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Table 1.

Galaxies analyzed in this work along with some general properties.

Galaxy name z RA Dec αAGN log LIR log LAGN SFR OHmax ( † ) OHEQW ( † ) Ref.
[L⊙] [L⊙] [M⊙ yr−1] [km s−1] [km s−1]
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
IRAS 00188−0856 0.1284 00:21:26.522 −08:39:25.98 0.51 12.39 12.16 120±50 ( * ) −1781 −305 γ
IRAS 01003−2238 0.1178 01:02:50.007 −22:21:57.22 0.83 12.32 12.30 36±14 −1238 −276 γ
IRAS F01572+0009 0.1631 01:59:50.253 +00:23:40.87 0.65 12.62 12.49 150±60 ( * ) −1100:: 0 β
IRAS 03521+0028 0.1519 03:54:42.219 +00:37:03.41 0.06 12.52 11.39 309±120 −100 −26 γ
IRAS F05024−1941 0.1935 05:04:36.555 −19:37:02.83 0.07 12.37 11.30 220±80 ( * ) −850:: −83 β
IRAS F05189−2524 0.0426 05:21:01.392 −25:21:45.36 0.72 12.16 12.07 40±16 ( * ) −850 −10 β
IRAS 06035−7102 0.0795 06:02:54.066 −71:03:10.48 0.60 12.22 12.06 70±30 −1117 −128 γ
IRAS 06206−6315 0.0924 06:21:01.210 −63:17:23.5 0.43 12.23 11.92 100±40 −750 −272 γ
IRAS 07251−0248 0.0876 07 :27:37.544 −02:54:54.67 0.30 12.39 11.92 170±70 ( * ) −550 −56 β
IRAS 08311−2459 0.1005 08:33:20.600 −25:09:33.7 0.79 12.50 12.46 70±30 163 γ
IRAS 09022−3615 0.0596 09:04:12.689 −36:27:00.76 0.55 12.29 12.09 90±30 ( * ) −650 17 β
IRAS 10378+1109 0.1363 10:40:29.169 +10:53:18.29 0.30 12.31 11.85 140±60 −1300 −155 γ
IRAS 11095−0238 0.1066 11:12:03.377 −02:54:22.58 0.49 12.28 12.03 100±40 107 γ
IRAS F12072−0444 0.1286 12:09:45.132 −05:01:13.76 0.75 12.40 12.33 60±20 ( * ) −1200 −51 β
IRAS F12112+0305 0.07309 12:13:45.978 +02:48:40.4 0.18 12.32 11.63 170±70 ( * ) −400 −2 β
IRAS 13120−5453 0.0308 13:15:06.358 −55:09:23.23 0.33 12.24 11.83 120±50 ( * ) −1200 −113 β
IRAS F13305−1739 0.1484 13:33:16.540 −17:55:10.7 0.88 12.26 12.26 23±9 ( * ) β
IRAS F13451+1232 0.1217 13:47:33.425 +12:17:24.32 0.81 12.32 12.29 41±15( * ) 136 β
IRAS F14348−1447 0.0830 14:37:38.317 −15:00:23.29 0.17 12.34 11.64 180±70 ( * ) −900 −25 β
IRAS F14378−3651 0.068127 14:40:59.008 −37:04:31.94 0.21 12.11 11.50 100±40 ( * ) −1200 −119 β
IRAS F15462−0450 0.100283 15:48:56.813 −04:59:33.61 0.61 12.21 12.05 60±20 ( * ) −600: 80 β
IRAS 16090−0139 0.1336 16:11:40.432 −01:47:06.56 0.43 12.55 12.25 200±80 −1422 −332 γ
IRAS 17208−0014 0.0428 17:23:21.920 −00:17:00.7 ≤ 0.05 12.39 11.15 230±90 ( * ) −148 β
IRAS 19254−7245 0.06149 19:31:21.400 −72:39:18.0 0.74 12.09 12.02 32±12 −1126 −130 γ
IRAS F19297−0406 0.08573 19:32:21.250 −03:59:56.3 0.23 12.38 11.81 180±70 ( * ) −1000 −119 β
IRAS 19542+1110 0.0624 19:56:35.786 +11:19:05.45 0.26 12.06 11.52 90±30 ( * ) −700 −29 β
IRAS 20087−0308 0.1057 20:11:23.870 −02:59:50.7 0.20 12.42 11.79 210±80 −812 −386 γ
IRAS 20100−4156 0.1296 20:13:29.540 −41:47:34.9 0.27 12.67 12.16 340±130 −1609 −461 γ
IRAS 20414−1651 0.0871 20:44:18.213 −16:40:16.22 0.00 12.22 < 11.46 170±60 −100 −101 γ
IRAS F20551−4250 0.0430 20:58:26.781 −42:39:00.20 0.57 12.05 11.87 48±19 ( * ) −1200 −70 β
IRAS F22491−1808 0.0778 22:51:49.264 −17:52:23.46 0.14 12.84 12.05 590±220 ( * ) −25 β
IRAS F23060+0505 0.1730 23:08:33.952 +05:21:29.76 0.78 12.53 ⋅ ⋅ ⋅ 80±30 δ
IRAS F23128−5919 0.0446 23:15:46.749 −59:03:15.55 0.63 12.03 11.89 40±15 ( * ) β
IRAS 23230−6926 0.1066 23:26:03.620 −69:10:18.8 0.32 12.37 11.93 160±60 −845 −55 γ
IRAS 23253−5415 0.1300 23:28:06.100 −53:58:31.0 0.23 12.36 11.78 180±70 −650 −134 γ
IRAS F23389+0300 0.1450 23:41:30.306 +03:17:26.44 0.23 12.13 11.54 100±40 ( * ) −600 46 β
IRAS F00509+1225 0.0611 00:53:34.940 +12:41:36.0 0.90 11.95 11.96 36±14 65 β
PG 1126−041 0.0600 11:29:16.729 −04:24:07.25 0.89 11.46 11.47 3±1 ( * ) β
IRAS F12243−0036 0.00708 12:26:54.620 −00:52:39.40 0.56 11.00 10.81 15±6 −63 β
PG 2130+099 0.0630 21:32:27.813 +10:08:19.46 0.92 11.71 11.76 4±2 ( * ) β

Notes. (1) Source name. (2) Redshift. (3) Right ascension. (4) Declination. (5) Reported fractional contribution of the AGN to the bolometric luminosity in the reference papers (αAGN = LAGN/Lbol). (6) Infrared luminosity (8 − 1000 μm), ( * )computed using LIR = Lbol/1.15 for sources retrieved from the reference paper β. (7) Reported AGN luminosity in the reference papers, derived using method 6 by Veilleux et al. (2009b), which uses the 15 to 30 μm continuum ratio (f30/f15) to infer αAGN, resulting in uncertainties of ∼20% on average for the LAGN for sources retrieved from the reference paper β, similar to the method used in the reference paper γ. (8) Star formation rate, computed using SFR = (1 − α)×10−10LIR. (9) In case of a detection of OH outflow through P-Cygni profile, the maximum velocity of the absorption feature is reported according to the reference paper. (10) The equivalent width of the OH 119 μm doublet as reported by the reference papers; a negative equivalent width implies that the absorption component is stronger than the emission component. ( † ) For sources taken from γ, the OH velocities have uncertainties of ±200 km s−1. Sources taken from β have uncertainties typically of 50 km s−1, unless the value is followed by a colon, meaning uncertainties from 50 to 150 km s−1, or a double colon, meaning uncertainties larger than 150 km s−1.

References. β: Veilleux et al. (2013), γ: Spoon et al. (2013).

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