Cosmic rays, gas, and dust in the central molecular zone

Context. The central molecular zone (CMZ) is a unique environment in our Galaxy, with extreme conditions to test our understanding of the gas, dust, and cosmic-ray (CR) physics. Aims. Our goal is to estimate the total gas mass in the direction of the Galactic centre (GC), quantify the various associated uncertainties, and discuss the implications for the estimates of CR energy densities and dust opacities. Methods. The H I 21 cm line and the carbon monoxide isotopes ( 12 CO ( J = 1 → 0), 13 CO ( J = 1 → 0; J = 2 → 1), and C 18 O ( J = 2 → 1)) line emission maps were used to derive the total gas column density. The gas in the CMZ is separated from the disk contribution in position and velocity thanks to its different properties in terms of the velocity dispersion and brightness ratio of CO isotopes. The variations of the X CO factors were modelled relying on both theoretical trends from simulations and empirical corrections. We used the new gas column density estimated together with gamma-ray and dust emission measurements to derive the CR energy density and dust opacities, respectively. Results. The X CO values in the CMZ range from (0.32–1.37) × 10 20 cm −2 K −1 km −1 s, with a distribution that is highly asymmetric and skewed. The median value is X̅ CO CMZ = 0.39 × 10 20 cm −2 K −1 km −1 s. The total gas mass in the CMZ is estimated to be 2.3 −0.3 +0.3 × 10 7 M ⊙ with an ∼10% contribution from the atomic phase. Without removing the disk contamination, the total mass is about twi-ce as higher, and the atomic gas fraction increases to ∼30%. The CR energy density in the CMZ, assuming a 1/r profile, is higher by a factor of two compared to the previous calculations at TeV energies. Conclusions. Towards the GC the contamination from both atomic and molecular gas in the disk is not negligible. Using molecular gas tracers, which probes only the densest molecular cores, leads to an overestimation of the CR energy density, while ignoring the foreground and background contribution leads to an underestimation of the CR energy density in the CMZ.