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How the first stars shaped the faintest gas-dominated dwarf galaxies

Published online by Cambridge University Press:  09 May 2016

Robbert Verbeke ,
Bert Vandenbroucke  and
Sven De Rijcke
Robbert Verbeke
Affiliation:
Sterrenkundig Observatorium, Ghent University Krijgslaan281, S9, 9000 Gent, Belgium email: [email protected]
Bert Vandenbroucke
Affiliation:
Sterrenkundig Observatorium, Ghent University Krijgslaan281, S9, 9000 Gent, Belgium email: [email protected]
Sven De Rijcke
Affiliation:
Sterrenkundig Observatorium, Ghent University Krijgslaan281, S9, 9000 Gent, Belgium email: [email protected]
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Abstract

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Cosmological simulations predict that dark matter halos with circular velocities lower than 30 km/s should have lost most of their neutral gas by heating of the ultra-violet background. This is in stark contrast with gas-rich galaxies such as e.g. Leo T, Leo P and Pisces A, which all have circular velocities of ~15 km/s (Ryan-Weber et al. 2008, Bernstein-Cooper et al. 2014, Tollerud et al. 2015). We show that when we include feedback from the first stars into our models, simulated dwarfs have very different properties at redshift 0 than when this form of feedback is not included. Including this Population-III feedback leads to galaxies that lie on the baryonic Tully-Fisher relation over the entire mass range of star forming dwarf galaxies, as well as reproducing a broad range of other observational properties.

Keywords

dwarf galaxiesfirst starsgalaxy formationgalaxy evolugtion
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Issue S317: The General Assembly of Galaxy Halos: Structure, Origin and Evolution , August 2015 , pp. 360 - 361
Copyright
Copyright © International Astronomical Union 2016 

References

Bernstein-Cooper, E. Z., Cannon, J. M., Elson, E. C., et al. 2014, AJ, 148, 35Google Scholar
McGaugh, S. S. 2012, AJ, 143, 40Google Scholar
Ryan-Weber, E. V., Begum, A., Oosterloo, T., et al. 2008, MNRAS, 384, 535Google Scholar
Susa, H., Hasegawa, K., & Tominaga, N. 2014, ApJ, 792, 32Google Scholar
Tollerud, E. J., Geha, M. C., Grcevich, J., Putman, M. E., & Stern, D. 2015, ApJL, 798, L21Google Scholar
Verbeke, R., Vandenbroucke, B., & De Rijcke, S., Submitted to ApJGoogle Scholar