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The physical and chemical properties of the circumgalactic medium (CGM) at$z\gtrsim6$ have been studied successfully through the absorption in thespectra of background Quasi-Stellar Objects (QSOs). One of the most crucialquestions is to investigate the nature and location of the source galaxies thatgive rise to these early metal absorbers. Theoretical models suggest thatmomentum-driven outflows from typical star-forming galaxies can eject metalsinto the CGM and the intergalactic medium (IGM) at z=5-6. Deep, dedicatedsurveys have searched for Ly$\alpha$ emission associated with strong CIVabsorbers at $z\approx 6$, but only a few Ly$\alpha$ emitter candidates havebeen detected. Interpreting these detections is moreover ambiguous becauseLy$\alpha$ is a resonant line, raising the need for complementary techniquesfor detecting absorbers' host galaxies. Here, using Atacama Large MillimeterArray (ALMA), we report a [C II] 158$\mu$m emitter associated with a stronglow-ionization absorber, OI, at $z=5.978$. The projected impact parameterbetween OI and [C II] emitter is 20.0 kpc. The measured [C II] luminosity is$7.0\times 10^7$ solar luminosities. Further analysis indicates that strong OIabsorbers may reside in the circumgalactic medium of massive halos one to twoorders of magnitude more massive than expected values.

A [C II] 158$\mu$m Emitter Associated with an OI Absorber at the End of the Reionization Epoch