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The Central Molecular Zone (CMZ; the central ~ 500 pc of the Galaxy) is akinematically unusual environment relative to the Galactic disc, with highvelocity dispersions and a steep size-linewidth relation of the molecularclouds. In addition, the CMZ region has a significantly lower star formationrate (SFR) than expected by its large amount of dense gas. An important factorin explaining the low SFR is the turbulent state of the star-forming gas, whichseems to be dominated by rotational modes. However, the turbulence drivingmechanism remains unclear. In this work, we investigate how the Galacticgravitational potential affects the turbulence in CMZ clouds. We focus on theCMZ cloud G0.253+0.016 (`the Brick'), which is very quiescent and unlikely tobe kinematically dominated by stellar feedback. We demonstrate that severalkinematic properties of the Brick arise naturally in a cloud-scalehydrodynamics simulation that takes into account the Galactic gravitationalpotential. These properties include the line-of-sight velocity distribution,the steepened size-linewidth relation, and the predominantly solenoidal natureof the turbulence. Within the simulation, these properties result from theGalactic shear in combination with the cloud's gravitational collapse. This isa strong indication that the Galactic gravitational potential plays a crucialrole in shaping the CMZ gas kinematics, and is a major contributor tosuppressing the SFR by inducing predominantly solenoidal turbulent modes.

Kinematics of Galactic Centre clouds shaped by shear-seeded solenoidal turbulence