Table 2
Chemical model parameters.
| Taurus | |
| nΗ | 3.16 × 103 to 3.16 × 106 cm−3 in steps of × 3.16 |
| AV | 1.5, 3.5, 5.5, 7.5, 9.5, 11.5 mag |
| Τ | 10, 15, 20, 25, 30, 35, 45 Κ |
| CRIR(1) | (1.0, 5.0, 10, 50) × 10−17 s−1 |
| χUV (Draine) | 5.0(2) |
| [S/H] | (1.5, 0.15, 0.008) × 10−5 |
| Perseus | |
| nH | 3.16 × 103 to 3.16 × 106 cm−3 in steps of × 3.16 |
| AV | 1.5, 3.5, 5.5, 7.5, 9.5, 11.5, 13.5 mag |
| Τ | 10, 15, 20, 25, 30, 35, 45 Κ |
| CRIR(1) | (1.0, 5.0, 10, 50) × 10−17 s−1 |
| χUV (Draine) | 25.0(2) |
| [S/H] | (1.5, 0.15, 0.008) × 10−5 |
| Orion | |
| nH | 3.16 × 103 to 3.16 × 106 cm−3 in steps of × 3.16 |
| ΑV | 1.5, 3.5, 5.5, 7.5, 9.5, 11.5, 15.5, 20 mag |
| Τ | 10, 15, 20, 25, 30, 35, 45 Κ |
| CRIR(1) | (1.0, 5.0, 10, 50) × 10−17 s−1 |
| χUV (Draine) | 50(3) |
| [S/H] | (1.5, 0.15, 0.008) × 10−5 |
Notes. (1)Molecular hydrogen cosmic-ray ionization rate 
. (2)Estimated by Navarro-Almaida et al. (2020) based on the dust temperature and the analytical expression derived by Hocuk et al. (2017). (3)Assumed value based on UV field estimated toward the photon-dominated region in the Horesehead nebula (Pety et al. 2005).
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