  We present new results on the evolution of the cosmic star formation rate as
a function of stellar mass in the SXDS-UDS field. We make use of narrow-band
selected emission line galaxies in four redshift slices between z = 1.46 and z
= 0.63, and compute stellar masses by fitting a series of templates to recreate
each galaxy's star formation history. We determine mass-binned luminosity
functions in each redshift slice, and derive the star formation rate density
(rhoSFR) as a function of mass using the [OIII] or [OII] emission lines. We
calculate dust extinction and metallicity as a function of stellar mass, and
investigate the effect of these corrections on the shape of the overall
rhoSFR(M). We find that both these corrections are crucial for determining the
shape of the rhoSFR(M), and its evolution with redshift. The fully corrected
rhoSFR(M) is a relatively flat distribution, with the normalisation moving
towards lower values of rhoSFR with increasing cosmic time/decreasing redshift,
and requiring star formation to be truncated across all masses studied here.
The peak of rhoSFR(M) is found in the 10^10.5<Msun<10^11.0 mass bin at z =
1.46. In the lower redshift slices the location of the peak is less certain,
however low mass galaxies in the range 10^7.0<Msun<10^8.0 play an important
part in the overall rhoSFR(M) out to at least z ~ 1.2.
