The Morphological Transformation of Red-Sequence Galaxies in the Distant
  Cluster XMMU J1229+0151
  We present the results of a detailed analysis of galaxy properties along the
red sequence in XMMU J1229+0151, an X-ray selected cluster at $z=0.98$ drawn
from the HAWK-I Cluster Survey (HCS). Taking advantage of the broad photometric
coverage and the availability of 77 spectra in the cluster field, we fit
synthetic spectral energy distributions, and estimate stellar masses and
photometric redshifts, which we use to determine the cluster membership. We
investigate morphological and structural properties of red sequence galaxies
and find that elliptical galaxies populate the bright end, while S0 galaxies
represent the predominant population at intermediate luminosities, with their
fraction decreasing at fainter magnitudes. A comparison with the low-redshift
sample of the WINGS cluster survey reveals that at $z\sim1$ the bright end of
the red sequence of XMMU J1229+0151 is richer in S0 galaxies. The faint end of
the red sequence in XMMUJ1229+0151 appears rich in disc-dominated galaxies,
which are rarer in the low redshift comparison sample at the same luminosities.
Despite these differences between the morphological composition of the red
sequence in XMMUJ1229+0151 and in low redshift samples, we find that to within
the uncertainties, no such difference exists in the ratio of luminous to faint
galaxies along the red sequence.
