Online material
Appendix A: Complementary figures and tables
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).
continued.
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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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Fig. A.2
Grid of OH LVG models for different gas temperatures and densities. Contour
levels of the OH |
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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.
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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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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