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Fig. 7

image

Left panel: rest-frame NUV-r+ versus r+ color-magnitude diagram for the zspec members of the PCl J1001+0220 proto-cluster (red diamonds) and a matched coeval field sample at 4.23 < z < 4.88 (small navy dots) at stellar masses . The stellar mass cut is imposed here in an attempt to mitigate any induced differential bias between the field and proto-cluster members. Overplotted are the expected locations in this phase space of a progentor of a low-redshift cluster L* galaxy (assuming passive evolution) estimated from synthetic spectra (see Sect. 4.2.1) at different stellar-phase metallicities and with different SFHs. The gray dashed track is generated from an instantaneous burst while the three green tracks are generated from an exponentially declining SFH with τ = 100 Myr at three different stellar-phase metallicities. Age ticks along each track indicate the time since the inception of the star formation event. Color and magnitude histograms for each sample are normalizedto each other such that they contain the same area. The solid light blue area indicates the area of this phase space for which VUDS is no longer representative of the underlying photometric sample at these redshifts and stellar masses (see Sect. 4.2.1). Right panel: rest-frame MNUV - versus color-stellar-mass diagram for the identical samples as in the left panel. The meanings of all symbols and lines are unchanged. While some of the brightest, reddest, and most (stellar) massive galaxies in the entire spectroscopic sample at these redshifts fall within PCl J1001+0220, only a moderately significant difference in the average brightness and a significant difference in the stellar mass distribution is detected relative to the coeval field population.

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