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We present the results of our Keck/DEIMOS spectroscopic follow-up ofcandidate galaxies of i-band-dropout protocluster candidate galaxies at$z\sim6$ in the COSMOS field. We securely detect Lyman-$\alpha$ emission linesin 14 of the 30 objects targeted, 10 of them being at $z=6$ with asignal-to-noise ratio of $5-20$, the remaining galaxies are eithernon-detections or interlopers with redshift too different from $z=6$ to be partof the protocluster. The 10 galaxies at $z\approx6$ make the protocluster oneof the riches at $z>5$. The emission lines exhibit asymmetric profiles withhigh skewness values ranging from 2.87 to 31.75, with a median of 7.37. Thisasymmetry is consistent with them being Ly$\alpha$, resulting in a redshiftrange of $z=5.85-6.08$. Using the spectroscopic redshifts, we re-calculate theoverdensity map for the COSMOS field and find the galaxies to be in asignificant overdensity at the $4\sigma$ level, with a peak overdensity of$\delta=11.8$ (compared to the previous value of $\delta=9.2$). Theprotocluster galaxies have stellar masses derived from Bagpipes SED fits of$10^{8.29}-10^{10.28} \rm \,M_{\rm \odot}$ and star formation rates of$2-39\,\rm M_{\rm \odot}\rm\,yr^{-1}$, placing them on the main sequence atthis epoch. Using a stellar-to-halo-mass relationship, we estimate the darkmatter halo mass of the most massive halo in the protocluster to be $\sim10^{12}\rm M_{\rm \odot}$. By comparison with halo mass evolution tracks fromsimulations, the protocluster is expected to evolve into a Virgo- or Coma-likecluster in the present day.

DEIMOS spectroscopy of $z=6$ protocluster candidate in COSMOS -- A massive protocluster embedded in a large scale structure?