Table 4
o-H2D+(11, 0−11, 1) spectral line parameters.
| Source | vLSR | ΔvLSR | TMB | ∫ TMBdv | τ(a) | Tex (b) |
|---|---|---|---|---|---|---|
| [km s−1] | [km s−1] | [K] | [K km s−1] | [K] | ||
| IRAS 05399-0121 | … | … | <0.09(c) | <0.07(d) | <0.02 | 13.5 ± 1.6 |
| SMM 1 | 9.20 ± 0.02 | 0.70 ± 0.04 | 0.34 ± 0.05 | 0.25 ± 0.03 | 0.07 ± 0.01 | 11.9 ± 0.9 |
| SMM 3 | 8.47 ± 0.02 | 0.74 ± 0.03 | 0.40 ± 0.05 | 0.32 ± 0.03 | 0.09 ± 0.01 | 11.3 ± 0.8 |
| IRAS 05405-0117 | … | … | <0.09(c) | <0.07(d) | <0.02 | 11.3 ± 0.6 |
| SMM 6 | 9.38 ± 0.01 | 0.48 ± 0.01 | 0.74 ± 0.08 | 0.38 ± 0.04 | 0.19 ± 0.02 | 11.0 ± 0.4 |
| SMM 7 | 3.56 ± 0.02 | 0.60 ± 0.04 | 0.28 ± 0.04 | 0.18 ± 0.02 | 0.09 ± 0.03 | 9.4 ± 1.1 |
Notes. Columns (2–5) give the local standard of rest (LSR) radial velocity (vLSR), full width at half maximum (FWHM; Δv), peak intensity (TMB), and the integrated intensity of the line (∫ TMBdv). (a) Peak optical thickness calculated using Tex from the last column. (b)The value of Tex was assumed to be equal to Tkin(NH3) (Miettinen et al. 2010).(c)A 3σ upper limit is placed for the non-detections. (d)The integrated intensity upper limit for these protostellar cores was estimated as the intensity upper limit (< 0.09 K) times the detected linewidth in the Class 0 object SMM 3 (0.74 km s−1).
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