All Tables

Table 1: Main characteristics of the observed AGN. Columns: (1) name of the source from the Third EGRET Catalog; (2) name of the known counterpart; (3) other name; (4) classification of the active nucleus (LBL: low frequency peaked BL Lacertae Object; HBL: high frequency peaked BL Lacertae Object; FSRQ: flat-spectrum radio quasar; RG: radio galaxy); (5) coordinates (J2000); (6) redshift; (7) Galactic absorption column density [10²⁰ cm^-2] from Dickey & Lockman (1990).
Table 2: Best fit model parameters for the 15 AGN (present work). In the case of sources with multiple pointings, the weighted averages are shown. Since PKS 2155-304 (3EG J2158-3023) is best fitted in 4 pointings with the broken power law model and in the remaining 5 with the simple power law model; we reported the averages of both models. Columns: (1) name of the source; (2) absorbing column density [10²⁰ cm^-2]; (3) photon index $\Gamma$ , if the best fit is a simple power law model or soft photon index $\Gamma _1$ , if the best fit model is a broken power law; (4) hard photon index $\Gamma _2$ for the broken power law model; (5) break energy [keV].
Table 3: Best fit model parameters for the 15 AGN from the BeppoSAX catalogs by Giommi et al. (2002) and Donato et al. (2005). The values are the weighted averages obtained from multiple observations (if any) and from the two catalogs. In the case of 3C 273 (3EG J1229-0210) there were 9 observations, 5 best fitted with a broken power law and 4 with a single power law model: both model averages are reported. For NGC 6251 (3EG J1621+8203) the average is obtained from Chiaberge et al. (2003) and Guainazzi et al. (2003) from a fit in the energy band 0.1-200 keV. Grandi et al. (2003) is the reference for Cen A (3EG J1324-4314), from a fit in the energy band 0.4-250 keV excluding the 5.5-7.5 keV band (iron emission line). The value for PKS 1830-211 (3EG J1832-2110) has been obtained by De Rosa et al. (2005) from a fit in the energy band 0.5-80 keV (Chandra and INTEGRAL). Columns: (1) name of the source; (2) absorbing column density [10²⁰ cm^-2]; (3) photon index $\Gamma$ , if the best fit is a simple power law model or soft photon index $\Gamma _1$ , if the best fit model is a broken power law; (4) hard photon index $\Gamma _2$ for the broken power law model; (5) break energy [keV].
Table 4: Parameters for the models of AO 0235+164, PKS 1334-127, PKS 1406-076, and PKS 1830-211: above the dividing line are listed the input parameters used to model the SED according to the finite injection time synchrotron-inverse Compton model of Ghisellini et al. (2002). Below the dividing line we list the output parameters for the four fitted sources. See the text for more details.
Table 5: Parameters useful to understand $\gamma$ -ray loudness. Columns: (1) source name; (2) beaming factor $\delta$ ; (3) observed flux in the 0.4-10 keV energy band [erg cm^-2 s^-1]; (4) intrinsic luminosity in the 0.4-10 keV energy band [erg s^-1]; (5) Confidence of the EGRET detection (high >95%; low <95%).
Table A.1: XMM-Newton Observation Log. Columns: (1) Source name; (2) Observation Identifier; (3) Date of the observation [DD-MM-YYYY]; (4,5,6) Observing mode of MOS1, MOS2, and PN, respectively [FF: Full Frame; SW: Small Window; TIMING: timing mode, without imaging] with the effective exposure time [ks]; (7) Angular distance from the boresight [arcsec].
Table A.2: Fit results with single powerl law model. Columns: (1) Source name; (2) absorbing column density [10²⁰ cm^-2]; (3) photon index of the power law; (4) normalization of the power law model [10^-2 ph cm^-2 s^-1 keV^-1 at 1 keV]; (5) reduced $\chi ^2$ and degrees of freedom; (6) observed flux in the 0.4-10 keV energy band [10^-11 erg cm^-2 s^-1]; (7) intrinsic luminosity in the 0.4-10 keV energy band rest frame [10⁴⁵ erg s^-1]. The uncertainties in the parameter estimates are at the $90\%$ confidence limits for 1 parameter. For $N_{{\rm H}}={\rm Gal}$ , it means that the absorption column has been fixed to the Galactic value.
