All Tables

Table 1: The 21 Type I AGN included in the present sample. The Galactic column density along the line-of-sight ( $N_{\rm H}^{\rm Gal}$ ) is expressed in units of 10²⁰ cm^-2. NLG: narrow line galaxy. RQQ: radio-quiet quasar. RLQ: radio-loud quasar.
Table 2: List of the XMM-Newton observations. Column (1): Name of the source; Col. (2): observation date (dd/mm/yyyy), Col. (3): orbit revolution number, Col. (4): Observation ID, and Col. (5): data exposure time of the pn data (in ks), except for PG 0804+761 for which the MOS exposure time is given.
Table 3: Black hole mass ( $M_{\rm BH}$ ), monochromatic luminosity $\nu$ $L_{\nu }$ (5100 Å), bolometric luminosity ( $L_{\rm bol}$ ), and accretion rate with respect to Eddington. (*) $L_{\rm bol}\simeq 9 \times \nu L_{\nu }$ (5100 Å). (**) using the relation (3) given by Woo & Urry et al. (2002) between $M_{\rm BH}$ and $\nu L_{\nu }$ (5100 Å). (^a) Kaspi et al. (2000), (^b) Vestergaard (2002), and (^c) Shields et al. (2003), (^d) Grupe et al. (2004), and (^e) Woo & Urry (2002).
Table 4: Spectral fits with an absorbed power law continuum in two energy bands (2-5 keV and 0.3-2 keV). Galactic absorption ( $N_{\rm H}^{\rm Gal}$ ) and intrinsic absorption ( $N^{\rm in}_{\rm H}$ ) of the QSO in its rest frame are expressed in 10²⁰ cm^-1. (^a) absorption edge(s) added to the continuum model (see parameter values in Table 6).
Table 5: Spectral fit with a broken power law model ( $\Gamma _{\rm soft}$ , $\Gamma _{\rm hard}$ , and $E_{\rm c}$ break point for the energy in keV), including the Galactic ( $N^{\rm Gal}_{\rm H}$ ) and intrinsic ( $N^{\rm in}_{\rm H}$ ) absorptions (expressed in 10²⁰ cm^-1). The unabsorbed fluxes are expressed in 10^-12 erg s^-1 cm^-2. In parentheses are reported the luminosities (expressed in 10⁴⁴ erg s^-1). The last column reports the flux ratio in the 0.3-2 keV and 0.3-10 keV energy bands. For PG 1114+445, two strong absorption edges are required (see values in Table 6).
Table 6: Spectral fit of absorption edge(s). $\tau$ is the optical depth. Significant detections ( $\geq$ 99 $\%$ ) are marked in bold face.
Table 7: Best-fitting spectral parameters for objects presenting a significant line detection (i.e. $P_{\rm prob} \geq 90\%$ ). GA: Gaussian profile. D (DISKLINE) and L (LAOR): profile line emitted by a relativistic accretion disk for a non-rotating BH (Fabian et al. 1989) and a maximally rotating BH (Laor 1991), respectively. The inclination of the disk is fixed to 30 deg. We assume q= -2 (emissivity law), (*) for PG 1402+261 q is let as a free parameter: |q|>3.0, and |q|=3.3^+0.3_-0.5, respectively for D and L. D: $R_{\rm in}=6~R_{\rm g}$ and $R_{\rm out}=1000~R_{\rm g}$ . L: $R_{\rm in}=1.26~R_{\rm g}$ , $R_{\rm out}=400~R_{\rm g}$ .
Table 8: Fit results, in the 2-12 keV energy band, of a disk reflection model assuming a LAMPPOST geometry for I Zw1, PG 0804+761, PG 1114+445, PG 1116+215 and PG 1309+355, i.e. we assume a height of 10 $R_{\rm g}$ , a ratio of X-ray to disk flux of 0.2 (with solar iron abundance). For PG 1402+261, a lower height above the AD of about 2.5 $R_{\rm g}$ , an iron abundance of 5 relative to solar abundance are required. Its spectrum is dominated by reflection.
Table 9: Spectral fit with an absorbed black body spectrum of an accretion disk ( DISKPN, ${\it kT}_{\rm diskpn}$ ) combined with a power law model. $T^{\rm max}_{\rm disk}$ (in eV) represents the maximal values of the disk temperature for a standard $\alpha$ thin accretion disk at 3 $R_{\rm S}$ . ${\it kT}_{\rm diskpn}$ is expressed in eV. (^a) one or two absorption edges are added to the continuum model due to the presence of a WA. (^b) a Fe K line is added (either a Gaussian line or a LAOR line).
Table 10: Spectral fit with absorbed compTT+power law. For the COMPTT component model, the soft photon temperature ( ${\it kT}^{\rm photon}_{1}$ ) is fixed to Tmax (Col. 1 of Table 9). ${\it kT}^{\rm plasma}$ is expressed in keV. $\tau$ corresponds to the plasma optical depth. The fits include the Galactic ( $N^{\rm Gal}_{\rm H}$ ) and intrinsic ( $N^{\rm in}_{\rm H}$ ) absorptions. Column densities are expressed in 10²⁰ cm^-1. The unabsorbed fluxes are expressed in 10^-12 erg s^-1 cm^-2. In parentheses are reported the luminosities (expressed in 10⁴⁴ erg s^-1). The last column reports the flux ratio in the 0.3-2 keV and 0.3-10 keV energy bands. (^a) one or two absorption edges are added to the continuum model due to the presence of a WA. (^b) a Fe K line is added (either a Gaussian line or a LAOR line).
Table 11: Mean and standard deviation ( $\sigma$ ) of the photon index in the 0.3-2 keV and 2-5 keV energy ranges. NLG: Narrow Line Galaxies ( ${\it FWHM}<2000$ km s^-1), RQQ: radio-quiet quasars, and RLQ (radio-loud quasars).
Table 12: Spearman-rank correlations. ( $r_{\rm s}$ , $P_{\rm rs}$ ): $r_{\rm s}$ Spearkman coefficient, and $P_{\rm rs}$ probability. $r_{\rm s}>0$ and $r_{\rm s}<0$ means a correlation and an anti-correlation, respectively. Significant correlations ( $\geq$ 99 $\%$ ) are marked in bold face.
Table A.1: Summary for all objects for detections of soft excess (SE), warm absorber (WA), and Fe K $\alpha$ line.