Kavli Affiliate: Ran Wang
| First 5 Authors: Feige Wang, Jinyi Yang, Xiaohui Fan, Bram Venemans, Roberto Decarli
| Summary:
The [CII] 158 $mu$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 $L_{rm
[CII]}=(0.3-5.5)times10^9~L_odot$ and detect the FIR continuum of 28 quasar
hosts with a luminosity range of $L_{rm FIR}=(0.5-13.0)times10^{12}~L_odot$.
Both $L_{rm [CII]}$ and $L_{rm FIR}$ are correlated ($rhosimeq0.4$) with
the quasar bolometric luminosity, albeit with substantial scatter. The quasar
hosts detected by ALMA are clearly resolved with a median diameter of $sim$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 $M_{rm dyn}=(0.1-7.5)times10^{11}~M_odot$. Considering
our findings alongside those of literature studies, we found that the ratio
between $M_{rm BH}$ and $M_{rm dyn}$ is about ten times higher than that of
local $M_{rm BH}-M_{rm dyn}$ relation on average but with substantial scatter
(the ratio difference ranging from $sim$0.6 to 60) and large uncertainties.
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