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The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. Going to higher redshifts, the effect of the environment should be reversed, inducing rather than suppressing star formation as gas-rich galaxies coalesce in the primeval universe. To this end, unlike its predecessors that were magnitude limited, the selection of VUDS spectroscopic targets was performed primarily through photometric redshift cuts, occasionally supplemented with a variety of magnitude and color (though not all interesting VUDS galaxies are at such high redshifts, see Amorín et al. As a result, the number of spectroscopically confirmed galaxies at these redshifts in the full VUDS sample rivals or exceeds the number of spectroscopically confirmed galaxies from all other surveys combined at redshifts .We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning ofenvironmentally induced quenching. 2013, 2014) have begun to provide a somewhat coherent picture at these redshifts in which galaxy evolution has a complicated dependence on secular (i.e., mass-related) processes, as well as on both the global and the local environment. Indeed, tentative evidence for the reversal of the correlation between star formation rate (SFR) and galaxy density has already been found at slightly higher redshifts (Tran et al. The main novelty of the VUDS observations is the depth of the spectroscopy and the large wavelength coverage that is afforded by the 50 400 s integration time per pointing and per grating with the low-resolution blue and red gratings on VIMOS ().The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy, which appears to be undergoing vigorous coeval nuclear and starburst activity. However, even at such redshifts, the effect of residing in the harsh cluster environment for several Gyr is evident among member galaxies, because the fraction of both red and quiescent galaxies is observed to be in excess of that of the field at similar redshifts (e.g., Patel et al. This combination of wavelength coverage and depth, along with the high redshift of the sample, allows not only for spectroscopic confirmation of the LAE galaxies, galaxies which dominate other high redshift spectroscopic samples, but also for redshift determination from Lyman ) and interstellar medium (ISM) absorption in those galaxies that exhibit no emission line features.The remaining member galaxies appear to have characteristics that are largely similar to the field population. Thus, the VUDS data allow for a selection of a spectroscopic volume-limited sample of galaxies at redshifts 1 at the redshifts of interest for the study presented in this paper (see Cassata et al. The flagging code for VUDS is identical to that of the VIMOS VLT Deep Survey (VVDS; see Le Fèvre et al. Although it has not been, to date, tested extensively whether the same statistics as derived for the VVDS flags apply to the VUDS data (though see discussion in Le Fèvre et al.Though we find weaker evidence of the suppression of the median star formation rates among and differences in the stacked spectra of member galaxies with respect to the field, we defer any conclusions about these trends to future work with the ensemble of protostructures that are found in the full VUDS sample. The lower mass counterparts to galaxy clusters, galaxy groups, also suffer the same ambiguities. At similar redshifts, systematic spectroscopic studies of clusters and cluster galaxies are somewhat rare. 2014), we adopt here the same reliability thresholds for secure spectroscopic redshifts in VUDS as for the VVDS.

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