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 \geq 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 } \mathrm { 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 } \geq 5 \times 10 ^ { 10 } \mathrm { 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 .