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The CII 158 m emission line and the underlying far-infrared (FIR) dust continuum are important tracers for studying star formation and kinematic properties of early galaxies. We present a survey of the CII emission lines and FIR continua of 31 luminous quasars at z>6. 5 using the Atacama Large Millimeter Array (ALMA) and the NOrthern Extended Millimeter Array (NOEMA) at sub-arcsec resolution. This survey more than doubles the number of quasars with CII and FIR observations at these redshifts and enables statistical studies of quasar host galaxies deep into the epoch of reionization. We detect CII emission in 27 quasar hosts with a luminosity range of L ₂₈₈= (0. 3-5. 5) 10⁹~L_ and detect the FIR continuum of 28 quasar hosts with a luminosity range of L ₅₈ₑ= (0. 5-13. 0) 10^12~L_. Both L ₂₈₈ and L ₅₈ₑ are correlated (0. 4) with the quasar bolometric luminosity, albeit with substantial scatter. The quasar hosts detected by ALMA are clearly resolved with a median diameter of 5 kpc. About 40% of the quasar host galaxies show a velocity gradient in CII emission, while the rest show either dispersion-dominated or disturbed kinematics. Basic estimates of the dynamical masses of the rotation-dominated host galaxies yield M ₃ₘ₍= (0. 1-7. 5) 10^11~M_. Considering our findings alongside those of literature studies, we found that the ratio between M ₁₇ and M ₃ₘ₍ is about ten times higher than that of local M ₁₇-M ₃ₘ₍ relation on average but with substantial scatter (the ratio difference ranging from 0. 6 to 60) and large uncertainties.
Wang et al. (Tue,) studied this question.