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Fig. B.2.
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Same as Fig. B.1 but for a time of t = 2.75 Gyr, where we instead of fitting the averaged column density with a parabola simply determine the furthest upstream location with ⟨NHI⟩≥1020.5 cm−2 (see black triangle). This approach is sufficient and preferred at times, where HI clumps in the CGM upstream the galaxy are absent.
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