Table 4
Published Herschel-SPIRE [C I] and CO line fluxes.
| Name | Observed line flux | Ref.a | |||||
| CO (4−3) | CO (7−6) | [C I] (1−0) | [C I] (2−1) | CO(2−1) | 13CO (2−1) | ||
| 461 GHz | 807 GHz | 492 GHz | 809 GHz | 230 GHz | 220 GHz | ||
| (10-17 W m-2) | (10-19 W m-2) | ||||||
|
|
|||||||
| NGC 1056 | − | 0.61 | − | 0.77 | 10.4 | − | PS13 |
| NGC 1068/M 77 | 21.7 | 21.1 | 12.8 | 21.1 | 866 | 76 | Sp12, P12* |
| IRAS 09022-3615 | − | 3.33 | 1.22 | 1.52 | − | − | |
| UGC 05101 | − | 1.05 | − | 1.28 | 9.7 | 0.13 | PS13 |
| NGC 3034/M 82 | 113 | 209 | 33.8 | 117 | 2070 | 142 | P10, W03* |
| NGC 3227 | 2.90 | 1.81 | 2.27 | 4.66 | 26.5 | 6.9 | PS13, I |
| NGC 3982 | 1.81 | 0.47 | − | 1.00 | 4.3 | − | PS13 |
| NGC 4038 | 5.47 | 1.48 | 1.00 | 1.86 | 88.2 | 3.7 | Sc14, I |
| NGC 4039 | 2.92 | 1.85 | 1.65 | 2.41 | 109.6 | 7.7 | Sc14, I |
| NGC 4051 | − | 0.73 | − | 0.78 | 24.9 | 1.3 | PS13, I |
| NGC 4151 | − | 0.36 | − | 0.84 | 3.0 | − | PS13 |
| NGC 4388 | 2.39 | 1.31 | 1.45 | 2.67 | 5.5 | − | PS13 |
| IC 3639 | 1.21 | − | − | 0.58 | 20.9 | − | PS13 |
| NGC 5128/Cen A | 11.3 | 4.16 | 11.5 | 30.2 | 172 | 12 | I14* |
| NGC 5236/M 83 | 11.5 | 8.82 | 4.54 | 14.0 | 582 | 62 | K14, IB01, * |
| NGC 7130 | 3.30 | 2.55 | 1.64 | 2.67 | 44.9 | − | PS13 |
| NGC 7172 | − | − | 3.82 | 4.50 | 26.0 | − | PS13 |
| NGC 7582 | 6.93 | 6.56 | 3.44 | 7.59 | 139 | − | PS13, A95 |
|
|
|||||||
| MilkyWay (× 10-6) | 2.70 | 1.52 | 1.68 | 1.68 | 0.98 | — | F99 |
Notes.
Reference to line fluxes: A95 = Aalto et al. (1995), F99 = Fixsen et al. (1999) – COBE measurement; I14 = Israel et al. (2014); I = Israel (JCMT, this paper); K14 = Kamenetzky et al. (2014) P10 = Panuzzo et al. (2010); P12 = Papadopoulos et al. (2012), P14 = Papadopoulos et al. (2014); PS13 = Pereira-Santaella et al. (2013); PS14 = Pereira-Santaella et al. (2014); Sc14 = Schirm et al. (2014); Sp12 = Spinoglio et al. (2012); W03 = Ward et al. (2003). For galaxies marked by an asterisk (*) we have determined J = 2−112CO and 13CO fluxes corresponding to the SPIRE aperture by map integration.
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