Characterizing the evolution of the faint end of the cluster red sequence ( RS ) galaxy luminosity function ( GLF ) with redshift is a milestone in understanding galaxy evolution .
However , the community is still divided in that respect , hesitating between an enrichment of the RS due to efficient quenching of blue galaxies from z \sim 1 to present-day or a scenario in which the RS is built at a higher redshift and does not evolve afterwards .
Recently , it has been proposed that surface brightness ( SB ) selection effects could possibly solve the literature disagreement , accounting for the diminishing of the RS faint population in ground based observations .
We investigate this hypothesis by comparing the RS GLFs of 16 CLASH clusters computed independently from ground-based Subaru/Suprime-Cam V and Ip or Ic and space-based HST/ACS F606W and F814W images in the redshift range 0.187 \leq z \leq 0.686 .
We stack individual cluster GLFs in two redshift ( 0.187 \leq z \leq 0.399 and 0.400 \leq z \leq 0.686 ) and two mass ( 6 \times 10 ^ { 14 } M _ { \odot } \leq M _ { 200 } < 10 ^ { 15 } M _ { \odot } and 10 ^ { 15 } M _ { \odot } \leq M _ { 200 } ) bins , and also measure the evolution with the enclosing radius from 0.5 Mpc up to the virial radius for the Subaru large field of view data .
Finally , we simulate the low redshift clusters at higher redshift to investigate SB dimming effects .

We find similar RS GLFs for space and ground based data , with a difference of 0.2 \sigma in the faint end parameter \alpha when stacking all clusters together and a maximum difference of 0.9 \sigma in the case of the high redshift stack , demonstrating a weak dependence on the type of observations in the probed range of redshift and mass .
When considering the full sample , we estimate \alpha = -0.76 \pm 0.07 and \alpha = -0.78 \pm 0.06 with HST and Subaru respectively .
We note a mild variation of the faint end between the high and low redshift subsamples at a 1.7 \sigma and 2.6 \sigma significance .
We investigate the effect of SB dimming by simulating our low redshift galaxies at high redshift .
We measure an evolution in the faint end slope of less than 1 \sigma in this case , implying that the observed signature is moderately larger than one would expect from SB dimming alone , and indicating a true evolution in the faint end slope .
Finally , we find no variation with mass or radius in the probed range of these two parameters .
We therefore conclude that quenching is mildly affecting cluster galaxies at z \lesssim 0.7 leading to a small enrichment of the RS until today , and that the different faint end slopes observed in the literature are probably due to specific cluster-to-cluster variation .