Central Molecular Zone cloud complexes datacubes

Low- and high-velocity gas components in G1.6 do not show such evidence of interaction, suggesting that they are spatially separated. We selected three positions in each cloud complex for further analysis. Based on non-LTE modelling of an ensemble of CH3CN lines, we derived kinetic temperatures of 60-100K and H2 volume densities of 10^4-10^5cm^-3^ in both complexes.

Molecular abundances relative to H2 suggest a similar chemistry of the two clouds, which is moreover similar to that of other GC clouds. We conclude that G1.3 may indeed exhibit signs of cloud-cloud interactions. We propose an interaction of gas that is accreted from the near-side dust lane to the CMZ, with gas pre-existing at this location.

Low- and high-velocity components in G1.6 are rather coincidentally observed along the same line of sight. They may be associated with either overshot decelerated gas from the far-side dust line or actual CMZ gas and high-velocity gas moving on a dust lane. These scenarios would be in agreement with numerical simulations.