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Radiative Feedback Effects during Cosmic Reionization

Published online by Cambridge University Press:  12 October 2016

David Sullivan  and
Ilian T. Iliev
David Sullivan
Affiliation:
Astronomy Centre, Department of Physics & Astronomy, Pevensey II Building, University of Sussex, Falmer, Brighton BN1 9QH, United Kingdom email: D.Sullivan@sussex.ac.uk
Ilian T. Iliev
Affiliation:
Astronomy Centre, Department of Physics & Astronomy, Pevensey II Building, University of Sussex, Falmer, Brighton BN1 9QH, United Kingdom email: D.Sullivan@sussex.ac.uk Speaker, email: I.T.Iliev@sussex.ac.uk
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Abstract

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We present coupled radiation hydrodynamical simulations of the epoch of reionization, aimed at probing self-feedback on galactic scales. Unlike previous works, which assume a (quasi) homogeneous UV background, we self-consistently evolve both the radiation field and the gas to model the impact of previously unresolved processes such as spectral hardening and self-shielding. We find that the characteristic halo mass with a gas fraction half the cosmic mean, Mc(z), a quantity frequently used in semi-analytical models of galaxy formation, is significantly larger than previously assumed. While this results in an increased suppression of star formation in the early Universe, our results are consistent with the extrapolated stellar abundance matching models from Moster et al. 2013.

Keywords

Radiative transfermethods: numericalstars: formationgalaxies: formationgalaxies: high-redshiftintergalactic mediumlarge-scale structure of universe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 372 - 377
Copyright
Copyright © International Astronomical Union 2016 

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