EDP Sciences
Free Access
Issue
A&A
Volume 548, December 2012
Article Number A77
Number of page(s) 17
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201219912
Published online 26 November 2012

Online material

Appendix A: Complementary figures and tables

Table A.1

List of detected lines towards Serpens SMM1 and line fluxes from SPIRE and PACS central spaxels (corrected for extended emission in the case of PACS).

Table A.1

continued.

thumbnail Fig. A.1

Grid of H2O LVG models for different gas temperatures and densities. Bottom: contour levels of the p-H2O 606–515/515–404 (83.284/95.627 μm) line ratio for N(p-H2O) = 1016 cm-2. Note the gas temperature dependence of this ratio. The black continuous curve shows the observed intensity line ratio of 0.33. Top: contour levels of the o-H2O 330–303/615–305 (67.269/82.031 μm) ratio for N(o-H2O) = 3  ×  1016 cm-2. Note the gas density dependence of this ratio. The black continuous curve shows the observed intensity line ratio of 0.14 while the black dotted curve shows the observed p-H2O 606–515/515–404 ratio. The intersection of both curves is marked with a star (see text).

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thumbnail Fig. A.2

Grid of OH LVG models for different gas temperatures and densities. Contour levels of the OH J = 9/2+–7/2/J = 3/2–5/2+ (65.279/96.363 μm) line ratio for N(OH) = 1016 cm-2. Note the gas temperature dependence of this ratio. The black continuous curves enclose the observed intensity line ratio with a  ~15% of relative flux calibration error.

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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.

thumbnail Fig. A.3

Best model discussed in the text (green curves) and a model where Tk is decreased by 30% in all components (blue curves).

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thumbnail Fig. A.4

Best model discussed in the text (green curves) and a model where n(H2) is decreased by a factor 3 in all components (blue curves).

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© ESO, 2012

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