GAMA/G10-COSMOS/3D-HST : evolution of the galaxy stellar mass function over 12.5 Gyr
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Using a combined and consistently analysed GAMA, G10-COSMOS, and 3D-HST data set, we explore the evolution of the galaxy stellar mass function over lookback times tL ∈ [0.2, 12.5] h70-1 Gyr. We use a series of volume-limited samples to fit Schechter functions in bins of ~constant lookback time and explore the evolution of the best-fitting parameters in both single and two-component cases. In all cases, we employ a fitting procedure that is robust to the effects of Eddington bias and sample variance. Surprisingly, when fitting a two-component Schechter function, we find essentially no evidence of temporal evolution in M*, the two α slope parameters, or the normalization of the low-mass component. Instead, our fits suggest that the various shape parameters have been exceptionally stable over cosmic time, as has the normalization of the low-mass component, and that the evolution of the stellar mass function is well described by a simple build-up of the high-mass component over time. When fitting a single component Schechter function, there is an observed evolution in both M* and α however, this is interpreted as being an artefact. Finally, we find that the evolution of the stellar mass function, and the observed stellar mass density, can be well described by a simple model of constant growth in the high-mass source density over the last 11 h70-1 Gyr.
Wright , A H , Driver , S P & Robotham , A S G 2018 , ' GAMA/G10-COSMOS/3D-HST : evolution of the galaxy stellar mass function over 12.5 Gyr ' Monthly Notices of the Royal Astronomical Society , vol. 480 , no. 3 , pp. 3491-3502 . https://doi.org/10.1093/MNRAS/STY2136
Monthly Notices of the Royal Astronomical Society
Copyright © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://doi.org/10.1093/mnras/sty2136
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