EDP Sciences
Free Access
Issue
A&A
Volume 554, June 2013
Article Number A83
Number of page(s) 34
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201220976
Published online 07 June 2013

Online material

Appendix A: Observation log and line flux tables

Table A.1

List of observations.

Table A.2

Central velocities, FWHM widths, and integrated line fluxes measured for the protostellar envelopes.

Table A.3

As Table A.2, for the outflows.

Table A.4

As Table A.2, for the foreground clouds.

Appendix B: Observed line profiles

thumbnail Fig. B.1

Spectra of the H2O 111 − 000 (bottom), HO 111 − 000 (second from bottom), H2O 212–101 (third from bottom) and H2O 202–111 (top) lines toward IRAS 05358. The vertical scale is Tmb in K, and the dashed line denotes the systemic velocity determined from ground-based observations. The spectra have been shifted vertically for clarity.

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thumbnail Fig. B.2

As Fig. B.1, toward IRAS 16272.

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thumbnail Fig. B.3

As Fig. B.1, toward NGC 6334I(N).

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thumbnail Fig. B.4

As Fig. B.1, toward W43 MM1.

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thumbnail Fig. B.5

As Fig. B.1, toward DR21(OH).

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thumbnail Fig. B.6

As Fig. B.1, toward W3 IRS5.

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thumbnail Fig. B.7

As Fig. B.1, toward IRAS 18089.

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thumbnail Fig. B.8

As Fig. B.1, toward W33A. The emission/absorption feature near 0 km s-1 in the 1669 GHz spectrum is the H2O 1661 GHz line from the other sideband.

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thumbnail Fig. B.9

As Fig. B.1, toward IRAS 18151.

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thumbnail Fig. B.10

As Fig. B.1, toward AFGL 2591. The emission feature near +18 km s-1 in the 1669 GHz spectrum is the H2O 1661 GHz line from the other sideband.

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thumbnail Fig. B.11

As Fig. B.1, toward G 327.

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thumbnail Fig. B.12

As Fig. B.1, toward NGC 6334I.

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thumbnail Fig. B.13

As Fig. B.1, toward G29.96.

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thumbnail Fig. B.14

As Fig. B.1, toward G31.41.

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thumbnail Fig. B.15

As Fig. B.1, toward G5.89. The emission feature near +90 km s-1 in the HO spectrum is the 13CO 10–9 line.

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thumbnail Fig. B.16

As Fig. B.1, toward G10.47.

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thumbnail Fig. B.17

As Fig. B.1, toward G34.26.

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thumbnail Fig. B.18

As Fig. B.1, toward W51e.

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thumbnail Fig. B.19

As Fig. B.1, toward NGC 7538 IRS1.

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Appendix C: Continuum models

thumbnail Fig. C.1

Continuum model for IRAS 05358. Top left: spectral energy distribution. Top right: submillimeter image with 3σ contour marked in white and useable map sectors marked in black. Bottom left: temperature and density structure as a function of radius. Bottom right: submillimeter emission profiles. The numbers in the top left panel are the modeled envelope mass, the modeled luminosity, the adopted envelope size and the adopted distance.

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thumbnail Fig. C.2

As Fig. C.1, for IRAS 16272.

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thumbnail Fig. C.3

As Fig. C.1, for NGC 6334I(N).

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thumbnail Fig. C.4

As Fig. C.1, for W43-MM1.

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thumbnail Fig. C.5

As Fig. C.1, for DR21(OH).

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thumbnail Fig. C.6

As Fig. C.1, for W3 IRS5.

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thumbnail Fig. C.7

As Fig. C.1, for IRAS 18089.

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thumbnail Fig. C.8

As Fig. C.1, for W33A.

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thumbnail Fig. C.9

As Fig. C.1, for IRAS 18151.

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thumbnail Fig. C.10

As Fig. C.1, for AFGL 2591.

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thumbnail Fig. C.11

As Fig. C.1, for G327–0.6.

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thumbnail Fig. C.12

As Fig. C.1, for NGC 6334I.

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thumbnail Fig. C.13

As Fig. C.1, for G29.96.

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thumbnail Fig. C.14

As Fig. C.1, for G31.41.

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thumbnail Fig. C.15

As Fig. C.1, for G5.89.

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thumbnail Fig. C.16

As Fig. C.1, for G10.47.

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thumbnail Fig. C.17

As Fig. C.1, for G34.26.

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thumbnail Fig. C.18

As Fig. C.1, for W51e.

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thumbnail Fig. C.19

As Fig. C.1, for NGC 7538 IRS1.

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Appendix D: Correlation analysis

thumbnail Fig. D.1

Observed line fluxes (positive: emission) or absorbances (negative: absorption) versus bolometric luminosity L of the source (top), versus envelope mass M (middle), and versus the ratio L/M (bottom). Open squares: mid-IR-quiet HMPOs; filled squares: mid-IR-bright HMPOs; triangles: hot molecular cores; circles: ultracompact Hii regions. Uncertainties in line fluxes are ≈10%, while the typical uncertainty of masses, luminosities and L/M ratios is a factor of 2.

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thumbnail Fig. D.2

As Fig. D.1, for the narrow outflow component.

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thumbnail Fig. D.3

As Fig. D.1, for the broad outflow component.

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thumbnail Fig. D.4

Line width of the narrow outflow component versus bolometric luminosity L of the source (top), versus envelope mass M (middle), and versus the ratio L/M (bottom). The error bar denotes the typical uncertainty in mass, luminosity, and L/M ratio; the uncertainty in line width is smaller than the symbol size.

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thumbnail Fig. D.5

As Fig. D.4, for the broad outflow component.

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© ESO, 2013

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