Table 1.
SN feedback efficiency required to sustain turbulence in the neutral gas of our sample of galaxies.
| Galaxy | SN efficiency |
||
|---|---|---|---|
| ηatom, c | ηatom, w | ηmol | |
| (1) | (2) | (3) | |
| DDO 154 | 0.049 |
0.009 |
– |
| – | – | – | |
| IC 2574 | 0.077 |
0.023 |
– |
 |
 |
– | |
| NGC 0925 | 0.029 |
0.014 |
0.0004 |
 |
 |
 |
|
| NGC 2403 | 0.037 |
0.015 |
0.004 |
 |
 |
 |
|
| NGC 2976 | 0.020 |
0.009 |
0.0013 |
 |
 |
 |
|
| NGC 3198 | 0.066 |
0.029 |
0.016 |
 |
 |
 |
|
| NGC 4736 | 0.037 |
0.020 |
0.006 |
 |
 |
 |
|
| NGC 5055 | 0.033 |
0.020 |
0.010 |
 |
 |
 |
|
| NGC 6946 | 0.010 |
0.006 |
0.003 |
 |
 |
 |
|
| NGC 7793 | 0.031 |
0.014 |
– |
 |
 |
– | |
| All | 0.035 |
0.015 |
0.0042 |
 |
 |
 |
|
Notes. The values in the white rows are obtained with the SFR surface density from Leroy et al. (2008) and Bigiel et al. (2010), while those in the shaded rows are derived with the profiles from Muñoz-Mateos et al. (2009), whose sample does not include DDO 154 (indicated with “–”). The last two rows show the median values obtain from the posteriors of all the galaxies in the sample. The three columns report the best values in different cases: (1) all atomic gas is CNM; (2) all atomic gas is WNM; (3) molecular gas (the “–” indicates that no molecular gas emission is detected).
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