Figure 11 from Characterizing the Transition from Diffuse Atomic to Dense Molecular Clouds in the Magellanic Clouds with [C II], [C I], and CO

Image Details

View Article Bookmark & Share

Choose export citation format:

Export Citation

Hi-Resolution Export to PDF PPT Format

Characterizing the Transition from Diffuse Atomic to Dense Molecular Clouds in the Magellanic Clouds with [C II], [C I], and CO

Authors: Jorge L. Pineda, William D. Langer, Paul F. Goldsmith, Shinji Horiuchi, Thomas B. H. Kuiper, Erik Muller, Annie Hughes, Jürgen Ott, Thangasamy Velusamy, and Tony Wong

2017 The Astrophysical Journal 839 107.

Provider: AAS Journals

Caption: Figure 11.

Comparison between the N(H⁺) + ﹩N({{\rm{H}}}^{0})﹩ + 2N(H₂) hydrogen column densities derived in this study and the visual extinction derived from dust continuum observations. The lines represent the total hydrogen column density predicted for a given A_V, assuming N(H)/﹩{A}_{{\rm{V}}}﹩ = 7.17 × 10²¹ cm⁻² mag⁻¹ for the LMC and 1.68 × 10²² cm⁻² mag⁻¹ for the SMC (Section 4.2).

Other Images in This Article

Copyright and Terms & Conditions