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We carry out a systematic study of the density structure of gas in theCentral Molecular Zone (CMZ) in the Galactic center by extracting clumps fromthe APEX Telescope Large Area Survey of the Galaxy survey at 870 $\mu$m. Wefind that the clumps follow a scaling of $m = \rho_0 r^3$ which corresponds toa characteristic density of $n_{\rm H_2} = 1.6 \times 10^3\,\rm cm^{-3}$($\rho_0 =112\;M_{\odot}\;\rm pc^{-3}$) with a variation of $\approx 0.5\,\rmdex$, where we assumed a gas-to-dust mass ratio of 100. This characteristicdensity can be interpreted as the result of thermal pressure equilibriumbetween the molecular gas and the warm ambient interstellar medium. Such anequilibrium can plausibly be established since shear has approximately the samestrength as self-gravity. Our findings may explain the fact that star formationin the CMZ is highly inefficient compared to the rest of the Milky Way disk. Wealso identify a population of clumps whose densities are two orders ofmagnitudes higher in the vicinity of the Sgr B2 region, which we propose areproduced by collisions between the clumps of lower densities. For thesecollisions to occur, processes such as compressive tides probably have createdthe appropriate condition by assembling the clumps together.

astrophysical journal/the astrophysical journal

A mean density of $112\, M_{\odot}\,\rm pc^{-3}$ for Central Molecular  Zone clumps -- Evidences for shear-enabled pressure equilibrium in the  Galactic Center