Towards a multi-scale understanding of the gas-star formation cycle in the Central Molecular Zone
arXiv:1609.08158 · doi:10.1017/S1743921316012138
Abstract
The Central Molecular Zone (CMZ, the central 500 pc of the Milky Way) contains the largest reservoir of high-density molecular gas in the Galaxy, but forms stars at a rate 10-100 times below commonly-used star formation relations. We discuss recent efforts in understanding how the nearest galactic nucleus forms its stars. The latest models of the gas inflow, star formation, and feedback duty cycle reproduce the main observable features of the CMZ, showing that star formation is episodic and that the CMZ currently resides at a star formation minimum. Using orbital modelling, we derive the three-dimensional geometry of the CMZ and show how the orbital dynamics and the star formation potential of the gas are closely coupled. We discuss how this coupling reveals the physics of star formation and feedback under the conditions seen in high-redshift galaxies, and promotes the formation of the densest stellar clusters in the Galaxy.
arXiv comment11 pages, 3 figures; keynote talk to appear in the proceedings of 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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