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Table A.2
Mid-IR lines detected with Spitzer/IRS towards the Class 0 protostar Serpens SMM1 and line fluxes (uncorrected for extinction) within a 7′′ × 7′′ aperture.
| Species | Transition | E up | λ | Line flux |
| (K) | (μm) | (W m-2) | ||
|
|
||||
| Fe+ |  – |
961 | 35.349 | 2.45E-17 |
| Si+ |  – |
414 | 34.815 | 6.29E-17 |
| p-H2 | 0–0 S(0) J = 2–0 | 509 | 28.219 | <5.92E-18 |
| Fe+ | – |
554 | 25.988 | 8.12E-17 |
| S |  – |
570 | 25.249 | 3.24E-17 |
| Fe+ |  – |
4087 | 24.519 | 4.46E-17 |
|
|
||||
| Fe+ | – |
3499 | 17.936 | 1.36E-17 |
| o-H2 | 0–0 S(1) J = 3–1 | 1015 | 17.035 | 5.96E-19 |
| Ne+ | – |
1124 | 12.814 | 7.06E-18 |
| p-H2 | 0–0 S(2) J = 4–2 | 1682 | 12.279 | 2.42E-18 |
Notes. The horizontal line shows the transition between the LH and SH modules. Intensity errors up to ~25%.
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