Figure 3 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 3.

Ratio of the TIR intensity (Section 5.4) to the H⁰ column density (Section 3.2) as a function of the visual extinction (Section 4.1) for the entire LMC and SMC. We also include data points that correspond to those in our sample in the LMC and SMC. The grayscale represents the number of pixels at a given TIR/N(H⁰) and A_V bin, with contour lines representing 2, 10, 100, and 1000 pixels.

Other Images in This Article

Copyright and Terms & Conditions