Simulated vs. observed UV emission at high redshift: a hint for a clumpy ISM?

Abstract

We discuss the rest-frame UV emission between 5< z < 7 from the MareNostrum High-z Universe, a SPH simulation done with more than 2 billion particles. Cosmological simulations of galaxy formation generally overpredict the UV restframe luminosity function at high redshift, both at the bright and faint ends. In this Letter we explore a dust attenuation model where a larger extinction is applied to star populations younger than a given age, mimicking the effect of a clumpy interstellar medium. We show that this scenario fits reasonably well both the UV luminosity functions and the UV-continuum slopes derived from observations. The model assumes a large obscuration for stars younger than 25 Myr from the gas clouds where they should be embedded at their formation time. We find that the optical depth in these clouds should be between 30 and 100 times larger than the mean optical depth for the homogeneous part of the interstellar medium. These values are one order of magnitude larger than those estimated in local galaxies. Therefore, we conclude that LambdaCDM predictions for the high-z UV emission can accommodate the current observations if we consider a dust extinction model based on the assumption of a clumpy environment at high redshift.

5 pages, 2 figures; few typos corrected; accepted for publication in MNRAS Letters

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• Exploring 21cm - Lyman Alpha emitter synergies for SKA
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• Clustering at high redshift: The connection between Lyman Alpha emitters and Lyman break galaxies
• Modelling the fraction of Lyman Break Galaxies with strong Lyman alpha emission at 5 < z < 7
• Enabling parallel computing in CRASH