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Quenching in gas-rich Milky Way-type galaxies

Published online by Cambridge University Press:  02 August 2018

S. Khoperskov ,
M. Haywood ,
P. Di Matteo ,
M. Lehnert  and
F. Combes
S. Khoperskov
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: sergey.khoperskov@obspm.fr
M. Haywood
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: sergey.khoperskov@obspm.fr
P. Di Matteo
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: sergey.khoperskov@obspm.fr
M. Lehnert
Affiliation:
Institut d’Astrophysique de Paris, CNRS UMR 7095, Université Pierre et Marie Curie, 98bis Bd Arago, 75014 Paris, France
F. Combes
Affiliation:
Observatoire de Paris, LERMA, College de France, CNRS, PSL, Sorbonne Univ. UPMC, F-75014, Paris, France
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Abstract

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To explore the relation between bar formation and star formation in Milky Way-type galaxies quantitatively, we simulated gas-rich disk isolated galaxies. We find that the action of the stellar bar efficiently quenches star formation, reducing the star-formation rate by a factor of 10 in less than 1 Gyr. Analytical and self-consistent galaxy simulations with bars suggest that the action of the stellar bar increases the gas random motions within the co-rotation radius of the bar. Indeed, we detect an increase in the gas velocity dispersion at the end of the bar formation phase. The star formation efficiency decreases rapidly, and in all of our models, the bar quenches the star formation in the galaxy. The star-formation efficiency is much lower in simulated barred compared to unbarred galaxies and more rapid bar formation implies more rapid quenching.

Keywords

galaxies: evolutiongalaxies: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 314 - 315
Copyright
Copyright © International Astronomical Union 2018 

References

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