ATLASGAL-selected massive clumps in the inner Galaxy - I. CO depletion and isotopic ratios

Free Access

Issue		A&A Volume 570, October 2014


Article Number		A65
Number of page(s)		55
Section		Stellar structure and evolution
DOI		https://doi.org/10.1051/0004-6361/201423692
Published online		17 October 2014

Online material

Appendix A: Tables

Table A.1

Distances and classification for sources in subsample S1, derived from C¹⁷O(3−2).

Table A.2

Distances and classification for the sources in subsample S2, derived from C¹⁷O(3−2).

Table A.3

Distances and classification for the sources in subsample S3 derived from C¹⁷O(3−2).

Table A.4

Line parameters for subsample S1.

Table A.5

Line parameters of C¹⁸O(1−0) for subsample S1.

Table A.6

Line parameters of ¹³CO(1−0) for subsample S1.

Table A.7

Line parameters of ¹³C¹⁸O(1−0) for subsample S1.

Table A.8

Line parameters for subsample S2.

Table A.9

Line parameters of C¹⁷O(3−2) for subsample S3.

Table A.10

Excitation temperature for subsample S1.

Table A.11

Excitation temperature for subsample S2.

Table A.12

Optical depths and isotopic ratios for subsample S1.

Table A.13

Molecular column densities for subsample S1.

Table A.14

Molecular column densities for subsample S2.

Table A.15

Molecular column densities for subsample S3.

Table A.16

Masses from 870 μm dust emission and virial masses for subsample S1.

Table A.17

Masses from 870 μm dust emission and virial masses for subsample S2.

Table A.18

Masses from 870 μm dust emission and virial masses for subsample S3.

Appendix B: Spectra

	Fig. B.1 ¹³C¹⁸O(1 − 0) (x10, green), C¹⁷O(1 − 0) (x3, red) and C¹⁸O(1 − 0) (black). The spectra are displaced for clarity.
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	Fig. B.1 continued.
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	Fig. B.2 C¹⁸O(2 − 1) (red) and ¹³CO(2 − 1) (black). The spectra are displaced for clarity.
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	Fig. B.2 continued.
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	Fig. B.2 continued.
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	Fig. B.3 C¹⁷O(3 − 2) for subsample S1. The fit is shown in green.
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	Fig. B.3 continued.
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	Fig. B.4 C¹⁷O(3 − 2) for subsample S2. The fit is shown in green.
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	Fig. B.4 continued.
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	Fig. B.4 continued.
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	Fig. B.5 C¹⁷O(3 − 2) for subsample S3. The fit is shown in green.
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	Fig. B.5 continued.
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Appendix C: RATRAN figures

Fig. C.1

RATRAN results for individual sources, using models with a constant abundance profile. The panels show: (top left) marginal probability distribution of the temperature/luminosity, depending on the group of the source, (top right) marginal probability distribution of the mass, (bottom left) joint probability distribution of mass and T or L (depending on whether model is centrally heated or isothermal), (bottom right) marginal probability distribution of the depletion factor.

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	Fig. C.1 continued.
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	Fig. C.1 continued.
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	Fig. C.1 continued.
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	Fig. C.1 continued.
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	Fig. C.2 RATRAN results for individual sources, using models with a drop profile. The panels show: (left) joint probability distribution of mass and critical density of molecular hydrogen above which all CO is locked onto dust grains, (centre) marginal probability distribution of critical density, (right) marginal probability distribution of mass.
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	Fig. C.2 continued.
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© ESO, 2014

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