Table A.2: Best-fit parameters of the ToO RGS and EPIC-PN spectra fitted with power-law and broken power-law models, in the common energy range ([0.6-1.77] keV). The absorption parameter was fixed to the Galactic value. Systematic errors of 3% and of 0.5% were added to the RGS and to the EPIC-PN data, respectively. The error bars refer to the 90% confidence interval for one parameter. ^a erg cm^-2 s^-1.
Inst. $\alpha_1$ E_b $\alpha_2$ $F_{1 ~\rm keV}$ $F_{0.6-1.5~\rm keV}$ $\chi^2_r/\rm d.o.f.$

(keV) ( $\mu$ Jy) ( $\times 10^{-10}$ )^a

November 14, 2003

RGS-1 $0.97\pm0.01$ 188.3 4.17 1.13/246

RGS-1 $0.76\pm0.07$ $\rm0.80^{+0.05}_{-0.03}$ $\rm 1.03^{+0.03}_{-0.02}$ 192.3 4.18 0.91/244

RGS-2 $0.97\pm0.01$ 176.4 3.91 1.11/330

RGS-2 $\rm0.75^{+0.09}_{-0.12}$ $0.78\pm0.04$ $1.02\pm0.02$ 180.0 3.90 1.0/328

PN $1.34\pm0.01$ 202.3 4.35 6.6/45

PN $\rm 1.23^{+0.02}_{-0.03}$ $1.02\pm0.06$ $1.43\pm0.02$ 207.2 4.35 0.81/43

**Table A.2:** Best-fit parameters of the ToO RGS and EPIC-PN spectra fitted with power-law and broken power-law models, in the common energy range ([0.6-1.77] keV). The absorption parameter was fixed to the Galactic value. Systematic errors of 3% and of 0.5% were added to the RGS and to the EPIC-PN data, respectively. The error bars refer to the 90% confidence interval for one parameter. ^a erg cm^-2 s^-1.
Inst.	$\alpha_1$	E_b	$\alpha_2$	$F_{1 ~\rm keV}$	$F_{0.6-1.5~\rm keV}$	$\chi^2_r/\rm d.o.f.$
		(keV)		( $\mu$ Jy)	( $\times 10^{-10}$ )^a
November 14, 2003
RGS-1	$0.97\pm0.01$			188.3	4.17	1.13/246
RGS-1	$0.76\pm0.07$	$\rm0.80^{+0.05}_{-0.03}$	$\rm 1.03^{+0.03}_{-0.02}$	192.3	4.18	0.91/244
RGS-2	$0.97\pm0.01$			176.4	3.91	1.11/330
RGS-2	$\rm0.75^{+0.09}_{-0.12}$	$0.78\pm0.04$	$1.02\pm0.02$	180.0	3.90	1.0/328
PN	$1.34\pm0.01$			202.3	4.35	6.6/45
PN	$\rm 1.23^{+0.02}_{-0.03}$	$1.02\pm0.06$	$1.43\pm0.02$	207.2	4.35	0.81/43

Source LaTeX | All tables | In the text

	1 Introduction
	2 The XMM-Newton observations and data reduction
	3 Looking for lines in various segments of the spectra
	4 Discussion
	5 Conclusions
	References
	Online Material
	Appendix A: RGS spectral analysis and comparison with EPIC-PN