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Table 3

Properties of the extended sample of galaxies.

Object Type z CO SFR log(Pkin,SF) α CO(1 − 0) log (MH2,TOT)† log (LAGN) LAGN/LBol Refs.
[M⊙ yr-1] [erg s-1] [M⊙/(K   km   s-1   pc2)] [M⊙] [erg s-1]
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)
IRAS F08572+3915 Sy 2 0.05821 20 43.15 0.8 9.18 45.72 0.860 1, b
IRAS F10565+2448 Sy 2 0.04311 95 43.82 0.8 9.90 44.81 0.170 1, c
IRAS 23365+3604 LINER 0.06438 137 43.98 0.8 9.93 44.67 0.072 1, b
Mrk 273 Sy 2 0.03777 139 43.99 0.8 9.70 44.73 0.080 1, a
IRAS F23060+0505 Sy 2 0.17300 75 43.72 0.8 10.39 46.06 0.780 1, b
Mrk 876 Sy 1 0.12900 6.5 42.66 0.8 9.84 45.84 0.930 1, d
I Zw 1 Sy 1 0.06114 36 43.40 0.8 9.56 45.37 0.520 1, d
Mrk 231 Sy 1 0.04217 234 44.21 0.8 9.73 45.72 0.340 2, b
NGC 1266 LINER 0.00719 1.6 42.05 4.4 9.23 43.31 0.250 3, f
M 82 HII 0.00068 10 42.85 1.2 8.64 ≤41.54 ≤0.00090 4, i
NGC 1377 LINER 0.00578 0.9 41.80 4.4 8.44 42.93 0.200 5, f
NGC 6240 Sy 2 0.02448 16 43.05 0.8 9.86 45.38 0.780 6, e
NGC 3256 HII 0.00926 36 43.40 1.2 9.68 ≤41.97 ≤0.00070 7, j
NGC 3628 HII 0.00280 1.8 42.10 1.2 9.53 ≤40.79 ≤0.00090 8, k
NGC 253 HII 0.00081 3 42.32 1.2 8.15 ≤40.66 ≤0.00040 9, j
NGC 6764 LINER 0.00807 2.6 42.26 1.2 8.90 42.23 0.017 10, g
NGC 1068 Sy 2 0.00379 18 43.10 0.8 9.11 43.94 0.097 11, h
IC 5063 Sy 2 0.01100 0.6 41.62 4.4 8.85 44.30 0.900 12, l
NGC 2146 HII 0.00298 12 42.92 1.2 8.94 ≤41.09 ≤0.00030 13, m

Notes. (1) Name; (2) optical classification; (3) redshift based on the CO spectrum; (4) star formation rate; (5) kinetic energy associated with the supernovae; (6) CO-to-H2 conversion factor adopted to infer MH2 from the CO(1–0) luminosity; (7) total mass of molecular gas; (8) AGN bolometric luminosity; (9) ratio between the bolometric luminosity of the AGN and the total bolometric luminosity of the galaxy; (10) references for the CO fluxes used to estimate MH2: 1 – this work; 2 – Cicone et al. (2012); 3 – Alatalo et al. (2011); 4 – Walter et al. (2002); 5 – Aalto et al. (2012b); 6 – Feruglio et al. (2013a,b); 7 – Sakamoto et al. (2006b); 8 – Tsai et al. (2012); 9 – Mauersberger et al. (1996); 10 – Sanders & Mirabel (1985); 11 – Maiolino et al. (1997); 12 – Wiklind et al. (1995); 13 – Tsai et al. (2009); references for LAGN: a – Nardini et al. (2009); b – Nardini et al. (2010); c – Veilleux et al. (2009); d – Piconcelli et al. (2005); e – Risaliti (priv. comm.); f – Moustakas & Kennicutt (2006); g – Croston et al. (2008); h – Prieto et al. (2010); i – Verrecchia et al. (2007); j – Ranalli et al. (2003); k – González-Martín et al. (2009); l – Koyama et al. (1992); m – della Ceca et al. (1999), Inui et al. (2005).

(†)

In these cases of NGC 1377 and NGC 3256, we estimate the total molecular gas mass by using the CO(2–1) transition (instead of the CO(1–0)), by assuming that the CO gas is thermalised and optically thick, i.e. that .

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