Fig. 10.

H2 (top panel) and CO (bottom panel) vs C I column densities for the GRB molecular gas absorbers studied in this paper. For comparison, we also show a compiled sample of ES-DLAs with a secure detection of H2 from Guimarães et al. (2012), Noterdaeme et al. (2015), Balashev et al. (2017), Ranjan et al. (2018), and selected sightlines through diffuse and translucent molecular clouds in the Milky Way (from Burgh et al. 2010). Top panel: a set of constant C I-to-H2 abundance ratios are shown for guidance. In the bottom panel, the transition region between diffuse and translucent molecular clouds at N(C I)/N(CO) = 1 is shown as well.
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