All Figures

Figure 1: HAWK-I Ks-band image of XMMU J2235.3-2557. Only the central 1% of the entire Ks-band image is shown here. The image is approximately 90 on a side, which, in the adopted cosmology, corresponds to 765 kpc at z=1.39. Spectrally confirmed cluster members (Rosati et al., in preparation) are marked with circles. The star that is close to the cluster centre is also marked. The dotted circle that surrounds the central region of the cluster has a diameter of 21 , which corresponds to 180 kpc at z=1.39. The C-M relation (the solid red line in Fig. 2) is determined from galaxies that lie within this circle.

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In the text

Figure 2: Colour magnitude diagram of XMMU J2235.3-2557. Galaxies in the core of the cluster (within the dotted circle that is shown in Fig. 1) are plotted as large red circles. The continuous red line is a fit to the large red symbols that lie within the blue box. Four of these galaxies are spectroscopically confirmed cluster members and are replotted as open squares. The dotted lines represent the detection limits reported in Table 1. The near-horizontal dashed green lines are the result of evolving the red sequence of the Coma cluster backwards in time for different formation redshifts. From top to bottom, the formation redshifts are 5, 4, 3, 2.5 and 2. Cluster members that are outside the core are plotted as small red circles (for those that have no detectable [OII] emission) or small blue squares (for those that have [OII] emission). See the main text for details.

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In the text