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We study the mass-metallicity relation for 19 members of aspectroscopically-confirmed protocluster in the COSMOS field at $z=2.2$(CC2.2), and compare it with that of 24 similarly selected field galaxies atthe same redshift. Both samples are $\rm H\alpha$ emitting sources, chosen fromthe HiZELS narrow-band survey, with metallicities derived from $\rm N2\(\frac{\rm [NII] \lambda 6584}{\rm H \alpha})$ line ratio. For the mass-matchedsamples of protocluster and field galaxies, we find that protocluster galaxieswith $10^{9.9} \rm M_\odot \leq M_* \leq 10^{10.9} \rm M_\odot$ are metaldeficient by $0.10 \pm 0.04$ dex ($2.5\sigma$ significance) compared to theircoeval field galaxies. This metal deficiency is absent for low mass galaxies,$\rm M_* < 10^{9.9} \rm M_\odot$. Moreover, relying on both SED-derived and$\rm {H\alpha}$ (corrected for dust extinction based on $\rm {M_*}$) SFRs, wefind no strong environmental dependence of SFR-$\rm {M_*}$ relation, however,we are not able to rule out the existence of small dependence due to inherentuncertainties in both SFR estimators. The existence of $2.5\sigma$ significantmetal deficiency for massive protocluster galaxies favors a model in whichfunneling of the primordial cold gas through filaments dilutes the metalcontent of protoclusters at high redshifts ($z \gtrsim 2$). At these redshifts,gas reservoirs in filaments are dense enough to cool down rapidly and fall intothe potential well of the protocluster to lower the gas-phase metallicity ofgalaxies. Moreover, part of this metal deficiency could be originated fromgalaxy interactions which are more prevalent in dense environments.

Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2