Table A.1: Best-fit parameters of the RGS spectra reproduced with power-law, broken power-law and parabolic models. We fixed the absorption parameter to the Galactic value. The error bars refer to the 90% confidence interval. ^a erg cm^-2 s^-1.
Inst. $\alpha_1$ E_b $\alpha_2$ $F_{1 ~\rm keV}$ $F_{0.5-1.5~\rm keV }$ $\chi^2_r/\rm d.o.f.$

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

Exp. 0136540301

RGS-1 0.99 101.9 2.71 3.26/127

RGS-1 $\rm0.755^{+0.055}_{-0.035}$ $\rm0.74^{+0.1}_{-0.03}$ $\rm 1.27^{+0.11}_{-0.04}$ 104.9 2.72 0.91/125

RGS-2 1.05 92.4 2.48 4.24/125

RGS-2 $0.81\pm0.03$ $\rm0.80^{+0.02}_{-0.03}$ $\rm 1.46^{+0.04}_{-0.06}$ 97.3 2.51 0.90/125

Exp. 0136540401

RGS-1 0.93 120.1 3.16 3.89/137

RGS-1 $\rm0.63^{+0.03}_{-0.06}$ $\rm0.69^{+0.02}_{-0.04}$ $\rm 1.20^{+0.03}_{-0.04}$ 123.2 3.19 0.94/135

RGS-2 0.94 115.9 3.05 2.52/144

RGS-2 $\rm0.77^{+0.04}_{-0.02}$ $\rm0.79^{+0.03}_{-0.05}$ $1.18\pm0.04$ 121.0 3.07 1.21/142

Exp. 0136541001

RGS-1 0.90 72.8 1.91 2.83/227

RGS-1 $0.64\pm0.02$ $\rm0.67^{+0.03}_{-0.02}$ $1.11\pm0.02$ 75.0 1.92 0.92/225

RGS-2 0.92 68.7 1.81 2.5/240

RGS-2 $\rm0.74^{+0.03}_{-0.02}$ $\rm0.76^{+0.03}_{-0.04}$ $\rm 1.17^{+0.02}_{-0.04}$ 71.6 1.82 0.97/238

Exp. 0158970101

RGS-1 1.06 74.0 1.98 3.5/138

RGS-1 $0.80\pm0.04$ $\rm0.71^{+0.02}_{-0.04}$ $\rm 1.33^{+0.03}_{-0.04}$ 75.3 2.00 1.16/136

