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Table 1:

Characteristics of our type 1 AGN mid-IR spectroscopic sample.

Object 		Typea z DLb log Luminosities (erg/s) Object scales
      (Mpc) $L_{\rm X}$ ($N_{\rm H}$)c $L_{\rm V}$d $L_{\rm [O {\sc iii}]}$e $L_{\rm 12~\rm\mu m}$f $r_{\rm sub}$g (pc) 8 $\rm\mu m$ (pc)h res. ( $r_{\rm sub}$)
NGC 3227 S1.5 0.0049  20.4 42.40 (22.80) 42.20 40.51 42.63 0.014  24.2 1680
NGC 3783 S1.5 0.0108  44.7 43.19 (22.47) 42.98 41.30 43.57 0.035  52.5 1482
NGC 4593 S1.0 0.0101  42.0 42.89 (20.30) 42.88 40.69 43.18 0.032  49.5 1560
ESO 323-G77 S1.2 0.0159  66.3 42.76 (23.25) 43.91 41.05 43.75 0.104  77.1  741
MCG-6-30-15 S1.5 0.0087  35.8 42.86 (21.67) 43.41 40.36 43.09 0.058  42.3  727
IC 4329A S1.2 0.0170  70.5 43.87 (21.65) 44.11 41.21 44.20 0.131  82.0  625
MARK 509 S1.5 0.0335 141   43.94 (20.70) 44.01 42.29 44.25 0.116 158   1365
NGC 7213 S1.5L 0.0051  21.2 42.33 (20.60) 42.76 39.87 42.50 0.028  25.2  913
NGC 7469 S1.5 0.0151  62.7 43.33 (20.61) 43.09 41.44 43.87 0.040  73.1 1808

Notes. (a) AGN types from Veron-Cetty & Veron (2006): S: Seyfert, L: LINER; (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 for NGC 3227 (Tueller et al. 2008), logarithmic intrinsic Hydrogen column densities $N_{\rm H}$ in units of cm-2 from Tueller et al. (2008), except ESO 323-G77 (average of Beckmann et al. 2006; Malizia et al. 2007); (d)  $L_{\rm V}\equiv\nu L_\nu$(5500 $\AA$); from Bentz et al. (2009), except NGC 7213 (Winkler 1992), ESO 323-G77 (Schmid et al. 2003), and MCG-6-30-15 (Bennert et al. 2006). Additional extinction correction applied to IC 4329A and ESO 323-G77 (Winkler et al. 1992), and NGC 3783 (AV=1.0 from H$\alpha $/H$\beta$; de Grijp et al. 1992); (e) [O III] total line fluxes from Schmitt et al. (2003) (NGC 3783, NGC 4593, MCG-6-30-15, NGC 7213), Meléndez et al. (2008) (NGC 3227, IC 4329A, MARK 509, NGC 7469), and Schmid et al. (2003) (ESO 323-G77); (f)  $L_{\rm 12~\rm\mu m}\equiv\nu L_\nu(12~\rm\mu m)$; this work; (g) from the fit to K-band reverberation mapping data as shown in Kishimoto et al. (2007); observed U-J or U-K time lag radii: 0.071 pc (NGC 3783), 0.084 pc (MARK 509), 0.044 pc (NGC 7469); (h) spatial scale corresponding to the 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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