Issue |
A&A
Volume 574, February 2015
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|
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Article Number | A127 | |
Number of page(s) | 33 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/201322805 | |
Published online | 05 February 2015 |
Online material
Appendix A: Atomic species
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Fig. A.1
Fine-structure emission grids with and without Γmech (Z = Z⊙). Top: emission grids. Bottom: relative changes in the emissions as a function of α. The dashed contour traces the R = 1 line, where the emissions with and without extra heating are the same. (See caption of Fig. 4.) |
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Fig. A.2
Line ratios for the reference models as a function of Γmech for the atomic fine structure lines, Z = 0.1, 0.5, and 2 Z⊙ in the left, middle and right panels respectively. |
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Fig. A.3
Atomic line ratio grids as a function of Γmech for AV = 10 mag (Z = Z⊙). |
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Appendix B: Molecular species
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Fig. B.1
Top: emission grids of PDR models without mechanical heating for a selection of CO transitions for AV = 10 mag (Z = Z⊙). Bottom: relative changes in the emission as a function of α. The dashed contour traces the R = 1 line, where the emission with and without extra heating are the same. (See caption of Fig. 4.) |
Open with DEXTER |
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Fig. B.2
Top: emission grids of PDR models without mechanical heating for a selection of 13CO transitions for AV = 10 mag (Z = Z⊙). Bottom: relative changes in the emission as a function of α. The dashed contour traces the R = 1 line, where the emission with and without extra heating are the same. (See caption of Fig. 4.) |
Open with DEXTER |
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Fig. B.3
Top: emission grids of PDR models without mechanical heating for a selection of HCN and HNC transitions for AV = 10 mag (Z = Z⊙). Bottom: relative changes in the emission as a function of α. The dashed contour traces the R = 1 line, where the emission with and without extra heating are the same. (See caption of Fig. 4.) |
Open with DEXTER |
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Fig. B.4
Various line ratios of HNC and HCN for the reference models (see Table 2) as a function of Γmech for Z = 0.1 Z⊙ (left), 0.5 Z⊙ (middle) and 2.0 Z⊙ (right.) |
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Fig. B.5
Top: emission grids of PDR models without mechanical heating for a selection of HCO+ transitions for AV = 10 mag (Z = Z⊙). Bottom: relative changes in the emission as a function of α. The dashed contour traces the R = 1 line, where the emission with and without extra heating are the same. (See caption of Fig. 4.) |
Open with DEXTER |
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Fig. B.6
Top: emission grids of PDR models without mechanical heating for a selection of CN and CS transitions for AV = 10 mag (Z = Z⊙). Bottom: relative changes in the emission as a function of α. The dashed contour traces the R = 1 line, where the emission with and without extra heating are the same. (See caption of Fig. 4.) |
Open with DEXTER |
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Fig. B.7
Various line ratios of HCO+, CS and CN for the reference models (see Table 2) as a function of Γmech for Z = 0.1 Z⊙ (left), 0.5 Z⊙ (middle) and 2.0 Z⊙ (right.) |
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Fig. B.8
Various line ratios (at AV = 10 mag) of HCN, HNC, HCO+, CN, and CS which show a strong dependence on Γmech for the reference models (see Table 2) for different metallicities, Z = 0.1 Z⊙ (left), 0.5 Z⊙ (middle) and 2.0 Z⊙ (right.) |
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Appendix C: Several model grids
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Fig. C.1
Grids of CO and 13CO line ratios for different values of α for AV = 10 mag. |
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Fig. C.2
Grids of various combination of molecular line ratios for different values of α and AV = 10 mag. |
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Fig. C.3
Grids of HCN and HNC line ratios for different values of α and AV. |
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Fig. C.4
Grids of HNC and HCO+ line ratios for different values of α and AV. |
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Fig. C.5
Grids of HCN and HCO+ line ratios for different values of α and AV. |
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Fig. C.6
Grids of HCN, HNC and HCO+ line ratios (J = 1–0 and 8–7) for different cosmic ray ionization rates with AV = 10 mag. |
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Fig. C.7
Constraining the Γmech, AV, n and G0 for starburst galaxies. Illustration for Av = 10 mag. See caption of Fig. 16 for details. |
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Fig. C.8
Constraining the Γmech, AV, n and G0 for starburst galaxies. Illustration for Av = 30 mag. See caption of Fig. 16 for details. |
Open with DEXTER |
© ESO, 2015
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