Table 4.
Adopted CO(1-0) outflow parameters for literature sources.
| Source | Jup | SCO (wings) | vout | Rout | Reference |
|---|---|---|---|---|---|
| (Jy km s−1) | (km s−1) | (″) | |||
| NGC 253 | 1 | 707.00 | 50 | 13.35 | Bolatto et al. (2013b) |
| I Zw 1 | 1 | < 0.30 | Cicone et al. (2014) | ||
| PG 0157+001 | 3 | 0.86 | 402 | 0.23 | Fluetsch et al. (2019) |
| NGC 1068 | 3 | 98.00 | 100 | 1.50 | García-Burillo et al. (2014) |
| NGC 1266 | 1 | 26.70 | 322 | 2.75 | Alatalo et al. (2011) |
| IRAS F03158+4227 | 1 | 1.11 | 876 | 2.60 | Gowardhan et al. (2018) |
| NGC 1377 | 2 | 29.77 | 138 | 1.96 | Aalto et al. (2012b) |
| NGC 1433 | 3 | 16.10 | 100 | 2.00 | Combes et al. (2013) |
| NGC 1614 | 1 | 3.55 | 360 | 1.73 | García-Burillo et al. (2015) |
| IRAS F05081+7936 | 1 | 0.90 | 800 | 0.96 | Leroy et al. (2015b) |
| NGC 2146 | 1 | 1450.0 | 200 | 25.00 | Tsai et al. (2009) |
| IRAS F08572+3915 | 1 | 2.91 | 800 | 0.73 | Cicone et al. (2014) |
| M 82 | 1 | 2413.33 | 100 | 53.00 | Walter et al. (2002) |
| IRAS F10035+4852 | 1 | < 1.80 | Leroy et al. (2015b) | ||
| NGC 3256 N | 1 | 7.65 | 700 | 2.40 | Sakamoto et al. (2014) |
| NGC 3256 S | 1 | 5.65 | 500 | 4.00 | Sakamoto et al. (2014) |
| IRAS F10565+2448 | 1 | 3.22 | 450 | 1.30 | Cicone et al. (2014) |
| IRAS F11119+3257 | 1 | 0.40 | 1000 | 2.22 | Veilleux et al. (2017) |
| NGC 3628 | 1 | 82.00 | 90 | 11.00 | Tsai et al. (2012) |
| ESO 320−G030 | 2 | 5.21 | 340 | 3.71 | Pereira-Santaella et al. (2016) |
| IRAS F12112+0305 SW | 2 | 0.57 | 324 | 0.55 | Pereira-Santaella et al. (2018) |
| IRAS F12112+0305 NE | 2 | 10.70 | 465 | 1.15 | Pereira-Santaella et al. (2018) |
| Mrk 231 | 1 | 4.16 | 700 | 0.72 | Cicone et al. (2012) |
| Mrk 273 | 1 | 3.11 | 650 | 0.73 | Cicone et al. (2014) |
| 4C 12.50 | 1 | < 0.18 | 640 | 0.07 | Dasyra & Combes (2012), Dasyra et al. (2014) |
| SDSSJ135656.10+102609.0 | 3 | 0.99 | 500 | 0.14 | Sun et al. (2014) |
| IRAS F14348−1447 SW | 2 | 7.60 | 419 | 1.05 | Pereira-Santaella et al. (2018) |
| IRAS F14348−1447 NE | 2 | 1.48 | 373 | 0.60 | Pereira-Santaella et al. (2018) |
| Zw 049.057 | 2 | 5.00 | 300 | 0.30 | Falstad et al. (2018) |
| Arp 220 | 1 | 0.88 | 380 | 0.20 | Barcos-Muñoz et al. (2018) |
| Mrk 876 | 1 | 3.75 | 1050 | 1.54 | Cicone et al. (2014) |
| NGC 6240 | 1 | 17.80 | 450 | 1.33 | Feruglio et al. (2013) |
| IRAS F17020+4544 | 1 | 1.37 | 1670 | 0.86 | Longinotti et al. (2018) |
| IRAS F17132+5313 | 1 | < 1.50 | Leroy et al. (2015b) | ||
| PDS 456 | 3 | 1.42 | 900 | 1.00 | Bischetti et al. (2019) |
| NGC 6764 | 1 | 1.40 | 53 | 7.00 | Leon et al. (2007) |
| IRAS F20100−4156 | 1 | 1.12 | 929 | 1.00 | Gowardhan et al. (2018) |
| IC 5063 | 2 | 12.30 | 500 | 2.00 | Dasyra et al. (2016) |
| IRAS F22491−1808 | 2 | 2.00 | 325 | 0.35 | Pereira-Santaella et al. (2018) |
| IRAS F23060+0505 | 1 | 2.26 | 700 | 1.38 | Cicone et al. (2014) |
| IRAS 23365+3604 | 1 | 0.86 | 450 | 1.00 | Cicone et al. (2014) |
Notes. These parameters may differ from those published in the original references. They are reconstructed from the published information in order to be consistent with our adopted separation between line core and line wings, and our definitions for vout and Rout. For consistency, they are not corrected for outflow inclination, even if this is constrained in some original references. See also Sect. 3.2 for details.
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