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Table 3:

Best-fitting physical parameters and inferred rest-frame properties.

Abbreviation 		$\chi^{2}_{\min}$/d.o.fa $\alpha$b ${\tau}_{9.7~{\mu}{\rm m}}$c $\Theta$d $\tau_{\rm sf}$e E(B-V)f $L_{\rm acc}$g $L_{1-1000_{\rm ~{\mu}m}}^{h}$ $L_{2-10~{\rm keV}}$i $L_{1.25-500~{\rm keV}}$l $L_{\rm bol}$m $k_{2-10~{\rm keV}}$n $M_{\rm star}$o $M_{\rm BH}$p $\lambda _{\rm Edd}$q
PKS 0537#43 66.7/6 -1.0 0.1 140 0.05 0.3 373.6 254 6.8 26.3 400 [400-422] 58.8 49.4 10.05 0.032

PKS 0537#11

 7.8/5 0.0 2.0 140 0.7 0.64 17.6 7.4 1.9 7.6 25.2 [14.1-34.4] 12.9 1.20 0.28 0.070

PKS 0537#164

 9.0/5 0.0 3.0 60 0.15 0.0 99.8 4.9 3.1 12.1 112 [63.0-174] 36.1 1.29 0.30 0.292

PKS 0537#123

 5.0/5 0.0 0.1 140 1.0 0.65 9.5 7.8 2.0 7.8 17.3 [17.3-36.4] 8.6 1.99 0.46 0.030

GD 158#62

 9.3/5 0.0 0.1 100 0.35 0.44 85.1 39.7 4.9 19.0 104 [67.3-214] 21.2 2.19 0.51 0.163

GD 158#19

 26.9/6 0.0 0.3 140 1.0 0.49 397. 289.7 6.3 24.4 422 [422-465] 67.0 12.3 2.64 0.127

Mrk 509#01

 17.9/5 -0.5 6.0 60 0.9 0.85 104.5 1.59 1.5 5.8 111 [42.8-131] 73.6 1.98 0.46 0.191

Mrk 509#13

 25.0/5 0.0 1.0 140 0.6 1.0 23.2 13.0 2.6 10.1 33.3 [27.1-53.9] 12.8 1.93 0.45 0.059

Abell 2690#75

 17.5/5 0.0 1.0 140 0.05 0.18 19.8 11.0 3.2 12.4 32.2 [20.8-66.8] 10.1 2.73 0.62 0.041

PKS 0312#36

 9.6/5 0.0 0.1 140 0.85 0.79 3.0 2.5 0.7 2.7 5.7 [5.7-8.1] 8.2 0.43 0.11 0.043

PKS 0537#91

 2.9/5 0.0 3.0 140 0.25 0.3 66.0 23.7 8.1 31.4 98.3 [40.2-326] 12.1 1.48 0.35 0.224

PKS 0537#54

 2.9/5 0.0 0.1 140 0.05 0.17 5.6 4.6 2.0 7.8 13.3 [13.3-25.8] 6.7 1.72 0.40 0.026

PKS 0537#111

 11.4/5 -0.5 10.0 140 0.05 0.31 103.1 13.4 1.7 6.6 110 [34.1-110] 64.4 4.61 1.03 0.084

Abell 2690#29

 0.5/2 0.0 1.0 140 0.15 0.55 168.8 94.7 8.4 32.6 201 [135-264] 23.9 17.9 3.80 0.042

PKS 0312#45

 0.5/5 0.0 0.1 100 0.25 0.48 24.25 11.3 6.2 24.0 48.3 [37.4-239] 7.8 3.61 0.81 0.047

BPM 16274#69

 0.5/5 0.0 0.6 140 0.05 0.25 11.4 7.3 2.4 9.3 20.7 [18.2-56.6] 8.6 4.68 1.05 0.016

Notes. (a) Best-fitting minimum $\chi ^{2}$ and number of degrees of freedom; (b-d) best-fitting torus parameters ($\alpha$: exponent of the power law parameterizing the density profile; ${\tau}_{9.7~{\mu}{\rm m}}$: 9.7 $\mu $m optical depth, $\Theta$: torus opening angle). The ratio parameter $R_{\max}/R_{\min}$ is frozen to 30; the density parameter $\gamma$ is frozen to 0; (e, f) best-fitting stellar parameters ( $\tau_{\rm sf}$: duration of the exponential decay of the burst in units of the oldest SSP; E(B-V): extinction); (g) accretion-disk model luminosity (from soft X-ray to IR frequencies) which represents the torus model input luminosity, in units of 1044 erg s-1; (h) torus luminosity in units of 1044 erg s-1 (not corrected, see Sect. 6.1); (i) absorption-corrected luminosity in units of 1044 erg s-1; (l) hard-X-ray luminosity in units of 1044 erg s-1 (derived from the 2-10 keV luminosity, see Sect. 6.2); (m) bolometric AGN luminosity ( $L_{\rm acc}$+ $L_{1.25-500~{\rm keV}}$) in units of 1044 erg s-1; the 1$\sigma $ range derived from the SED-fitting analysis is reported; (n) 2-10 keV bolometric correction ( $L_{\rm bol}/L_{2-10~{\rm keV}}$); (o) galaxy masses in units of 10 $^{11}~M_{\odot}$; (p) black hole masses in units of 10 $^{9}~M_{\odot}$ (estimated from Marconi & Hunt 2003, relation); (q) Eddington ratios ( $L_{\rm bol}/L_{\rm Edd}$).


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