2021ApJ...910...57S

We study the mass-metallicity relation for 19 members of a spectroscopically confirmed protocluster in the COSMOS field at z = 2.2 (CC2.2), and compare it with that of 24 similarly selected field galaxies at the same redshift. Both samples are Hα emitting sources, chosen from the HiZELS narrowband survey, with metallicities derived from the N2 ([NII]λ6584/ Hα) line ratio. For the mass-matched samples of protocluster and field galaxies, we find that protocluster galaxies with 10^9.9 M_☉ <= M_* <= 10^10.9 M_☉ are metal deficient by 0.10 ± 0.04 dex (2.5σ significance) compared to their coeval field galaxies. This metal deficiency is absent for low-mass galaxies, M_* < 10^9.9 M_☉. Moreover, relying on both spectral energy distribution derived and Hα (corrected for dust extinction based on M_*) star formation rates (SFRs), we find no strong environmental dependence of the SFR-M_* relation; however, we are not able to rule out the existence of small dependence due to inherent uncertainties in both SFR estimators. The existence of 2.5σ significant metal deficiency for massive protocluster galaxies favors a model in which funneling of the primordial cold gas through filaments dilutes the metal content of protoclusters at high redshifts (z >= 2). At these redshifts, gas reservoirs in filaments are dense enough to cool down rapidly and fall into the potential well of the protocluster to lower the gas-phase metallicity of galaxies. Moreover, part of this metal deficiency could be originated from galaxy interactions that are more prevalent in dense environments.