Table 5.
Comparison of NGC 1365 and other galaxies.
| Object | Region | Density | Gas/Dust | H2O abundance | Comments |
|---|---|---|---|---|---|
| (cm−3) | temperature (K) | vs H2 (×10−8) | |||
| NGC 1365 | Absorption (a) | 102 − 104 | ≈20 (c) | 5−8 | A |
| (Barred | emission (a)(b) | 104 − 106 | 40−60/55 (c) | 6−600 (j)(k) | A |
| spiral) | Shocks (b) | 104 − 105(d) | 350/22−32 (c) | 200 (n)–10 000 (l) | B |
| Sgr A (e) | Absorption | 102 − 103(i) | 100−30 (i)/15 (m) | 3 | C |
| Emission | 104 − 105(f) | 80 (f)/20−30 (m) | 2−7 | D | |
| Line wings | 3 × (104 − 105) | 80−160/20−30 (m) | 80−570 | E | |
| NGC 6240 | Warm emission | 106 | 60−70/60−70 | 10 | F |
| (Merger (g)(h)) | Shocks | 5 × (104 − 106) (d) | 120−400/20−30 | 10 | G |
| Galaxy | Absorption | 103 − 105 | 20−200/20−30 | 0.1−10 | H, J |
| Sample (h) | Cold emission | 103 − 105 | 20−30/20−30 | 0.1−1 | H |
| Warm emission | 105 − 106 | 40−70/40−70 | 1−10 | H | |
| Hot emission | 105 − 106 | 100−200/100−200 | 100−1000 | K |
Notes.
Dust temperatures from Alonso-Herrero et al. (2012) and Tabatabaei et al. (2013).
From Odin observations of ground state o-H2O and o-H
O, assuming an ortho-to-para ratio of 3 (Karlsson et al. 2013).
From Walmsley et al. (1986).
From Herschel SPIRE oservations (Meijerink et al. 2013).
From Herschel HIFI, SPIRE and PACS observations (Liu et al. 2017).
From the Sandqvist et al. (2015)Herschel HIFI 487 GHz search for O2.
Lower abundances may be accomodated by PDR models, while the high ones indicate shocks (see Comments).
Fast shock model abundance (Flower & Pineau des Forêts 2010) in an effective accumulated 10″ size area (see Comments).
From Sandqvist et al. (2008).
From slow shock chemistry, in case FIR pumping dominates (González-Alfonso et al. 2010, 2012, 2014).
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