Table 4
Mean column densities obtained in this work for Taurus, Perseus, and Orion and column densities observed in a sample of nearby galaxies.
| Molecule | Taurus | Perseus | Orion | M 83 | NGC 253 | M 82 | M 51 | NGC 1068 | NGC 7469 | Arp 220 | Mrk 231 |
|---|---|---|---|---|---|---|---|---|---|---|---|
| SFR (M⊙ yr−1) | 715 ⋅ 10−6 | 150 ⋅ 10−6 | 715 ⋅ 10−6 | 2.5 | 3.6 | 10 | 2.5 | 0.4 | 30 | 240 | 220 |
| 13CO | 1.1 ⋅ 1016 | 3.8 ⋅ 1016 | 7.5 ⋅ 1016 | 5.7 ⋅ 1016 | 1.9 ⋅ 1017 | 1.3 ⋅ 1017 | 2.1 ⋅ 1016 | 4.6 ⋅ 1017 | 3.6 ⋅ 1016 | 6.6 ⋅ 1017 | 5.6 ⋅ 1016 |
| C18O | 1.4 ⋅ 1015 | 3.0 ⋅ 1015 | 4.6 ⋅ 1015 | 1.1 ⋅ 1016 | 5.1 ⋅ 1016 | 2.6 ⋅ 1016 | 5.2 ⋅ 1015 | 1.3 ⋅ 1017 | 6.4 ⋅ 1015 | 6.2 ⋅ 1017 | 4.9 ⋅ 1016 |
| HCO+ | 3.1 ⋅ 1012 | 6.3 ⋅ 1012 | 2.6 ⋅ 1013 | 4.6 ⋅ 1013 | 1.9 ⋅ 1014 | 2.6 ⋅ 1014 | 1.3 ⋅ 1013 | 5.5 ⋅ 1014 | 7.4 ⋅ 1013 | 1.1 ⋅ 1015 | 3.3 ⋅ 1014 |
| H13CO+ | 1.7 ⋅ 1012 | 1.5 ⋅ 1012 | 1.6 ⋅ 1012 | 1.1 ⋅ 1013 | 1.3 ⋅ 1013 | 6.9 ⋅ 1012 | ≤6.6 ⋅ 1011 | 2.0 ⋅ 1013 | ≤8.0 ⋅ 1012 | 9.8 ⋅ 1013 | ≤9.1 ⋅ 1013 |
| HC18O+ | 1.4 ⋅ 1011 | 1.3 ⋅ 1011 | 1.4 ⋅ 1011 | 0 | 4.3 ⋅ 1012 | 4.70 ⋅ 1012 | 0 | 0 | 0 | 0 | 0 |
| HCN | 4.8 ⋅ 1013 | 5.5 ⋅ 1013 | 2.2 ⋅ 1014 | 8.6 ⋅ 1013 | 3.8 ⋅ 1014 | 2.9 ⋅ 1014 | 4.5 ⋅ 1013 | 2.4 ⋅ 1015 | 1.0 ⋅ 1014 | 4.6 ⋅ 1015 | 8.5 ⋅ 1014 |
| H13CN | 4.7 ⋅ 1012 | 4.5 ⋅ 1012 | 4.9 ⋅ 1012 | 2.3 ⋅ 1012 | 2.8 ⋅ 1013 | 5.0 ⋅ 1012 | 1.8 ⋅ 1012 | 8.1 ⋅ 1013 | ≤1.4 ⋅ 1013 | 7.1 ⋅ 1014 | 2.0 ⋅ 1014 |
| HNC | 1.3 ⋅ 1013 | 1.8 ⋅ 1013 | 5.7 ⋅ 1013 | 3.1 ⋅ 1013 | 1.8 ⋅ 1014 | 1.2 ⋅ 1014 | 1.4 ⋅ 1013 | 7.0 ⋅ 1014 | 4.2 ⋅ 1013 | 3.2 ⋅ 1015 | 2.5 ⋅ 1014 |
| HCS+ | 4.5 ⋅ 1011 | 4.3 ⋅ 1011 | 3.5 ⋅ 1011 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 |
| CS | 6.1 ⋅ 1013 | 5.6 ⋅ 1013 | 5.5 ⋅ 1013 | 5.7 ⋅ 1013 | 4.1 ⋅ 1014 | 2.5 ⋅ 1014 | 1.8 ⋅ 1013 | 7.6 ⋅ 1014 | 8.1 ⋅ 1013 | 3.4 ⋅ 1015 | 3.5 ⋅ 1014 |
| SO | 2.0 ⋅ 1013 | 3.8 ⋅ 1013 | 2.1 ⋅ 1013 | 2.0 ⋅ 1013 | 1.7 ⋅ 1014 | 7.7 ⋅ 1013 | 1.1 ⋅ 1013 | 2.2 ⋅ 1014 | ≤6.9 ⋅ 1013 | ≤4.4 ⋅ 1014 | ≤5.0 ⋅ 1014 |
| 34SO | 1.8 ⋅ 1012 | 3.3 ⋅ 1012 | 7.6 ⋅ 1011 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 |
| H2S | 2.4 ⋅ 1013 | 5.0 ⋅ 1013 | 7.2 ⋅ 1013 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 |
| OCS | 5.2 ⋅ 1012 | 1.1 ⋅ 1013 | 0 | ≤7.3 ⋅ 1013 | 4.9 ⋅ 1014 | ≤8.4 ⋅ 1013 | ≤7.4 ⋅ 1013 | ≤8.9 ⋅ 1014 | ≤8.2 ⋅ 1014 | ≤6.1 ⋅ 1015 | ≤9.2 ⋅ 1015 |
| 13CO/C18O(1) | 10.9 | 17.3 | 23.7 | 5.2 | 3.7 | 5 | 4 | 3.5 | 5.6 | 1 | 1.1 |
