The LMC geometry and outer stellar populations from early DES data
  The Dark Energy Camera has captured a large set of images as part of Science
Verification (SV) for the Dark Energy Survey. The SV footprint covers a lar ge
portion of the outer Large Magellanic Cloud (LMC), providing photometry 1.5
magnitudes fainter than the main sequence turn-off of the oldest LMC stel lar
population. We derive geometrical and structural parameters for various stellar
populations in the LMC disk. For the distribution of all LMC stars, we find an
inclination of $i=-38.14^{\circ}\pm0.08^{\circ}$ (near side in the North) and a
position angle for the line of nodes of
$\theta_0=129.51^{\circ}\pm0.17^{\circ}$. We find that stars younger than $\sim
4$ Gyr are more centrally concentrated than older stars. Fitting a projected
exponential disk shows that the scale radius of the old populations is $R_{>4
Gyr}=1.41\pm0.01$ kpc, while the younger population has $R_{<4
Gyr}=0.72\pm0.01$ kpc. Howe ver, the spatial distribution of the younger
population deviates significantly from the projected exponential disk model.
The distribution of old stars suggests a large truncation radius of
$R_{t}=13.5\pm0.8$ kpc. If this truncation is dominated by the tidal field of
the Galaxy, we find that the LMC is $\simeq 24^{+9}_{-6}$ times less massive
than the encircled Galactic mass. By measuring the Red Clump peak magnitude and
comparing with the best-fit LM C disk model, we find that the LMC disk is
warped and thicker in the outer regions north of the LMC centre. Our findings
may either be interpreted as a warped and flared disk in the LMC outskirts, or
as evidence of a spheroidal halo component
