All Tables

Table 1: PG-name, redshift and Galactic column density. The redshifts are taken from Véron-Cetty & Véron (2000).
Table 2: Exposure details: (1) observation ID; (2) exposure number used in Table 3.
Table 3: Source extraction and low background screening process: (1) an annulus with an inner radius of 1' and an outer radius 5' centered on the source position was used as reference area for the screening. The data were binned with 10 s; (2) coordinates in J2000; (3) extraction radius for the source; (4) energy range considered for the screening; (5) rejection threshold for screening; (6) for annular background areas the inner and the outer radius are provided. (7) background corrected count rate in the energy range of 0.3-12.0 keV for pn and 0.5-10.0 keV for MOS, respectively; (8) accumulated exposure time.
Table 4: Spectral fits of the EPIC spectra of the quasars. The errors for the 90% confidence level are provided if $\chi ^2_{\rm reduced} < 2.0$ . Fits labeled with $\ddagger$ have $\chi ^2_{\rm reduced} > 2.0$ and consequently no errors were determined. 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. Explanation of labels: (1) explanation of the used models: pl: power-law (XSPEC: pow), nab: neutral absorber at the redshift of the source (XSPEC: zphabs), pab: partial covering with neutral absorber at the redshift of the source (XSPEC: zpcfabs), iab: ionized absorption at the redshift of the source (XSPEC: absori), ga: Gaussian line at the redshift of the source (XSPEC: zgauss), la: relativistic disk line after Laor (XSPEC: laor, Laor et al. 1997); Parameters: (a) equivalent column density; (b) covering fraction; (c) ionization level of absorbing material $\xi =L/nr^{2}$ , as defined in XSPEC; (d) photon flux at $1 \rm ~keV$ ; (e) degrees of freedom.
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
Table 6: CLOUDY models for the three quasars: (1) $U=\frac{Q(H)}{4\pi r^{2} n c}$ where Q(H) is the number of hydrogen ionizing photons, r is the distance of the gas to the continuum source, n is the gas number density and c the speed of light.