Kinematics of $z\geq 6$ galaxies from [CII] line emission
  We study the kinematical properties of galaxies in the Epoch of Reionization
via the [CII] 158$\mu$m line emission. The line profile provides information on
the kinematics as well as structural properties such as the presence of a disk
and satellites. To understand how these properties are encoded in the line
profile, first we develop analytical models from which we identify disk
inclination and gas turbulent motions as the key parameters affecting the line
profile. To gain further insights, we use "Althaea", a highly-resolved ($30\,
\rm pc$) simulated prototypical Lyman Break Galaxy, in the redshift range $z =
6-7$, when the galaxy is in a very active assembling phase. Based on
morphology, we select three main dynamical stages: I) Merger , II) Spiral Disk,
and III) Disturbed Disk. We identify spectral signatures of merger events,
spiral arms, and extra-planar flows in I), II), and III), respectively. We
derive a generalised dynamical mass vs. [CII]-line FWHM relation. If precise
information on the galaxy inclination is (not) available, the returned mass
estimate is accurate within a factor $2$ ($4$). A Tully-Fisher relation is
found for the observed high-$z$ galaxies, i.e. $L_{\rm[CII]}\propto
(FWHM)^{1.80\pm 0.35}$ for which we provide a simple, physically-based
interpretation. Finally, we perform mock ALMA simulations to check the
detectability of [CII]. When seen face-on, Althaea is always detected at $>
5\sigma$; in the edge-on case it remains undetected because the larger
intrinsic FWHM pushes the line peak flux below detection limit. This suggests
that some of the reported non-detections might be due to inclination effects.
