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Star formation rates on global and cloud scales within the Galactic Centre

Published online by Cambridge University Press:  09 February 2017

A.T. Barnes ,
S.N. Longmore ,
C. Battersby ,
J. Bally  and
J.M.D. Kruijssen
A.T. Barnes
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University
S.N. Longmore
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University
C. Battersby
Affiliation:
Harvard-Smithsonian Center for Astrophysics
J. Bally
Affiliation:
Centre for Astrophysics and Space Astronomy, University of Colorado
J.M.D. Kruijssen
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg Max-Planck Institut für Astronomie
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Abstract

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The environment within the inner few hundred parsecs of the Milky Way, known as the “Central Molecular Zone” (CMZ), harbours densities and pressures orders of magnitude higher than the Galactic Disc; akin to that at the peak of cosmic star formation (Kruijssen & Longmore 2013). Previous studies have shown that current theoretical star-formation models under-predict the observed level of star-formation (SF) in the CMZ by an order of magnitude given the large reservoir of dense gas it contains. Here we explore potential reasons for this apparent dearth of star formation activity.

Keywords

Galaxy: centreISM: cloudsISM: HII regionsstars: formation

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