We use cookies to ensure that we give you the best experience on our website. You can change your cookie settings at any time. Otherwise, we'll assume you're OK to continue.

Durham University

Research & business

View Profile

Publication details for Prof Ray Sharples

Chan, J.C.C., Beifiori, A., Mendel, J.T., Saglia, R.P., Bender, R., Fossati, M., Galametz, A., Wegner, M., Wilman, D.J., Cappellari, M., Davies, R.L., Houghton, R.C.W., Prichard, L.J., Lewis, I.J., Sharples, R. & Stott, J.P. (2016). Sizes, Colour gradients and Resolved Stellar Mass Distributions for the Massive Cluster Galaxies in XMMUJ2235-2557 at z = 1.39. Monthly Notices of the Royal Astronomical Society 458(3): 3181-3209.

Author(s) from Durham


We analyse the sizes, colour gradients, and resolved stellar mass distributions for 36 massive and passive galaxies in the cluster XMMUJ2235-2557 at z = 1.39 using optical and near-infrared Hubble Space Telescope imaging. We derive light-weighted Sérsic fits in five HST bands (i775, z850, Y105, J125, H160), and find that the size decreases by ∼20% going from i775 to H160 band, consistent with recent studies. We then generate spatially resolved stellar mass maps using an empirical relationship between M∗/LH160M∗/LH160 and (z850 − H160) and use these to derive mass-weighted Sérsic fits: the mass-weighted sizes are ∼41% smaller than their rest-frame r-band counterparts compared with an average of ∼12% at z ∼ 0. We attribute this evolution to the evolution in the M∗/LH160M∗/LH160 and colour gradient. Indeed, as expected, the ratio of mass-weighted to light-weighted size is correlated with the M★/L gradient, but is also mildly correlated with the mass surface density and mass-weighted size. The colour gradients (∇z − H) are mostly negative, with a median value of ∼0.45 mag dex−1, twice the local value. The evolution is caused by an evolution in age gradients along the semi-major axis (a), with ∇age = dlog (age)/dlog (a) ∼−0.33, while the survival of weaker colour gradients in old, local galaxies implies that metallicity gradients are also required, with ∇Z = dlog (Z)/dlog (a) ∼−0.2. This is consistent with recent observational evidence for the inside-out growth of passive galaxies at high redshift, and favours a gradual mass growth mechanism, such as minor mergers.