Table 5: Spectral fits of the emission line of PG 1535+547. The corresponding continuum fits are provided in Table 4. Fits labeled with $\dagger$ were performed over the 2-10 keV energy range for MOS and the 2-12 keV energy range of pn, respectively. (1) The following two models are used: ga: Gaussian line at redshift of source (XSPEC: zgauss), la: relativistic disk line after Laor (XSPEC: laor, Laor 1991); Parameters: (a) energy of line in rest frame of quasar; (b) line width ( $\sigma$ ); (c) total photons in line; (d) inclination angle
Fit Emission Energy^(a) Width^(b) Norm^(c) R(in) R(out) Inclination^(d)

line model [ $\rm keV$ ] [ $\rm keV$ ] [ $\rm cm^{-2}\;s^{-1}$ ] [ $\rm G\;M\;c^{-2}$ ] [ $\rm G\;M\;c^{-2}$ ] [ $\rm degree$ ]

11 la 6.4 (fixed) $\rm 5.38_{-0.68}^{+0.49} \;10^{-5}$ $\rm 1.77_{-0.77}^{+0.22}$ $\rm 7.83_{-0.66}^{+1.40}$ $\rm 31.85_{-1.45}^{+2.40}$

12 ga $\rm 6.00_{-0.21}^{+0.14}$ $\rm0.26_{-0.11}^{+0.21}$ $\rm 7.16_{-2.70}^{+2.69} \;10^{-6}$

13 $^{\dagger}$ ga $\rm 6.06_{-0.14}^{+0.14}$ $\rm0.19_{-0.08}^{+0.14}$ $\rm 5.22_{-2.71}^{+3.16} \;10^{-6}$

14 la 6.4 (fixed) $\rm 1.63_{-0.42}^{+0.42} \;10^{-5}$ $\rm 5.67_{-1.32}^{+2.16}$ $\rm 9.47_{-2.08}^{+1.59}$ $\rm 28.38_{-2.28}^{+4.36}$

15 $^{\dagger}$ la 6.4 (fixed) $\rm 1.28_{-0.44}^{+0.49} \;10^{-5}$ $\rm 7.00_{-2.57}^{+0.96}$ $\rm 8.16_{-0.75}^{+3.06}$ $\rm 28.63_{-2.18}^{+4.43}$

**Table 5:** Spectral fits of the emission line of PG 1535+547. The corresponding continuum fits are provided in Table 4. Fits labeled with $\dagger$ were performed over the 2-10 keV energy range for MOS and the 2-12 keV energy range of pn, respectively. (1) The following two models are used: ga: Gaussian line at redshift of source (XSPEC: zgauss), la: relativistic disk line after Laor (XSPEC: laor, Laor 1991); Parameters: (a) energy of line in rest frame of quasar; (b) line width ( $\sigma$ ); (c) total photons in line; (d) inclination angle
Fit	Emission	Energy^(a)	Width^(b)	Norm^(c)	R(in)	R(out)	Inclination^(d)
	line model	[ $\rm keV$ ]	[ $\rm keV$ ]	[ $\rm cm^{-2}\;s^{-1}$ ]	[ $\rm G\;M\;c^{-2}$ ]	[ $\rm G\;M\;c^{-2}$ ]	[ $\rm degree$ ]
11	la	6.4 (fixed)		$\rm 5.38_{-0.68}^{+0.49} \;10^{-5}$	$\rm 1.77_{-0.77}^{+0.22}$	$\rm 7.83_{-0.66}^{+1.40}$	$\rm 31.85_{-1.45}^{+2.40}$
12	ga	$\rm 6.00_{-0.21}^{+0.14}$	$\rm0.26_{-0.11}^{+0.21}$	$\rm 7.16_{-2.70}^{+2.69} \;10^{-6}$
13 $^{\dagger}$	ga	$\rm 6.06_{-0.14}^{+0.14}$	$\rm0.19_{-0.08}^{+0.14}$	$\rm 5.22_{-2.71}^{+3.16} \;10^{-6}$
14	la	6.4 (fixed)		$\rm 1.63_{-0.42}^{+0.42} \;10^{-5}$	$\rm 5.67_{-1.32}^{+2.16}$	$\rm 9.47_{-2.08}^{+1.59}$	$\rm 28.38_{-2.28}^{+4.36}$
15 $^{\dagger}$	la	6.4 (fixed)		$\rm 1.28_{-0.44}^{+0.49} \;10^{-5}$	$\rm 7.00_{-2.57}^{+0.96}$	$\rm 8.16_{-0.75}^{+3.06}$	$\rm 28.63_{-2.18}^{+4.43}$

Source LaTeX | All tables | In the text

	1 Introduction
	2 Optical and previous X-ray studies
	3 Observations and data reduction
	4 X-ray spectral analysis
	5 Spectral energy distribution
	6 Discussion
	7 Conclusions
	References