| HCO+/H13CO+ (1) | 1.8 | 4.3 | 16 | 4.1 | 14.9 | 37 | >20 | 27 | >9 | 11 | >3.6 |
| HCN/H13CN(1) | 10.3 | 12.4 | 45.5 | 37.4 | 13.8 | 58 | 25 | 30.3 | 7.4 | 6.5 | 4.3 |
| CS/SO | 5.4 | 4.1 | 3.2 | 2.8 | 2.4 | 3.2 | 1.6 | 3.4 | 1.2 | >7 | >0.7 |
| H13CO+/13CO | 1.5 ⋅ 10−4 | 3.7 ⋅ 10−5 | 8.6 ⋅ 10−6 | 1.9 ⋅ 10−4 | 6.9 ⋅ 10−5 | 5.3 ⋅ 10−5 | <3 ⋅ 10−5 | 4.3 ⋅ 10−5 | <0.00022 | 1.40 ⋅ 10−4 | <1.6 ⋅ 10−3 |
| HC18O+/C18O | 9.8 ⋅ 10−5 | 3.6 ⋅ 10−5 | 1.9 ⋅ 10−5 | 8.4 ⋅ 10−5 | 1.3 ⋅ 10−4 | ||||||
| HCO+/HCN | 0.14 | 0.19 | 0.24 | 0.53 | 0.50 | 0.88 | 0.29 | 0.37 | 0.71 | 0.24 | 0.39 |
| H13CO+/H13CN | 0.69 | 0.68 | 0.83 | 0.46 | 1.38 | 0.25 | 0.14 | <0.45 | |||
| X(H13CO+) | 1.3 ⋅ 10−10 | 6.4 ⋅ 10−11 | 2.9 ⋅ 10−11 | 1.6 ⋅ 10−10 | 4.8 ⋅ 10−11 | 4.2 ⋅ 10−11 | <2 ⋅ 10−11 | 2.5 ⋅ 10−11 | <2 ⋅ 10−10 | 2.5 ⋅ 10−11 | <3 ⋅ 10−10 |
| X(H13CN) | 2.9 ⋅ 10−10 | 1.9 ⋅ 10−10 | 7.7 ⋅ 10−11 | 3.4 ⋅ 10−11 | 8.8 ⋅ 10−11 | 3.0 ⋅ 10−11 | 5.5 ⋅ 10−12 | 1.0 ⋅ 10−10 | <3.5 ⋅ 10−10 | 8.2 ⋅ 10−10 | 6.5 ⋅ 10−10 |
| X(CS) | 6.3 ⋅ 10−9 | 3.9 ⋅ 10−9 | 2.2 ⋅ 10−9 | 8.3 ⋅ 10−9 | 1.3 ⋅ 10−9 | 1.5 ⋅ 10−9 | 5.5 ⋅ 10−11 | 9.0 ⋅ 10−10 | 2.0 ⋅ 10−9 | 8.7 ⋅ 10−10 | 1.1 ⋅ 10−9 |
| X(SO) | 1.8 ⋅ 10−9 | 2.0 ⋅ 10−9 | 7.3 ⋅ 10−10 | 2.9 ⋅ 10−10 | 5.3 ⋅ 10−10 | 4.7 ⋅ 10−10 | |||||
| X(34SO) | 1.3 ⋅ 10−10 | 1.4 ⋅ 10−10 | 1.5 ⋅ 10−11 |
Notes. The galaxy sample data are obtained from Aladro et al. (2015) (upper limits are shown for undetected species), with the exception of the HCO+ and H13CO+ column densities in NGC 1068, obtained from Usero et al. (2004). Star formation rates of the comparison galaxies are obtained from Walter et al. (2008) for M 83; Strickland et al. (2004) for NGC 253 and M 82; Schuster et al. (2007) for M 51; Esquej et al. (2014) for NGC 1068; Genzel et al. (1995) for NGC 7469; Anantharamaiah et al. (2000) for Arp 220; Taylor et al. (1999) for Mrk 231. This parameter is only meant to give a rough idea of the activity, as it was calculated for different volumes in each galaxy. Star formation rate in galactic molecular clouds are taken from Lada et al. (2010). (1) We would like to reiterate that the low values of the HCO+/H13CO+ in Taurus and Perseus are mainly due to the proliferation of self-absorbed profiles in the HCO+ 1–0 spectra in the observed positions. These values need to be understood as lower limits to the real column density ratios. To a lesser extent, this effect is also affecting the HCN/H13CN and 13CO/C18O ratios.
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