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Galaxies arrive on the red sequences of clusters at high redshift ($z>1$)once their star formation is quenched and evolve passively thereafter. However,we have previously found that cluster red sequence galaxies (CRSGs) undergosignificant morphological evolution subsequent to the cessation of starformation, at some point in the past 9-10~Gyr. Through a detailed study of alarge sample of cluster red sequence galaxies spanning $0.2<z<1.4$ we elucidatethe details of this evolution. Below $z \sim 0.5-0.6$ (in the last 5-6 Gyr)there is little or no morphological evolution in the population as a whole,unlike in the previous 4-5 Gyrs. Over this earlier time (i) disk-like systemswith S{\'e}rsic $n < 2$ progressively disappear, as (ii) the range of theiraxial ratios similarly decreases, removing the most elongated systems (thoseconsistent with thin disks seen at an appreciable inclination angle), and (iii)radial colour gradients (bluer outwards) decrease in an absolute sense fromsignificant age-related gradients to a residual level consistent with themetallicity-induced gradients seen in low redshift cluster members. Thedistribution of their effective radii shows some evidence of evolution,consistent with growth of {\it at most} a factor $<1.5$ between $z\sim 1.4$ and$z \sim 0.5$, significantly less than for comparable field galaxies, while thedistribution of their central ($<1$kpc) bulge surface densities shows noevolution at least at $z<1$. A simple model involving the fading and thickeningof a disk component after comparatively recent quenching (after $z\sim 1.5$)around an otherwise passively evolving older spheroid component is consistentwith all of these findings.

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr