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Table 2:

Characteristics of our type 2 AGN mid-IR spectroscopic sample.

Object 		Typea z DLb log Luminosities (erg/s) Object scales
      (Mpc) $L_{\rm X}$ ($N_{\rm H}$)c $L_{\rm [O {\sc iii}]}$d $L_{\rm 12~\rm\mu m}$e $r_{\rm sub}$f (pc) 8 $\rm\mu m$ (pc)g res. ( $r_{\rm sub}$)
NGC 2110 S1i 0.0080  33.2 42.60 (22.57) 40.35 43.00 0.028  39.2 1392
ESO 428-G14 S2 0.0063  26.0 $\ldots$ (>24) 40.62 42.73 0.020  30.8 1509
MCG-5-23-16 S1i 0.0095  39.5 43.24 (22.47) 40.63 43.53 0.052  46.6  900
NGC 4507 S1h 0.0128  53.0 43.34 (23.46) 41.57 43.69 0.062  62.1 1004
MCG-3-34-64 S1h 0.0176  73.2 42.78 (23.69) 41.45 44.14 0.104  84.9  814
NGC 5643 S2 0.0047  19.2 $\ldots$ (>24) 40.55 42.49 0.016  22.9 1471
NGC 5995 S1.9 0.0257 107   43.52 (21.95) 42.01 44.06 0.095 122   1294
IC 5063 S1h 0.0109  45.3 42.87 (23.28) 41.28 43.82 0.072  53.2  737
NGC 7582 S1i 0.0044  18.3 42.04 (22.98) 40.15 42.71 0.020  21.8 1093
NGC 7674 S1h 0.0277 116   43.72 (24.00) 41.93 44.26 0.120 132   1103

Notes. (a) AGN types from Veron-Cetty & Veron (2006): S: Seyfert, L: LINER, S1i: optical type 2 with broad Hydrogen lines in the infrared; S1h: type 2 with detected polarized optical broad lines; (b) luminosity distance based on CMB reference frame redshifts from NED and H0=73, $\Omega_{\rm m}=0.27$, and $\Omega_{\rm vac}=0.73$; (c) $L_{\rm X}$ = absorption-corrected 2-10 keV luminosity from Dadina (2007), except IC 5063 (Tueller et al. 2008), MCG-3-34-64 and NGC 4507 (Hönig et al. 2008a), NGC 5995 (Horst et al. 2008), and NGC 7674 (Bianchi et al. 2005); logarithmic intrinsic Hydrogen column densities in units of 1022 cm-2 from Tueller et al. (2008), except ESO 428-G14 (Della Ceca et al. 2008), NGC 5643 (Maiolino et al. 1998), and NGC 7674 (Bianchi et al. 2005, changing-look AGN); (d) [O III] fluxes from Schmitt et al. (2003) (NGC 4507, IC 5063, NGC 7674), Meléndez et al. (2008) (NGC 5643, NGC 7582), Gu et al. (2006) (ESO 428-G14, MCG-3-34-64), Haas et al. (2007) (NGC 2110), Winkler (1992) (MCG-5-23-16), and Tran (2003) (NGC 5995); (e)  $L_{\rm 12~\rm\mu m}\equiv\nu L_\nu(12~\rm\mu m)$; this work; (f) based on Eq. (1); (g) theoretical diffraction limit for a 8.2 m VLT telescope: 0 $\hbox{$.\!\!^{\prime\prime}$ }$25 at 8 $\rm\mu m$, 0 $\hbox{$.\!\!^{\prime\prime}$ }$31 at 10 $\rm\mu m$, 0 $\hbox{$.\!\!^{\prime\prime}$ }$37 at 12 $\rm\mu m$.


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