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Gamma ray observations have found evidence of an extremely energetic outflowemanating from the Galactic Centre, and an `excess' of emission at GeV energiestowards the Galactic Centre over that expected from current models. Determiningwhether the outflow is AGN- or star formation-driven, and whether the `excess'is astrophysical in origin or requires new physics (e.g. self-annihilation ofdark matter), requires the accurate modelling of the expected energy injectionfrom astrophysical sources and the subsequent interaction with the surroundingenvironment. We briefly summarise current constraints on the distribution ofgas and young stars in the inner few hundred parsec of the Galaxy that can beincluded in future 2D and 3D modelling of the astrophysical gamma ray emission.The key points to highlight with respect to predominantly axisymmetric modelscurrently in use are: (i) the distribution of dense gas, young stars andinterstellar radiation field is highly asymmetric around the Galactic Centre;(ii) star formation is almost exclusively constrained to a Galactocentricradius of ~100pc; (iii) the star formation rate in this region has beenconstant at <0.1Msun/yr to within a factor of 2 over the last ~5 Myr.

Constraints on the distribution of gas and young stars in the Galactic Centre in the context of interpreting gamma ray emission features