RGS-2 1.10 68.5 1.85 2.3/139

RGS-2 $\rm0.92^{+0.03}_{-0.04}$ $0.76\pm0.05$ $1.35\pm0.04$ 71.2 1.86 0.83/137

Exp. 0150498701

RGS-1 0.80 186.5 4.83 3.17/454

RGS-1 $0.56\pm0.02$ $0.71\pm0.02$ $1.015\pm0.015$ 192.4 4.87 1.13/452

RGS-2 0.82 174.3 4.52 2.42/490

RGS-2 $0.64\pm0.02$ $0.73\pm0.02$ $\rm 1.02^{+0.01}_{-0.02}$ 179.8 4.56 1.08/488

Parabolic model

a b

Exp. 0136540301

RGS-1 $\rm 1.21^{+0.02}_{-0.03}$ $0.77\pm0.08$ 110.9 2.74 1.02/126

RGS-2 $\rm 1.33^{+0.02}_{-0.03}$ $\rm0.96^{+0.06}_{-0.1}$ 101.2 2.52 1.1/126

Exp. 0136540401

RGS-1 1.17^+0.02_-0.03 $\rm0.86^{+0.05}_{-0.09}$ 131.5 3.21 1.11/136

RGS-2 $\rm 1.10^{+0.02}_{-0.03}$ $\rm0.58^{+0.05}_{-0.09}$ 125.4 3.08 1.36/143

Exp. 0136541001

RGS-1 $\rm 1.09^{+0.01}_{-0.04}$ $\rm0.67^{+0.04}_{-0.07}$ 79.3 1.93 1.07/226

RGS-2 $\rm 1.10^{+0.01}_{-0.02}$ $\rm0.60^{+0.05}_{-0.06}$ 74.5 1.83 1.13/239

Exp. 0158970101

RGS-1 $\rm 1.28^{+0.02}_{-0.03}$ $\rm0.77^{+0.06}_{-0.08}$ 80.6 2.01 1.33/137

RGS-2 $1.29\pm0.02$ $\rm0.65^{+0.06}_{-0.09}$ 74.3 1.87 0.91/138

Exp. 0150498701

RGS-1 $0.96\pm0.01$ $\rm0.65^{+0.05}_{-0.03}$ 204.0 4.91 1.25/453

RGS-2 $\rm0.97^{+0.01}_{-0.02}$ $\rm0.53^{+0.03}_{-0.04}$ 188.6 4.57 1.25/489

**Table A.1:** Best-fit parameters of the RGS spectra reproduced with power-law, broken power-law and parabolic models. We fixed the absorption parameter to the Galactic value. The error bars refer to the 90% confidence interval. ^a erg cm^-2 s^-1.
Inst.	$\alpha_1$	E_b	$\alpha_2$	$F_{1 ~\rm keV}$	$F_{0.5-1.5~\rm keV }$	$\chi^2_r/\rm d.o.f.$
		(keV)		( $\nu$ Jy)	( $\times 10^{-10}$ )^a
Exp. 0136540301
RGS-1	0.99			101.9	2.71	3.26/127
RGS-1	$\rm0.755^{+0.055}_{-0.035}$	$\rm0.74^{+0.1}_{-0.03}$	$\rm 1.27^{+0.11}_{-0.04}$	104.9	2.72	0.91/125
RGS-2	1.05			92.4	2.48	4.24/125
RGS-2	$0.81\pm0.03$	$\rm0.80^{+0.02}_{-0.03}$	$\rm 1.46^{+0.04}_{-0.06}$	97.3	2.51	0.90/125
Exp. 0136540401
RGS-1	0.93			120.1	3.16	3.89/137
RGS-1	$\rm0.63^{+0.03}_{-0.06}$	$\rm0.69^{+0.02}_{-0.04}$	$\rm 1.20^{+0.03}_{-0.04}$	123.2	3.19	0.94/135
RGS-2	0.94			115.9	3.05	2.52/144
RGS-2	$\rm0.77^{+0.04}_{-0.02}$	$\rm0.79^{+0.03}_{-0.05}$	$1.18\pm0.04$	121.0	3.07	1.21/142
Exp. 0136541001
RGS-1	0.90			72.8	1.91	2.83/227
RGS-1	$0.64\pm0.02$	$\rm0.67^{+0.03}_{-0.02}$	$1.11\pm0.02$	75.0	1.92	0.92/225
RGS-2	0.92			68.7	1.81	2.5/240
RGS-2	$\rm0.74^{+0.03}_{-0.02}$	$\rm0.76^{+0.03}_{-0.04}$	$\rm 1.17^{+0.02}_{-0.04}$	71.6	1.82	0.97/238
Exp. 0158970101
RGS-1	1.06			74.0	1.98	3.5/138
RGS-1	$0.80\pm0.04$	$\rm0.71^{+0.02}_{-0.04}$	$\rm 1.33^{+0.03}_{-0.04}$	75.3	2.00	1.16/136
RGS-2	1.10			68.5	1.85	2.3/139
RGS-2	$\rm0.92^{+0.03}_{-0.04}$	$0.76\pm0.05$	$1.35\pm0.04$	71.2	1.86	0.83/137
Exp. 0150498701
RGS-1	0.80			186.5	4.83	3.17/454
RGS-1	$0.56\pm0.02$	$0.71\pm0.02$	$1.015\pm0.015$	192.4	4.87	1.13/452
RGS-2	0.82			174.3	4.52	2.42/490
RGS-2	$0.64\pm0.02$	$0.73\pm0.02$	$\rm 1.02^{+0.01}_{-0.02}$	179.8	4.56	1.08/488
Parabolic model
	a		b
Exp. 0136540301
RGS-1	$\rm 1.21^{+0.02}_{-0.03}$		$0.77\pm0.08$	110.9	2.74	1.02/126
RGS-2	$\rm 1.33^{+0.02}_{-0.03}$		$\rm0.96^{+0.06}_{-0.1}$	101.2	2.52	1.1/126
Exp. 0136540401
RGS-1	1.17^+0.02_-0.03		$\rm0.86^{+0.05}_{-0.09}$	131.5	3.21	1.11/136
RGS-2	$\rm 1.10^{+0.02}_{-0.03}$		$\rm0.58^{+0.05}_{-0.09}$	125.4	3.08	1.36/143
Exp. 0136541001
RGS-1	$\rm 1.09^{+0.01}_{-0.04}$		$\rm0.67^{+0.04}_{-0.07}$	79.3	1.93	1.07/226
RGS-2	$\rm 1.10^{+0.01}_{-0.02}$		$\rm0.60^{+0.05}_{-0.06}$	74.5	1.83	1.13/239
Exp. 0158970101
RGS-1	$\rm 1.28^{+0.02}_{-0.03}$		$\rm0.77^{+0.06}_{-0.08}$	80.6	2.01	1.33/137
RGS-2	$1.29\pm0.02$		$\rm0.65^{+0.06}_{-0.09}$	74.3	1.87	0.91/138
Exp. 0150498701
RGS-1	$0.96\pm0.01$		$\rm0.65^{+0.05}_{-0.03}$	204.0	4.91	1.25/453
RGS-2	$\rm0.97^{+0.01}_{-0.02}$		$\rm0.53^{+0.03}_{-0.04}$	188.6	4.57	1.25/489

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