A SkyMapper view of the Large Magellanic Cloud: The dynamics of stellar
  populations
  We present the first SkyMapper stellar population analysis of the Large
Magellanic Cloud (hereafter LMC),including the identification of 3578 candidate
Carbon Stars through their extremely red $g-r$ colours. Coupled with Gaia
astrometry, we analyse the distribution and kinematics of this Carbon Star
population, finding the LMC to be centred at $(R.A., Dec.) =
(80.90^{\circ}\pm{0.29}, -68.74^{\circ}\pm{0.12})$, with a bulk proper motion
of $(\mu_{\alpha},\mu_{\delta}) = (1.878\pm0.007,0.293\pm0.018) \mathrm{mas\
yr^{-1}}$ and a disk inclination of $i = 25.6^{\circ}\pm1.1$ at position angle
$\theta = 135.6^{\circ}\pm 3.3^{\circ}$. We complement this study with the
identification and analysis of additional stellar populations, finding that the
dynamical centre for Red Giant Branch (RGB) stars is similar to that seen for
the Carbon Stars, whereas for young stars the dynamical centre is significantly
offset from the older populations. This potentially indicates that the young
stars were formed as a consequence of a strong tidal interaction, probably with
the Small Magellanic Cloud (SMC). In terms of internal dynamics, the tangential
velocity profile increases linearly within $\sim3\ \mathrm{kpc}$, after which
it maintains an approximately constant value of $V_{rot} = 83.6\pm 1.7
\mathrm{km\ s^{-1}}$ until $\sim7 \mathrm{kpc}$. With an asymmetric drift
correction, we estimate the mass within $7 \mathrm{kpc}$ to be $M_{\rm
LMC}(<7\mathrm{kpc}) = (2.5\pm0.1)\times10^{10}\ \mathrm{M}_{\odot}$ and within
the tidal radius ($\sim 30\ \mathrm{kpc}$) to be $M_{\rm LMC}(<30\mathrm{kpc})
= (1.06 \pm 0.32)\times10^{11}\ \mathrm{M}_{\odot}$, consistent with other
recent measurements.
