Table A.6
Beam averaged column densities and abundances for S-bearing molecules from different substructures in NGC 7538S and IRS1 denoted in Fig. 3.
| Species | MM1 | MM2 | MM3 | JetN | JetS | IRS1−mmS | IRS1−peak |
| (172 ± 23 K) | (137 ± 14 K) | (50 K) | (150 K) | (150 K) | (162 ± 14 K) | (214 ± 66 K) | |
| I. Column densities (in the form of x ± y(z) = (x ± y) × 10zcm-2) | |||||||
| OCS † | 5.86± 0.26(16) | 4.41± 0.10(16) | 6.42± 0.20(16) | ≤ 1.10(16) | ≤ 6.57(15) | 8.71± 0.14(16) | ≤ 2.87(15) |
| O13CS | 7.63± 0.15(14) | 6.05± 1.92(14) | 9.27± 0.13(14) | ≤ 6.88(13) | ≤ 9.11(13) | 1.01± 0.50(15) | ≤ 4.15(15) |
| SO2 | 1.93± 0.20(17) | ≤ 1.57(15) | ≤ 2.65(16) | ≤ 1.13(15) | ≤ 1.89(15) | 6.12± 1.56(16) | 9.71± 4.18(16) |
| 34SO2 | 1.38± 0.20(16) | ≤ 7.17(13) | ≤ 1.95(13) | ≤ 5.41(13) | ≤ 1.50(14) | 1.62± 0.13(15) | 1.17± 1.20(15) |
| SO † | 3.16± 0.31(17) | 2.45± 0.12(16) | − | ≤ 1.56(16) | ≤ 2.44(16) | 6.91± 0.47(16) | 1.52± 1.10(16) |
| 33SO | 2.81± 0.30(15) | 2.59± 0.46(14) | ≤ 1.52(13) | ≤ 2.45(13) | ≤ 5.96(13) | 5.22± 1.43(14) | ≤ 9.85(14) |
| II. Abundances (in the form of x ± y(z) = (x ± y) × 10z) | |||||||
| OCS † | 3.47± 0.79(−8) | 2.58± 0.43(−8) | 1.22± 0.09(−8) | ≤ 4.33(−8) | ≤ 1.97(−8) | − | ≤ 6.52(−10) |
| O13CS | 4.52± 0.90(−10) | 3.55± 1.79(−10) | 1.77± 0.10(−10) | ≤ 2.71(−10) | ≤ 2.74(−10) | − | ≤ 9.42(−10) |
| SO2 | 1.14± 0.34(−7) | ≤ 9.21(−10) | ≤ 5.05(−9) | ≤ 4.47(−9) | ≤ 5.67(−9) | − | 2.20± 0.95(−8) |
| 34SO2 | 8.19± 2.80(−9) | ≤ 4.21(−11) | ≤ 3.71(−12) | ≤ 2.13(−10) | ≤ 4.51(−10) | − | 2.67± 2.71(−10) |
| SO† | 2.11± 0.64(−7) | 1.93± 0.66(−8) | − | ≤ 1.23(−8) | ≤ 2.27(−8) | − | 3.45± 2.49(−9) |
| 33SO | 1.66± 0.50(−9) | 1.52± 0.52(−10) | ≤ 2.90(−12) | ≤ 9.66(−11) | ≤ 1.79(−10) | − | ≤ 2.23(−10) |
Notes. 1). Abundances with respect to H2 were computed using NH2 derived from dust continuum for MM1–MM3, and from C18O for the other substructures (assuming x(C18O) ≈ 1.64 × 10-7; see Table 1). 2). All species are assumed to have the same temperature as CH3CN in MM1, MM2, and IRS1-mmS. 3). Values of all species in MM3, the outflow regions (JetN and JetS), and IRS1-peak are derived under assumed temperatures (Sect. 5.1). 4). Molecular column densities are obtained from the strongest transition of each isotopologue by assuming LTE with the excitation temperatures listed in the table head. 5). Uncertainties for the values derived from one transition (written in subscript) are determined from Trot, partition function Q(Trot), and fit to 
(or ∫τ(υ)dυ in IRS1-peak). 6). For species which are not detected, an upper limit derived from 3σ rms is given. 7). “−” indicates that the line area could not be computed because it has obvious absorption in IRS1-mmS, or obvious emission in IRS1-peak, or non-detection of both main and rare isotopologues. 8).
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