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Due to our vantage point in the disk of the Galaxy, its 3D structure is notdirectly accessible. However, knowing the spatial distribution, e.g. of atomicand molecular hydrogen gas is of great importance for interpreting andmodelling cosmic ray data and diffuse emission. Using novel Bayesian inferencetechniques, we reconstruct the 3D densities of atomic and molecular hydrogen inthe Galaxy together with (part of) the galactic velocity field. In order toregularise the infinite number of degrees of freedom and obtain information inregions with missing or insufficient data, we incorporate the correlationstructure of the gas fields into our prior. Basis for these reconstructions arethe data-sets from the HI4PI-survey on the 21-cm emission line and theCO-survey compilation by Dame et al. (2001) on the ($1\rightarrow0$) rotationaltransition together with a variable gas flow model. We present the preliminaryestimated mean surface mass densities and corrections to the prior assumptionof the galactic velocity field. In the future, we plan to relax assumptions onthe optical thickness and include additional data to further constrain eitherthe galactic velocity field or the gas densities.

Bayesian inference of 3D densities of galactic HI and H2