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As the progenitors of present-day galaxy clusters, protoclusters areexcellent laboratories to study galaxy evolution. Since existing observationsof protoclusters are limited to the detected constituent galaxies at UV and/orinfrared wavelengths, the details of how typical galaxies grow in these young,pre-virialized structures remain uncertain. We measure the total stellar massand star formation within protoclusters, including the contribution from faintundetected members by performing a stacking analysis of 211 $z=2-4$protoclusters selected as Planck cold sources. We stack WISE and Herschel/SPIREimages to measure the angular size and the spectral energy distribution of theintegrated light from the protoclusters. The fluxes of protoclusters selectedas Planck cold sources can be contaminated by line of sight interlopers. Usingthe WebSky simulation, we estimate that a single protocluster contributes$33\pm15$% of the flux of a Planck cold source on average. After thiscorrection, we obtain a total star formation rate of $7.3\pm3.2 \times 10^3\M_{\odot} {\rm yr}^{-1}$ and a total stellar mass of $4.9\pm 2.2\times 10^{12}\M_{\odot}$. Our results indicate that protoclusters have, on average, 2x morestar formation and 4x more stellar mass than the total contribution fromindividually-detected galaxies in spectroscopically-confirmed protoclusters.This suggests that much of the total flux within $z=2-4$ protoclusters comesfrom galaxies with luminosities lower than the detection limit of SPIRE($L_{IR} < 3 \times 10^{12} L_{\odot}$). Lastly, we find that protoclusterssubtend a half-light radius of 2.8' (4.2-5.8 cMpc) which is consistent withsimulations.

Tracing the Total Stellar Mass and Star Formation of High-Redshift Protoclusters