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Table 3
CO(1–0) and HCN(1–0) conversion factors in units of M⊙(K km s-1 pc2)-1.
| Galaxy sample | CO(1–0) | HCN(1–0) | HCN(1–0) | HCO+(1–0) |
| –H2 | –H2 | –dense gas | –dense gas | |
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| Preferred model | ||||
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| local spirals | 4.7 ± 1.8 | 62 ± 15 | 21 ± 6 | 11 ± 2 |
| ULIRGs | 1.7 ± 0.4 | 11 ± 5 | 21 ± 6 | 17 ± 5 |
| smm-galaxies | 1.4 ± 0.7 | 20 ± 10 | 33 ± 17 | 19 ± 11 |
| high-z star-forming | 2.6 ± 0.9 | 85 ± 37 | 59 ± 21 | 25 ± 7 |
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| No substructure | ||||
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| local spirals | 2.9 ± 0.9 | 52 ± 10 | – | – |
| ULIRGs | 1.3 ± 0.3 | 10 ± 5 | 8 ± 3 | 6 ± 2 |
| smm-galaxies | 0.9 ± 0.3 | 16 ± 8 | 6 ± 2 | 3 ± 1 |
| high-z star-forming | 1.6 ± 0.6 | 111 ± 75 | 11 ± 9 | 4 ± 3 |
Notes. For dense gas αHCN = 10M⊙(K km s-1 pc2)-1 (e.g., Gao & Solomon 2004).
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