Molecular gas kinematics of the CMZ: Great oaks from little acorns grow

Abstract

The central molecular zone (CMZ) hosts some of the most massive and dense molecular clouds and star clusters in the Galaxy, offering an important window into star formation under extreme conditions. Star formation in this extreme environment may be closely linked to the 3-D distribution and orbital dynamics of the gas. Here I discuss how our new, accurate description of the $\{l,b,v\}$ structure of the CMZ is helping to constrain its 3-D geometry. I also present the discovery of a highly-regular, corrugated velocity field located just upstream from the dust ridge molecular clouds (which include G0.253+0.016 and Sgr B2). The extremes in this velocity field correlate with a series of massive ($\sim 10^4$ M${}_{\odot }$) cloud condensations. The corrugation wavelength ($\sim 23$ pc) and cloud separation ($\sim 8$ pc) closely agree with the predicted Toomre ($\sim 17$ pc) and Jeans ($\sim 6$ pc) lengths, respectively. I conclude that gravitational instabilities are driving the formation of molecular clouds within the Galactic Centre gas stream. Furthermore, I suggest that these seeds are the historical analogues of the dust ridge molecular clouds - possible progenitors of some of the most massive and dense molecular clouds in the Galaxy. If our current best understanding for the 3-D geometry of this system is confirmed, these clouds may pinpoint the beginning of an evolutionary sequence that can be followed, in time, from cloud condensation to star formation.

arXiv commentProceedings IAU Symposium 322, The Multi-Messenger Astrophysics of the Galactic Centre, Eds. R. Crocker, S. Longmore & G. Bicknell, Cambridge University Press

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