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[Si II], [Fe II], [C II], and H2 Emission from Massive Star‐forming Regions

  • Authors: Michael J. Kaufman, Mark. G. Wolfire, and David J. Hollenbach

Kaufman, Wolfire, & Hollenbach 2006 The Astrophysical Journal 644 283.

  • Provider: AAS Journals

Caption: Fig. 16.

Schematic representation of the merged H II region and PDR models. ﹩P_{\mathrm{H}\,\,{}^{{\rm{\small II}}}}=P_{\mathrm{PDR}\,}﹩. Starburst99 is used for the cluster spectrum. Mappings is used for the H II region structure; emitted H II region spectrum; ﹩[ \mathrm{Fe}\,\ {}^{{\rm{\small II}}}] _{\mathrm{H}\,\,{}^{{\rm{\small II}}}}﹩, ﹩[ \mathrm{Si}\,\ {}^{{\rm{\small II}}}] _{\mathrm{H}\,\,{}^{{\rm{\small II}}}}﹩, and ﹩[ \mathrm{C}\,\ {}^{{\rm{\small II}}}] _{\mathrm{H}\,\,{}^{{\rm{\small II}}}}﹩ emission; and RS. The emitted spectrum plus RS gives G0. Our PDR models give [Fe II]PDR, [Si II]PDR, [C II]PDR, and H2 emission. AV in the H II region is ≲1, AV in the PDR is gsim2, and AV at the H I/H2 boundary is ≲1.

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