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Table 1:

Properties of our luminous obscured quasars.

Complete name 		Abbreviation 2-10 keV fluxa Rb $K_{\rm s}$c X/O zd $N_{\rm H}$e $L_{2-10~{\rm keV}}$f
HELLAS2XMM 054022.0-283139 PKS 0537#43 3.35 22.70 17.50 1.10 1.797 $\rm 10.5^{9.4}_{4.8}$ 6.8
HELLAS2XMM 053920.4-283721 PKS 0537#11a 4.19 23.40 18.25 1.48 0.981 $\rm 1.3^{1.5}_{0.9}$ 1.9
HELLAS2XMM 053917.1-283819 PKS 0537#164 1.50 23.60 19.02 1.12 1.824 - 3.1
HELLAS2XMM 053851.3-283949 PKS 0537#123 2.97 23.10 17.94 1.21 1.153 $\rm 6.6^{21.6}_{4.1}$ 2.0
HELLAS2XMM 003413.8-115559 GD 158#62 3.59 23.30 21.83 1.38 1.568 $\rm 26.3^{44.7}_{18.1}$ 4.9
HELLAS2XMM 003357.2-120039 GD 158#19 2.43 21.80 - 0.63 1.957 $\rm 7.3^{11.7}_{5.5}$ 6.3
HELLAS2XMM 204428.7-105629 Mrk 509#01 2.10 23.85 17.88 1.36 1.049 <1.1 1.5
HELLAS2XMM 204349.7-103243 Mrk 509#13 3.10 23.99 18.79 1.59 1.261 $\rm 2.5^{4.6}_{2.2}$ 2.6
HELLAS2XMM 235956.6-251019 Abell 2690#75 3.30 24.60 18.33 1.85 $\rm 1.3^{+0.30}_{-0.20}$ $^{\dagger}$ $\rm 15.0^{20.0}_{8.5}$ 3.2
HELLAS2XMM 031343.5-765426 PKS 0312#36 1.90 24.70 19.13 1.66 $\rm0.9^{+0.05}_{-0.15}$ $^{\dagger}$ $\rm 1.0^{1.2}_{0.9}$ 0.7
HELLAS2XMM 054021.1-285037 PKS 0537#91 4.2 23.70 18.99 1.60 1.538 $\rm 45.9^{102.0}_{36.0}$ 8.1
HELLAS2XMM 053945.2-284910 PKS 0537#54 2.1 25.10 18.91 1.86 >1.3 $^{\dagger}$ - 2.0
HELLAS2XMM 053911.4-283717 PKS 0537#111 2.1 24.50 17.64 1.62 $\rm 1.2^{+0.20}_{-0.10}$ $^{\dagger}$ $\rm 9.1^{12.4}_{5.3}$ 1.7
HELLAS2XMM 000111.6-251202 Abell 2690#29 2.8 25.10 17.67 1.99 2.08 $\rm 2.1^{2.6}_{1.6}$ 8.4
HELLAS2XMM 031018.9-765957 PKS 0312#45 2.8 24.40 18.62 1.70 $\rm 1.85^{+0.20}_{-0.30}$ $^{\dagger}$ $\rm 8.0^{8.4}_{4.6}$ 6.2
HELLAS2XMM 005030.7-520046 BPM 16274#69 2.27 24.08 17.87 1.48 1.35 $\rm 2.5^{1.5}_{1.0}$ 2.4

Notes. (a) Fluxes in units of 10-14 erg cm-2 s-1 from Perola et al. (2004) (with the exception of BPM 16274#69, from Lanzuisi et al., in preparation); (b) magnitude from Fiore et al. (2003) (with the exception of source BPM 16274#69, from Cocchia et al. 2007); (c) for a sub-sample of sources, the $K_{\rm s}$-band analysis can be found in Mignoli et al. (2004); (d) spectroscopic redshift from optical spectroscopy (Fiore et al. 2003) and, for three sources, from near-IR spectroscopy (Abell 2690#29 and BPM 16274#69 from Maiolino et al. 2006; PKS 0537#91 from Sarria et al., in preparation); photometric redshifts ( $^{(\dagger)}$ symbol, and corresponding 1$\sigma $ errors, from Pozzi et al. (2007); (e) column densities in source rest-frame in units of 1022 cm-2 measured from X-ray spectral fitting (see Perola et al. 2004; and Lanzuisi et al., in preparation). For the sources with photometric redshifts, values are taken from Pozzi et al. (2007). For PKS 0537#164 the X-ray spectral fitting is prevented by the few X-ray counts; for Mrk 509#01, only an upper limit was derived (Perola et al. 2004); for PKS 0537#54, the column density is $9.3\times 10^{22}$ cm-2 for z= 1.3. Galactic absorption column densities adopted in the spectral fitting are: $8\times 10^{20}$ cm-2 for the field PKS 0312-77; $2\times 10^{20}$ cm-2 for the field Abell 2690; $2.1\times 10^{20}$ cm-2 for the field PKS 0537-28; $4\times 10^{20}$ cm-2 for the field Mrk 509; $2.5\times 10^{20}$ cm-2 for the field GD 158-100 (see Stark et al. 1992); (f) rest-frame, absorption-corrected, X-ray luminosity in units of 1044 erg s-1 from Perola et al. (2004) and from Pozzi et al. (2007) for sources with photometric redshifts. Luminosities are computed using H0=70 km s-1 Mpc-1, $\Omega_{\rm m}=0.3$ and $\Omega_{\Lambda}=0.7$.


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