Table C.1.
Other properties of combined sample.
Source | DL | log(Mout) | tflow | Ṁout | log(Pkin) | log(Ṁoutv) | log(ΣFIR) | log(LBol) | log(LAGN) | Ref. (AGN) |
---|---|---|---|---|---|---|---|---|---|---|
(Mpc) | (M⊙) | (Myr) | (M⊙ yr−1) | (erg s−1) | (g cm s−2) | (L⊙ kpc−2) | (L⊙) | (L⊙) | ||
NGC 253 | 3.40 | 7.20 | 4.30 | 3.71 | 39.47 | 33.07 | 12.14 | 10.58 | <7.07 | Cicone et al. (2014) |
I Zw 1 | 273.98 | <7.62 | 10.87 | 12.01 | 11.96 | Veilleux et al. (2013) | ||||
III Zw 035 | 119.91 | 8.59 | 6.88 | 56.70 | 42.24 | 35.05 | 11.81 | 11.71 | <7.76 | González-Martín et al. (2015) |
PG 0157+001 | 781.80 | 7.99 | 1.54 | 63.81 | 42.51 | 35.21 | > 11.18 | 12.68 | 12.50 | Veilleux et al. (2013) |
NGC 1068 | 14.40 | 6.93 | 1.02 | 8.27 | 40.42 | 33.72 | 11.36 | 11.37 | 10.15 | Ricci et al. (2017) |
NGC 1266 | 29.90 | 7.67 | 1.21 | 38.31 | 42.10 | 34.89 | > 11.89 | 10.54 | 9.73 | Cicone et al. (2014) |
IRAS F03158+4227 | 632.90 | 8.88 | 6.92 | 110.83 | 43.43 | 35.79 | 12.68 | 12.36 | Fluetsch et al. (2019) | |
NGC 1377 | 21.00 | 6.88 | 1.42 | 5.36 | 40.51 | 33.67 | > 11.49 | 10.09 | 9.35 | Cicone et al. (2014) |
NGC 1433 | 9.90 | 5.82 | 0.94 | 0.70 | 39.34 | 32.64 | 9.24 | 8.32 | Fluetsch et al. (2019) | |
NGC 1614 | 68.88 | 7.51 | 1.52 | 21.33 | 41.94 | 34.68 | 11.21 | 11.73 | <8.94 | Brightman & Nandra (2011) |
IRAS F05081+7936 | 239.20 | 7.98 | 1.22 | 28.23 | 43.20 | 35.60 | 10.61 | 12.05 | <8.79 | Fluetsch et al. (2019) |
IRAS F05189−2524 | 189.47 | 7.87 | 2.30 | 32.56 | 42.31 | 34.96 | 11.78 | 12.22 | 12.09 | Veilleux et al. (2013) |
NGC 2146 | 17.20 | 7.94 | 10.20 | 8.49 | 41.03 | 34.03 | 10.46 | 11.16 | <7.51 | Cicone et al. (2014) |
NGC 2623 | 80.03 | 7.05 | 1.01 | 11.21 | 42.09 | 34.62 | 11.93 | 11.62 | 10.62 | Evans et al. (2008) |
NGC 2623 fossil | 6.66 | 12.80 | 0.36 | 40.26 | 32.96 | |||||
IRAS F08572+3915 | 260.32 | 8.56 | 1.00 | 363.80 | 43.87 | 36.26 | 11.73 | 12.20 | 12.06 | Veilleux et al. (2013) |
IRAS F09111−1007 W | 242.11 | 8.01 | 1.81 | 57.12 | 42.29 | 35.08 | 11.64 | 12.01 | <10.80 | Nardini et al. (2010) |
M 82 | 3.90 | 7.86 | 9.78 | 7.34 | 40.36 | 33.67 | 11.08 | 10.90 | <7.96 | Cicone et al. (2014) |
IRAS F10035+4852 | 291.20 | <8.45 | 12.06 | <11.52 | Fluetsch et al. (2019) | |||||
IRAS F10173+0828 | 217.64 | <7.29 | 11.77 | 11.90 | <8.18 | Iwasawa et al. (2011) | ||||
NGC 3256 N | 35.00 | 7.26 | 0.57 | 31.93 | 42.69 | 35.15 | 10.79 | 11.60 | <8.39 | Cicone et al. (2014) |
NGC 3256 S | 7.13 | 1.33 | 10.11 | 41.90 | 34.50 | |||||
IRAS F10565+2448 | 190.70 | 8.34 | 2.39 | 91.90 | 42.77 | 35.42 | 11.54 | 12.12 | 11.79 | Veilleux et al. (2013) |
IRAS F11119+3257 | 920.20 | 8.75 | 6.85 | 81.43 | 43.41 | 35.71 | 12.72 | 12.63 | Veilleux et al. (2013) | |
NGC 3628 | 7.70 | 6.98 | 4.46 | 2.13 | 39.74 | 33.08 | 11.13 | 10.08 | <7.21 | Cicone et al. (2014) |
ESO 320−G030 | 46.60 | 6.81 | 2.36 | 2.76 | 41.00 | 33.77 | 11.28 | 11.33 | <9.33 | Alonso-Herrero et al. (2012) |
IRAS F12112+0305 SW | 330.34 | 7.53 | 2.31 | 14.62 | 41.68 | 34.47 | 12.38 | 11.64 | Veilleux et al. (2013) | |
IRAS F12112+0305 NE | 8.80 | 3.36 | 188.41 | 43.11 | 35.74 | |||||
IRAS F12224−0624 | 115.71 | 6.95 | 0.46 | 19.42 | 42.29 | 34.84 | 11.83 | 11.35 | <10.75 | This work |
NGC 4418 | 25.35 | 5.73 | 0.09 | 6.29 | 41.32 | 34.11 | 12.50 | 10.94 | 10.68 | Veilleux et al. (2013) |
