Table 3
Initial elemental abundances considered for the H II-PDR, diffuse clud, dark cloud, and hot core cloud models with respect to total hydrogen nuclei.
| PDRa | Diffuse cloudb | Dark cloudc | Hot cored | ||||
|---|---|---|---|---|---|---|---|
| Species | Abundances | Species | Abundances | Species | Abundances | Species | Abundances |
| H2 | 5.0 × 10−1 | H2 | 4.99 × 10−1 | ||||
| H | 1.0 × 100 | H | 1.0 × 100 | H | 5.0 × 10−5 | H | 2.0 × 10−3 |
| He | 9.5 × 10−2 | He | 8.5 × 10−2 | He | 9.0 × 10−2 | He | 9.0 × 10−2 |
| C | 3.0 × 10−4 | C+ | 2.7 × 10−4 | C+ | 1.4 × 10−4 | C+ | 1.4 × 10−4 |
| N | 7.0 × 10−5 | N | 6.8 × 10−5 | N | 7.5 × 10−5 | N | 7.5 × 10−5 |
| O | 4.0 × 10−4 | O | 4.9 × 10−4 | O | 3.2 × 10−4 | O | 3.2 × 10−4 |
| F | 3.6 × 10−8 | F | 2.0 × 10−8 | F | 2.0 × 10−8 | ||
| Na | 3.0 × 10−7 | Na+ | 1.7 × 10−6 | Na+ | 2.0 × 10−9 | Na+ | 2.0 × 10−8 |
| Mg | 3.0 × 10−6 | Mg+ | 3.9 × 10−5 | Mg+ | 7.0 × 10−9 | Mg+ | 7.0 × 10−9 |
| Al | 2.0 × 10−7 | Al+ | 2.3 × 10−6 | Al+ | 2.7 × 10−10 | Al+ | 2.7 × 10−10 |
| Si | 4.0 × 10−6 | Si+ | 3.2 × 10−5 | Si+ | 8.0 × 10−9 | Si+ | 8.0 × 10−9 |
| P+ | 2.6 × 10−7 | P+ | 3.0 × 10−9 | P+ | 3.0 × 10−9 | ||
| S | 1.0 × 10−5 | S+ | 1.3 × 10−5 | S+ | 1.5 × 10−6 | S+ | 8.0 × 10−8 |
| Cl | 1.0 × 10−7 | Cl+ | 3.2 × 10−7 | Cl+ | 4.0 × 10−9 | Cl+ | 4.0 × 10−9 |
| K | 1.1 × 10−8 | K+ | 1.2 × 10−7 | K+ | 1.2 × 10−10 | K+ | 1.2 × 10−10 |
| Fe | 3.0 × 10−6 | Fe+ | 3.2 × 10−5 | Fe+ | 3.0 × 10−9 | Fe+ | 3.0 × 10−9 |
Notes. a Initial abundances are considered from Shaw et al. (2022), except Na, K, and Al. b Initial abundances are considered from Chantzos et al. (2020), except for Al and K, which are set to standard solar abundances from Asplund et al. (2009). Additionally, F is considered neutral. c Initial abundances are considered from Millar et al. (2024) except for Al and K. d Initial abundances are considered from Garrod et al. (2017) except for Al, K, and F.
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