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The Galactic Halo’s O VI Resonance Line Intensity

  • Authors: Robin L. Shelton, Shauna M. Sallmen, and Edward B. Jenkins

Shelton, Sallmen, & Jenkins 2007 The Astrophysical Journal 659 365.

  • Provider: AAS Journals

Caption: Fig. 5.

Density of O VI vs. distance along our line of sight for the hypothetical case in which all of the regions are arranged in an end‐to‐end sequence from low to high temperature. The solid curve represents our solution to the power‐law temperature (or length scale) relation for a foreground absorption equivalent to ﹩N_{\mathrm{H}\,\,{}^{{\rm{\small I}}}}=1.0\times 10^{20}﹩ cm−2, ﹩p_{\mathrm{th}\,}/ k=8320﹩ cm−3 K, and ﹩\beta =1.48﹩. On this curve, points are labeled according to their respective values of ﹩\mathrm{log}\,T﹩. The other (dotted) curves represent other values of foreground absorption, as indicated (with ﹩p_{\mathrm{th}\,}/ k﹩ and β in each case set to the respective optimum values; see Table 4).

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