The MaGICC volume: reproducing statistical properties of high redshift galaxies

Abstract

We present a cosmological hydrodynamical simulation of a representative volume of the Universe, as part of the Making Galaxies in a Cosmological Context (MaGICC) project. MaGICC uses a thermal implementation for supernova and early stellar feedback. This work tests the feedback model at lower resolution across a range of galaxy masses, morphologies and merger histories. The simulated sample compares well with observations of high redshift galaxies ($z\ge 2$) including the stellar mass - halo mass ($M_{\star }-M_h$ ) relation, the Galaxy Stellar Mass Function (GSMF) at low masses ($M_{\star }<5\times 10^{10}{M}_{\odot }$ ) and the number density evolution of low mass galaxies. The poor match of $M_{\star }-M_h$ and the GSMF at high masses ($M_{\star }\ge 5\times 10^{10}{M}_{\odot }$ ) indicates supernova feedback is insufficient to limit star formation in these haloes. At $z=0$, our model produces too many stars in massive galaxies and slightly underpredicts the stellar mass around $L_{\star }$ mass galaxy. Altogether our results suggest that early stellar feedback, in conjunction with supernovae feedback, plays a major role in regulating the properties of low mass galaxies at high redshift.

Simulation extended to z=0, conclusions unchanged. Accepted for publication in MNRAS

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