Table 2.
LHCN − vib and outflow properties.
| Name | LHCN − vib | LHCN − vib/LIR | v50(abs)a | Observatory | References |
|---|---|---|---|---|---|
| (103 L⊙) | (10−8) | (km s−1) | |||
| J = 3 − 2 | |||||
| NGC 4418 | 5.0 ± 1.2 | 3.77 ± 0.71 | 111 | SMA | 1 |
| IC 860 | 4.2 ± 0.8 | 2.65 ± 0.37 | not obs. | PdBI | 2 |
| Zw 049.057 | 7.3 ± 2.0 | 3.57 ± 0.76 | 37 | PdBI | 2 |
| NGC 7469 | < 0.1 | < 0.03 | emi. | ALMA | 3 |
| I Zw 1 | < 1.7 | < 0.21 | emi. | ALMA | 3 |
| UGC 5101 | 20.5 ± 5.5 | 2.15 ± 0.50 | −9 | NOEMA | 4 |
| IRAS 20551–4250 | 2.3 ± 0.7 | 0.21 ± 0.06 | −381 | ALMA | 5 |
| IRAS 15250+3609 | < 11.3b | < 1.02 | 189 | ALMA | 3 |
| IRAS 08572+3915 NW | < 6.4 | < 0.48 | −489 | ALMA | 3 |
| IRAS 22491–1808 E | 13.2 ± 3.9 | 0.95 ± 0.25 | 99 | ALMA | 3 |
| Mrk 273 | < 16.9 | < 1.14 | −201 | NOEMA | 6 |
| IRAS 20414-1651 | < 7.5 | < 0.50 | −32 | ALMA | 3 |
| Arp 220 W | 40.9 ± 7.0 | 2.37 ± 0.25c | 21 | ALMA | 7 |
| Arp 220 E | 8.9 ± 1.5 | 0.51 ± 0.05c | 21 | ALMA | 7 |
| IRAS 12112+0305 NE | 14.3 ± 4.0 | 0.70 ± 0.17c | −117 | ALMA | 3 |
| Mrk 231 | 14.5 ± 3.1 | 0.42 ± 0.07 | −237 | PdBI | 8 |
| J = 4 − 3 | |||||
| NGC 4418 | 12.4 ± 2.5 | 9.41 ± 1.25 | 111 | SMA | 1 |
| IRAS 12224–0624 | 16.9 ± 4.5 | 8.52 ± 1.95 | not obs. | ALMA | 9 |
| IRAS 20551–4250 | 4.8 ± 1.2 | 0.45 ± 0.09 | −381 | ALMA | 10 |
| IRAS 05189–2524 | 8.0 ± 2.7 | 0.59 ± 0.18 | −387d | ALMA | 9 |
| Arp 220 W | 108.1 ± 19.9 | 6.27 ± 0.77 | 21 | ALMA | 7 |
| Arp 220 E | 25.8 ± 4.4 | 1.49 ± 0.15 | 21 | ALMA | 7 |
| IRAS 13120–5453 | < 5.5 | < 0.29 | −195 | ALMA | 11 |
| IRAS 17208–0014 | 101.9 ± 17.5 | 3.89 ± 0.40 | 51 | ALMA | 2 |
Notes.
Median OH outflow velocities taken from Veilleux et al. (2013) or, for sources not in their sample, from archival data following the same procedure. Sources that were not observed or where the doublet was detected in emission are indicated with not obs. or emi., respectively. The typical uncertainty on the velocities is 50 km s−1.
Imanishi et al. (2016a) interpreted an emission feature at the position of the HCN-vib line as a subpeak of the nearby HCO+ line. We use this value as an upper limit to the HCN-vib luminosity.
The LHCN − vib/LIR is calculated using the total LIR of the system, possibly introducing some bias in systems with multiple nuclei.
The median velocity of the lines in IRAS 05189–2524 is adjusted to correct for the different redshift adopted compared to that used by Veilleux et al. (2013).
References. (1) Sakamoto et al. (2010); (2) Aalto et al. (2015a); (3) Imanishi et al. (2016a); (4) König et al. (in prep.); (5) Imanishi et al. (2016b); (6) Aladro et al. (2018); (7) Martín et al. (2016); (8) Aalto et al. (2015b); (9) This work; (10) Imanishi & Nakanishi (2013); (11) Privon et al. (2017).
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