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The Planck satellite has identified more than 2000 protocluster candidateswith extreme star formation rates (SFRs). Here, we present the spectroscopicidentification of a Planck-selected protocluster located in the Cosmos field,PHz G237.01+42.50 (G237). G237 contains a galaxy overdensity of 31spectroscopically identified galaxies at z~2.16 (significant at 5.4 sigma) in a10'x11' region. The overdensity contains two substructures or protoclusters at<z>~2.16 and 2.195 with estimated halo masses at z=0 of ~(5-6)x10^14 Msun. Theoverdensity total SFR, ~4000 Msun/yr, is higher than predicted by simulationsbut much smaller than the SFR derived from the Planck data. The analysis of theHerschel data, in combination with the available ancillary data, shows thatsuch a difference is due to an effect of source alignment along the line ofsight that produces a 5 sigma overdensity of red Herschel sources in the field.We analyze the members' UV spectra and UV-far-infrared spectral energydistributions to derive their SFR, stellar mass, and metallicity. Galaxymembers include blue star-forming galaxies and AGN with SFRs and stellar massesconsistent with the main sequence. AGN, identified through optical spectroscopyor X-ray data, represent a significant fraction (20+/-10%) of all members ofthe protocluster at z=2.16, and they are powerful enough to produce radiativefeedback. The core of this protocluster, besides being denser, includes membersthat are, on average, more massive and star-forming and contains a largerfraction of AGN and Herschel-detected galaxies than the full sample, suggestingan environmental effect on galaxy growth. A comparison between G237 and otherprotoclusters in the literature at similar redshifts reveals some common traitsand differences that reflect both observational biases and a diversity inintrinsic properties that is not yet fully understood.

Spectroscopic observations of PHz G237.01+42.50: A galaxy protocluster at z=2.16 in the Cosmos field