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Towards a multi-scale understanding of the gas-star formation cycle in the Central Molecular Zone

Published online by Cambridge University Press:  09 February 2017

J. M. Diederik Kruijssen
J. M. Diederik Kruijssen*
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraße 12-14, 69120 Heidelberg, Germany email: kruijssen@uni-heidelberg.de
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Abstract

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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.

Keywords

stars: formationISM: cloudsISM: kinematics and dynamicsISM: structureGalaxy: centerGalaxy: evolutionGalaxy: kinematics and dynamicsgalaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S322: The Multi-Messenger Astrophysics of the Galactic Centre , July 2016 , pp. 64 - 74
Copyright
Copyright © International Astronomical Union 2017 

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