Table A.3: Fit results with the broken power law model. Columns: (1) source name; (2) absorbing column density [10²⁰ cm^-2]; (3) low energy photon index of the power law; (4) high energy photon index; (5) break energy [keV]; (6) normalization of the power law model [10^-2 ph cm^-2 s^-1 keV^-1 at 1 keV]; (7) reduced $\chi ^2$ and degrees of freedom; (8) observed flux in the 0.4-10 keV energy band [10^-11 erg cm^-2 s^-1]; (9) intrinsic luminosity in the 0.4-10 keV energy band rest frame [10⁴⁵ erg s^-1]; (10) Ftest probability [%]; fit with probability below 90% are not reported. The uncertainties in the parameter estimates are at the $90\%$ confidence limits for 1 parameter. For $N_{{\rm H}}={\rm Gal}$ , it means that the absorption column has been fixed to the Galactic value.
Table A.4: Additional fit results for 3C 273 (3EG J1229+0210) with the model composed of a black body plus a power law (wa(zbb+zpo)), absorbed with the Galactic column density. Columns: (1) temperature [keV]; (2) normalization of the black body model [ 10^-4L₃₉/D₁₀², where L₃₉ is the source luminosity in units of 10³⁹ erg/s and D₁₀ is the source distance in units of 10 kpc]; (3) photon index; (4) normalization of the power law model [10^-2 ph cm^-2 s^-1 keV^-1 at 1 keV]; (5) reduced $\chi ^2$ and degrees of freedom; (6) observed flux in the 0.4-10 keV energy band [10^-11 erg cm^-2 s^-1]; (7) intrinsic luminosity in the 0.4-10 keV energy band rest frame [10⁴⁵ erg s^-1]. The uncertainties in the parameter estimates are at the $90\%$ confidence limits for 1 parameter.
Table A.5: Detections and upper limits on the equivalent width of iron lines for 3C 273 (3EG J1229+0210). The continuum is best fitted with the broken power law model with Galactic absorbtion reported in Table A.3. Columns: (1) equivalent width [eV] for E=6.4 keV and $\sigma =0.15$ keV; (2) $\Delta \chi ^2$ with respect to the best fit continuum (2 d.o.f.); (3) equivalent width [eV] for E=6.4 keV and $\sigma =0.5$ keV; (4) $\Delta \chi ^2$ with respect to the best fit continuum (2 d.o.f.); (5) equivalent width [eV] for E=6.7 keV and $\sigma =0.15$ keV; (6) $\Delta \chi ^2$ with respect to the best fit continuum (2 d.o.f.); (7) equivalent width [eV] for E=6.7 keV and $\sigma =0.5$ keV; (8) $\Delta \chi ^2$ with respect to the best fit continuum (2 d.o.f.); The uncertainties in the parameters and upper limits estimate are at the $90\%$ confidence limits for 1 parameter.
Table A.6: (Left) Additional fit results for Cen A (3EG J1324-4314) with the model composed of an absorbed power law, plus one or two Gaussian emission lines. Fit performed in the 4-10 keV energy band and then extrapolated to 0.4-10 keV. The two columns refer to the two observations. The rows list the following parameters: (1) absorbing column density [10²⁰ cm^-2]; (2) photon index of the power law model; (3) normalization of the power law model [10^-2 ph cm^-2 s^-1 keV^-1 at 1 keV]; (4) energy of the emission line 1 [keV]; (5) line width $\sigma$ 1 [keV]; (6) flux of the emission line 1 [10^-4 ph cm^-2 s^-1]; (7) equivalent width of the emission line 1 [eV]; (8) energy of the emission line 2 [keV]; (9) line width $\sigma$ 2 [keV]; (10) flux of the emission line 2 [10^-4 ph cm^-2 s^-1]; (11) equivalent width of the emission line 2 [eV]; (12) reduced $\chi ^2$ and degrees of freedom; (13) observed flux in the 0.4-10 keV energy band [10^-11 erg cm^-2 s^-1]; (14) intrinsic luminosity in the 0.4-10 keV energy band rest frame [10⁴⁵ erg s^-1]. The uncertainties in the parameter estimates are at the $90\%$ confidence limit for one parameter of interest. For $N_{{\rm H}}={\rm Gal}$ , it means that the absorption column has been fixed to the Galactic value. The luminosities were calculated using d=3.84 Mpc. (Right) EPIC spectrum in the 4-10 keV energy band.
Table A.7: Optical properties of the AGN of the present catalog (from the Optical Monitor data). The data refers to the magnitude averaged over the whole observation. Columns: (1) Source name; (2) V magnitude [543 nm]; (3) B magnitude [450 nm]; (4) U magnitude [344 nm]; (5) UVW1 magnitude [291 nm]; (6) UVM2 magnitude [231 nm]; (7) UVW2 magnitude [212 nm]; The uncertainties in the parameter estimates are at the $1\sigma$ level and also include systematics.