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Table 3

Main results obtained from the analysis of the X-ray spectra of all AGN present in the sample.

Source N Hgal Γ + N H χ2/ν F (2−10) keV F (20−100) keV
× 1022 cm-2 × 1022 cm-2 × 10-11 erg s-1 cm-2 × 10-11 erg s-1 cm-2
PBC J0041.6+2534 A 0.038 6.2/7 0.02 1.0
PBC J0100.6−4752A 0.019 4.3/11 0.28 0.6
PBC J0122.3+5004A 0.136 44 1.9/3 0.09 0.6
PBC J0140.4−5320A 0.026 28.7/26 0.50 0.7
PBC J0248.9+2627 0.103 [1.8] 3.6/3 0.40 1.2
PBC J0353.5+3713A 0.168 13.2/14 0.35 0.8
PBC J0356.9−4040A 0.019 25.9/38 0.74 1.1
PBC J0503.0+2300 0.226 148.6/149 1.25 1.1
PBC J0543.6−2738A 0.022 8.3/8 0.47 1.1
PBC J0544.3+5905 0.158 8.3/18 0.47 1.1
PBC J0623.8−3212B 0.038 [1.8] 3.3/2 0.07 1.5
PBC J0641.3+3251A 0.159 14.5/16 0.29 1.0
PBC J0759.9+2324 0.047 9/10 0.44 1.3
PBC J0814.4+0421 0.032 9.3/15 0.50 1.1
PBC J0919.9+3712 C1 0.011 326.9/328 0.36 1.2
PBC J0954.8+3724∗ 0.014 [1.8] 2.4/2 0.15 0.4
PBC J1246.9+5432 D 0.014 15/22 0.09 1.5
PBC J1335.8+0301 A 0.019 313.3/299 0.64 1.1
PBC J1344.2+1934 0.017 [1.8] 38 2/4 0.10 0.9
PBC J1345.4+4141A 0.009 10.4/25 0.74 0.7
PBC J1439.0+1413A 0.014 [1.8] 12/8 0.32 0.5
PBC J1453.0+2553 0.033 – 73.8/87 1.06 1.0
PBC J1506.6+0349 0.037 14/19 0.42 0.7
PBC J1546.5+6931∗ 0.031 [1.8] 16 3.3/2 0.08 0.5
PBC J1620.3+8101 0.046 [1.8] 9.6/13 0.54 0.7
PBC J2148.2−3455 0.019 [1.8] – 6/11 0.04 0.9
PBC J2333.9−2343 0.016 – 97/104 0.80 0.7
PBC J2341.9+3036 C2 0.058 25/28 0.11 1.0

Notes.

(+)

The square brackets in the Γ column indicate that we used a fixed value.

(*)

Grouping of 10 instead of 20 applied owing to the poor statistical quality of the data.

(A)

Best-fit model requires an extra power-law component, having the same photon index as the primary absorbed power-law and passing only through the galactic column density (wagal*(po+wa*po) in xspec terminology).

(B)

Best-fit model requires an extra black-body component with keV (wagal*(bb+wa*po) in xspec terminology).

(C1)

Best-fit model requires an extra power-law component, having the same photon index as the primary absorbed power-law and passing only through the Galactic column density plus a narrow line at keV with eV (wagal*(po+wa*(po+ga)) in xspec terminology).

(D)

Best-fit model requires a black-body component with a keV and two narrow lines at keV and keV with an EW of eV and eV, respectively (wagal*(bb+wa*(po+ga+ga)) in xspec terminology).

(C2)

Best-fit model requires a second power-law component, having the same photon index as the primary absorbed power-law and passing only through the Galactic column density plus a narrow line with and eV (wagal*(po+wa*(po+ga)) in xspec terminology).

In bold face, we indicate sources for which we performed an X-ray data analysis using XMM-Newton observations.

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