Mrk 231 | 186.42 | 8.43 | 0.84 | 323.84 | 43.70 | 36.15 | > 12.26 | 12.61 | 12.51 | Veilleux et al. (2013) |
IC 860 | 56.11 | <6.55 | 12.07 | 11.19 | <9.19 | Alonso-Herrero et al. (2012) | ||||
IRAS 13120−5453 | 136.14 | 8.18 | 1.35 | 111.53 | 42.50 | 35.33 | 11.99 | 12.33 | 11.85 | Veilleux et al. (2013) |
Mrk 273 | 166.43 | 8.21 | 0.83 | 196.30 | 43.42 | 35.91 | > 12.13 | 12.24 | 11.77 | Veilleux et al. (2013) |
4C 12.50 | 568.50 | <8.11 | 12.41 | 12.11 | Fluetsch et al. (2019) | |||||
SDSS J135646.10+102609.0 | 574.70 | 8.09 | 0.59 | 207.49 | 43.21 | 35.82 | 12.43 | 12.41 | Sun et al. (2014) | |
IRAS F14348−1447 SW | 375.26 | 8.76 | 3.80 | 151.34 | 42.92 | 35.60 | 12.42 | 11.66 | Veilleux et al. (2013) | |
IRAS F14348−1447 NE | 8.05 | 2.44 | 45.91 | 42.30 | 35.03 | |||||
IRAS F14378−3651 | 306.70 | <7.87 | 11.81 | 12.26 | 11.59 | Veilleux et al. (2013) | ||||
Zw 049.057 | 56.40 | 6.96 | 0.26 | 35.09 | 42.00 | 34.82 | 11.90 | 11.26 | <9.26 | Alonso-Herrero et al. (2012) |
Arp 220 | 78.70 | 7.02 | 0.19 | 54.93 | 42.40 | 35.12 | 12.53 | 12.24 | 11.01 | Veilleux et al. (2013) |
Mrk 876 | 605.21 | 9.38 | 3.31 | 720.05 | 44.40 | 36.68 | 10.70 | 12.30 | 12.17 | Ricci et al. (2017) |
NGC 6240 | 106.81 | 8.59 | 1.43 | 272.00 | 43.24 | 35.89 | 11.28 | 11.91 | 11.66 | Veilleux et al. (2013) |
IRAS F17020+4544 | 270.52 | 8.27 | 0.59 | 315.95 | 44.44 | 36.52 | 11.61 | 11.13 | Giroletti et al. (2017) | |
IRAS F17132+5313 | 226.60 | <8.16 | 12.00 | 8.70 | Iwasawa et al. (2011) | |||||
IRAS F17207−0014 | 189.20 | 7.52 | 3.33 | 98.96 | 43.59 | 35.84 | 11.97 | 12.48 | <11.18 | Veilleux et al. (2013) |
PDS 456 | 898.60 | 8.61 | 3.37 | 120.03 | 43.39 | 35.83 | 13.42 | 13.41 | Bischetti et al. (2019) | |
NGC 6764 | 32.00 | 6.44 | 20.00 | 0.14 | 38.09 | 31.67 | 10.46 | 8.65 | Cicone et al. (2014) | |
IRAS F20100−4156 | 608.20 | 8.86 | 2.43 | 295.08 | 43.90 | 36.24 | 12.73 | 12.16 | Spoon et al. (2013) | |
IC 5063 | 48.71 | 7.23 | 0.90 | 18.61 | 42.17 | 34.77 | 10.24 | 10.92 | 10.84 | Ricci et al. (2017) |
IRAS F20551−4250 | 190.20 | 7.43 | 0.46 | 59.44 | 42.65 | 35.26 | 11.64 | 12.11 | 11.87 | Veilleux et al. (2013) |
IRAS F22491−1808 | 352.74 | 8.13 | 1.55 | 86.73 | 42.46 | 35.25 | 11.26 | 12.26 | 11.42 | Veilleux et al. (2013) |
NGC 7479 | 34.31 | <6.22 | 11.31 | 10.89 | 9.95 | Ricci et al. (2017) | ||||
IRAS F23060+0505 | 834.25 | 9.42 | 5.66 | 463.76 | 43.85 | 36.31 | 12.59 | 12.48 | Cicone et al. (2014) | |
IRAS 23365+3604 | 289.17 | 8.12 | 2.67 | 49.46 | 42.50 | 35.15 | 11.65 | 12.27 | 11.92 | Veilleux et al. (2013) |
Notes. Molecular outflow masses, flow times, and outflow rates for the combined sample, as computed using the observed quantities from Tables 3 and 4. We also list adopted distances, far-infrared surface brightnesses (from Lutz et al. 2016, 2018), and bolometric and AGN luminosities. Some references quote AGN fractions to the bolometric luminosity which we have converted to LAGN for consistency. The limit for IRAS F12224−0624 was estimated from Spitzer-IRS data with methods as used by Veilleux et al. (2013). We note that AGN luminosities are a mixture of X-ray-based (reacting rapidly to accretion variations) and mid-infrared-based (averaging over typically tens of years).
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