Table 5
H2S/OCS ratio for the studied sources, including their evolutionary class, binarity, environment, and the derived column densities of H2S and OCS for the stated excitation temperatures.
| Source | Class | Binarity | Environment | Tex (K) | N(H2S) (cm−2) | N(OCS) (cm−2) | N(H2S)/N(OCS) |
|---|---|---|---|---|---|---|---|
| IRAS 16293-2422 A | 0 | CB | Clustered | 125±20 | (2.4±0.4)×1017 | (3.6±1.4)×1017 | 0.7±0.3 |
| IRAS 16293-2422 B | 0 | WB | Clustered | 125±20 | (9.2±1.7)×1016 | (7.0±0.8)×1016 | 1.3±0.3 |
| NGC 1333-IRAS4A | 0 | CB | Clustered | 150–300 | (3.4±0.8)×1016 | (1.8±0.2)×1016 | 1.9±0.5 |
| RCrA IRS7B | 0/I | WB | Clustered | 100±20 | (5.6±0.8)×1013 | ≤3.6×1013 | ≥1.5 |
| Per-B1-c | 0 | S | Clustered | 60 | >9.7×1015 | >5.0×1015 | (1.9) |
| 200 | >1.2×1016 | >3.6×1015 | (3.3) | ||||
| BHR71-IRS1 | 0 | WB | Isolated | 100 | >2.4×1016 | >2.7×1015 | (8.9) |
| 250 | >3.3×1016 | (3.4±0.3)×1015 | ≥9.7 | ||||
| Per-emb-25 | 0/I | S | Clustered | 50–300 | ≤8.3×1013 | ≤3.2×1014 | – |
| NGC 1333-IRAS4B | 0 | WB | Clustered | 100±20 | >5.8×1015 | (2.8±0.6)×1016 | ≥0.21 |
| Ser-SMM3 | 0 | S | Clustered | 100–250 | (5.8±3.2)×1014 | (8.7±4.9)×1014 | 0.7±0.5 |
| TMC1 | I | CB | Clustered | 40 | ≤1.5×1013 | ≤2.6×1013 | – |
| Comet (67P/C-G) |  (a) |
||||||
| N(H2S)/N(H2O) | N(OCS)/N(H2O) | N(H2S)/N(OCS) | |||||
| ISM ices (W33A) | <3.0×10−2, (b) | 4.0×10−4, (c) | <75 | ||||
| ISM ices (Mon R2 IRS2) | <4.7×10−3,(d) | 5.5×10−4,(c) | <8.5 | ||||
Notes. The H2S/OCS ratios for the cold and warm components of B1-c, and the cold component of BHR71-IRS1 are the best-available estimates pending opacity issues. CB: close binary (<500 au) that is not spatially resolved in the data used for this work; WB: wide binary (500–5000 au) that is spatially resolved in the data used for this work; S: single source within 5 000 au. ISM stands for interstellarmedium.
References. (a)Rubin et al. (2019), (b)van der Tak et al. (2003), (c)Palumbo et al. (1995),(d)Smith (1991).
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