Table A.2
Central velocities, FWHM widths, and integrated line fluxes measured for the protostellar envelopes.
| Source | V LSR | ΔV | 1113 GHz | H O |
1669 GHz | 987 GHz |
|
|
||||||
| IRAS 05358 | −17.9(6) | 3.8(14) | −13.4 | −0.49 | >17.4 | −1.39 |
| IRAS 16272 | −45.9(7) | 4.7(20) | −7.51 | −0.26 | >13.5 | +6.83 |
| NGC 6334I(N) | −2.4(5) | 3.9(4) | −2.96 | −0.70 | >12.3 | −11.8 |
| W43 MM1 | +100.5(7) | 6.0(15) | −12.9 | −2.07 | −10.1 | −2.17 |
| DR21(OH) | −3.3(4) | 3.4(13) | >12.0 | −0.68 | >9.9 | −0.69 |
| W3 IRS5 | −37.7(12) | 3.2(6) | −3.06 | +1.84 | −2.00 | +21.9 |
| IRAS 18089 | +33.7(11) | 3.1(11) | −3.47 | −0.45 | −8.44 | +0.90 |
| W33A | +35.1(12) | 5.6(13) | −4.34 | −0.61 | >21.0 | <0.60 |
| a | +39.3(6) | 4.8(14) | −2.85 | +1.09 | −5.66 | +9.46 |
| IRAS 18151 | +33.1(2) | 1.8(10) | −0.52 | <0.07 | >5.63 | +1.35 |
| AFGL 2591 | −3.6(14) | 4.0(10) | +24.0 | +0.92 | +8.67 | +11.8 |
| G327-0.6 | −42.5(5) | 3.3(9) | −1.96 | −0.62 | >15.3 | −1.43 |
| NGC 6334I | −5.7(16) | 5.7(7) | −5.31 | −0.79 | −5.46 | +15.3 |
| G29.96 | +98.2(6) | 4.3(13) | −0.97 | +1.10 | >13.8 | +19.2 |
| G31.41 | +99.1(4) | 5.2(14) | >16.7 | −1.68 | >23.2 | −1.67 |
| G5.89 | +12.0(4) | 7.2(20) | −5.71 | +4.85 | >22.8 | +70.0 |
| G10.47 | +70.0(10) | 3.9(4) | −1.88 | −0.68 | −5.82 | +4.17 |
| a | +65.5(9) | 4.3(13) | −1.63 | +0.50 | −6.43 | +18.3 |
| G34.26 | +61.5(8) | 4.9(11) | −22.1 | −0.63 | −8.40 | −1.35 |
| a | +57.1(4) | 5.0(6) | −5.81 | +2.99 | −7.85 | +27.4 |
| W51e | +55.7(17) | 6.3(12) | −12.5 | −0.81 | −10.2 | +43.8 |
| NGC 7538 | −57.0(3) | 3.6(10) | −4.10 | +0.34 | −8.02 | +18.7 |
Notes.Positive fluxes denote integrated intensities (∫TmbdV in K km s-1) of emission features, where upper limits denote non-detections. Negative fluxes denote integrated optical depths (∫τdV in km s-1) of absorption features, where lower limits denote saturated absorptions. Central velocities and FWHM line widths are in units of km s-1, and numbers in parentheses are 1σ errors in units of the last decimal. Line fluxes have uncertainties of ≈10%.
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