A revised view of the Canis Major stellar overdensity with DECam and
  Gaia: new evidence of a stellar warp of blue stars
  We present DECam imaging combined with Gaia DR2 data to study the Canis Major
overdensity. The presence of the so-called Blue Plume stars in a low-pollution
area of the color-magnitude diagram allows us to derive the distance and proper
motions of this stellar feature along the line of sight of its hypothetical
core. The stellar overdensity extends on a large area of the sky at low
Galactic latitudes, below the plane, and between 230$^\circ < \ell <
255^\circ$. According to the orbit derived for Canis Major, it presents an
on-plane rotation around the Milky Way. Moreover, additional overdensities of
Blue Plume stars are found around the plane and across the Galaxy, proving that
these objects are not only associated with that structure. The spatial
distribution of these stars, derived using Gaia astrometric data, confirms that
the detection of the Canis Major overdensity results more from the warped
structure of the Milky Way disk than from the accretion of a dwarf galaxy.
