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Direct measurements of cosmic ray (CR) species combined with observations oftheir associated gamma-ray emissions can be used to constrain models of CRpropagation, trace the structure of the Galaxy, and search for signatures ofnew physics. The spatial density distribution of the interstellar gas is avital element for all these studies. So far models have employed the 2Dcylindrically symmetric geometry, but their accuracy is well behind that of theavailable data. In this paper, 3D spatial density models for the neutral andmolecular hydrogen are constructed based on empirical model fitting to gasline-survey data. The developed density models incorporate spiral arms andaccount for the warping of the disk, and the increasing gas scale height withradial distance from the Galactic center. They are employed together with theGALPROP CR propagation code to investigate how the new 3D gas models affectcalculations of CR propagation and high-energy gamma-ray intensity maps. Thecalculations made reveal non-trivial features that are directly related to thenew gas models. The best-fit values for propagation model parameters employing3D gas models are presented and they differ significantly from the valuesderived with the 2D gas density models that have been widely used. Thecombination of 3D CR and gas density models provide a more realistic basis forthe interpretation of non-thermal emissions from the Galaxy.

The Three-Dimensional Spatial Distribution of Interstellar Gas in the Milky Way: Implications for Cosmic Rays and High-Energy Gamma-Ray Emissions