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The diffuse high-energy gamma-ray emission of the Milky Way arises frominteractions of cosmic-rays (CRs) with interstellar gas and radiation field inthe Galaxy. The neutral hydrogen (H I) gas component is by far the most massiveand broadly distributed component of the interstellar medium. Using the 21-cmemission line from the hyperfine structure transition of atomic hydrogen it ispossible to determine the column density of H I if the spin temperature (Ts) ofthe emitting gas is known. Studies of diffuse gamma-ray emission have generallyrelied on the assumption of a fixed, constant spin temperature for all H I inthe Milky Way. Unfortunately, observations of H I in absorption against brightbackground sources has shown it to vary greatly with location in the Milky Way.We will discuss methods for better handling of spin temperatures for Galacticdiffuse emission modeling using the Fermi-LAT data and direct observation ofthe spin temperature using H I absorption.

H I spin temperature in the Fermi-LAT era