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Table 1:

X-ray properties.

Name 		ObsID $\rm N_H$ $\Gamma$ kT E EW $ \log L_{\rm X}$ $\log L_{\rm FIR}$ class. Ref.
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
VII Zw031 7887 <0.12 $1.92^{\rm +0.47}_{-0.32}$ -     41.38 11.71 - x
05189-2524 2034 $7.6^{\rm +0.85}_{-0.94}$ $1.75^{\rm +0.18}_{-0.23}$ $0.07_{-0.11}^{\rm +0.07}$     43.30 11.83 Sy2 x, a
Arp55 6857 <0.92 $2.65_{-0.83}^{\rm +5.3}$ -     40.10 11.48 - x, b
09320+6134$\dagger$ 2033 <0.3 $1.17_{-0.21}^{\rm +0.57}$ - $6.76\pm0.04$ $3500^{\rm +1500}_{-1300}$ 41.56 11.74 L x, a, b
10565+2448 3952 $0.18_{-0.08}^{\rm +0.08}$ 2.13-0.24+0.24 -     41.19 11.78 - x, d
12112+0305 4934 <1.2 $2.78^{\rm +1.21}_{-0.99}$ -     40.36 12.09 L x, d
Mrk231$\dagger$ - $273^{\rm +100}_{-68}$ $2.95^{\rm +0.15}_{-0.16}$   $6.39^{\rm +0.17}_{-0.15}$ $180^{\rm +170}_{-150}$ 42.41 12.15 QSO e, h, a
Arp193 7811 $0.10^{\rm +0.08}_{-0.10}$ $1.71^{\rm +0.38}_{-0.36}$ -     40.99 11.41 - x
Mrk273 809 $46.7_{-5.4}^{\rm +7.0}$ 2. $0.96^{\rm +0.05}_{-0.07}$ $6.59\pm 0.04$ $220^{\rm +120}_{-100}$ 42.99 11.93 Sy2 x, f, a
Arp220$\dagger$ 869 $0.43^{\rm +0.54}_{-0.28}$ $1.11_{-0.28}^{\rm +0.52}$ $0.92_{-0.05}^{\rm +0.15}$     40.95 11.96 L x, a, j, k
NGC 6240$\dagger$ - $179^{\rm +40}_{-15}$ $1.98^{\rm +0.25}_{-0.16}$   $6.50^{\rm +0.15}_{-0.07}$ $1880^{\rm +1590}_{-730}$ 42.01 11.57 L h, g, a
17208-0014 2035 $0.13_{-0.09}^{\rm +0.10}$ $1.66_{-0.30}^{\rm +0.26}$ -     41.28 12.17 HII x
NGC7469 - <0.03 $2.05^{\rm +0.02}_{-0.03}$   $6.35^{\rm +0.14}_{-0.07}$ $84^{\rm +20}_{-19}$ 43.27 11.30 Sy1.5 h
23365+3604 4115 <0.4 $1.2^{\rm +0.47}_{-0.43}$ -     41.38 11.96 L x, i

Notes.  The columns are: (1) Name; A $\dagger$ denotes candidate Compton-thick sources. (2) Chandra Observation ID in the case where we performed our own spectral fits. (3) Column density in units of $10^{22}~\rm cm^{-2}$. (4) Power-law photon index. (5) Temperature of the thermal component in keV. (6) Energy of the FeK$\alpha$ line in keV. (7) EW of the FeK$\alpha$ line in eV. (8) Logarithm of the absorbed hard (2-10 keV) X-ray luminosity (erg s-1). (9) Logarithm of the far-infrared luminosity (40-100 $\rm\mu m$) in units of solar luminosity. (10) Optical classification according to Veilleux et al. (1999) or the NASA Extragalactic Database. (11) X-ray reference: a. Ptak et al. (2003), b. González-Martin et al. (2009), c. Imanishi et al. (2003) d. Iwasawa et al. (2009) e. Braito et al. (2004) f. Xia et al. (2002) g. Vignati et al. (1999) h. Dadina (2007) i. Teng et al. (2005) j. Clements (2002) k. Iwasawa et al. (2005) x. this work.


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