for each galaxy using a Bayesian analysis, to account for the degeneracy between physical parameters. Further details may be found in Wild et al. (2016). A library of 10’s of thousands of population synthesis models was created using BC03 and fit to the supercolours to obtain a probability density function for each physical property. A wide range of star formation histories, dust properties, and metallicities were explored, including exponentially declining star formation rates with superimposed stochastic starbursts. Stellar masses were calculated assuming a Chabrier initial mass function (IMF), defined as the stellar mass at the time of observation, i.e. allowing for the fraction of mass in stars returned to the interstellar medium due to mass loss and supernovae. The resulting stellar mass uncertainties from the Bayesian fits are typically $\pm ~0.1$ dex for all populations, assuming BC03 stellar population synthesis models and allowing for uncertainties in the photometric redshifts. The potential impact of stellar mass errors (random and systematic) is discussed further in Section \[sec:uncertainties\].

Figure \[fig:zmass\] shows the resulting distribution of stellar mass as a function of redshift, separated into the three primary populations. Mass completeness limits (95%) were determined as a function of redshift using the method of 