1.4}$
Equiv. width (eV)	$22 \pm 2$	$32 \pm 2$	$17 \pm 2$
$\beta$ emiss. index	$-2.1 \pm 0.2$	$-2.10^{\rm +0.12}_{-0.23}$	$-2.10^{\rm +0.11}_{-0.16}$
$R_{\rm in}$ ( $R_{\rm g}$ )	$6.2^{\rm +19.1}_{-0.2}$	$6.6^{\rm +12.2}_{-0.6}$	$10^{\rm +14}_{-4}$
$R_{\rm out}$ ( $R_{\rm g}$ )	$1980^{\rm +2900}_{-710}$	1980 (fixed)	1980 (fixed)
$\theta$ (degrees)	$41.4^{\rm +1.0}_{-2.1}$	41.4 (fixed)	41.4 (fixed)
$E_{{\rm S} \; {\rm XVI}}$ (keV)	2.62 (fixed)	2.62 (fixed)	2.62 (fixed)
$I_{{\rm S} \; {\rm XVI}}$	$2.2^{\rm +0.5}_{-0.9}$	$3.4^{\rm +0.9}_{-1.0}$	$0.9 \pm 0.6$
Equiv. width (eV)	$5 \pm 3$	$8^{\rm +4}_{-3}$	$2^{\rm +3}_{-2}$
$E_{{\rm Ar \; XVIII}}$ (keV)	$3.29 \pm 0.03$	$3.32 \pm 0.02$	$3.28^{\rm +0.02}_{-0.04}$
$I_{{\rm Ar} \; {\rm XVIII}}$	$3.5^{\rm +0.5}_{-0.6}$	$3.8^{\rm +0.9}_{-1.1}$	$2.7^{\rm +0.6}_{-0.8}$
Equiv. width (eV)	$11 \pm 4$	$12 \pm 4$	$9 \pm 4$
$E_{{\rm Ca} \; {\rm XIX}}$ (keV)	$3.89 \pm 0.03$	$3.89^{\rm +0.03}_{-0.04}$	$3.90 \pm 0.03$
$I_{{\rm Ca} \; {\rm XIX}}$	$3.6^{\rm +0.5}_{-0.7}$	$3.5 \pm 0.9$	$3.2 \pm 0.7$
Equiv. width (eV)	$15 \pm 4$	$15 \pm 5$	$13 \pm 5$
$E_{{\rm Fe} \; {\rm XXV}}$ (keV)	$6.76 \pm 0.02$	$6.74 \pm 0.04$	$6.78 \pm 0.03$
$I_{{\rm Fe} \; {\rm XXV}}$	$5.7^{\rm +0.5}_{-0.6}$	$5.5 \pm 0.8$	$5.8^{\rm +0.7}_{-0.8}$
Equiv. width (eV)	$61 \pm 9$	$64 \pm 11$	$59 \pm 11$
$\chi_{\rm red}^2({\rm d.o.f.})$	1.47(268)	1.24(271)	1.30(271)

Note. Uncertainties are at the 90% confidence level for a single parameter. The parameters are defined as in XSPEC. The continuum emission is fitted with a blackbody plus a multicolored disk blackbody, diskbb. The four broad emission features are modelled adopting diskline components. All components are subject to interstellar absorption. The intensity of the lines are in units of 10^-3 ph cm^-2 s^-1.

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