Exploring the Galactic Anticenter substructure with LAMOST & Gaia DR2
  We characterize the kinematic and chemical properties of 589 Galactic
Anticenter Substructure Stars (GASS) with K-/M- giants in Integrals-of-Motion
space. These stars likely include members of previously identified
substructures such as Monoceros, A13, and the Triangulum-Andromeda cloud
(TriAnd). We show that these stars are on nearly circular orbits on both sides
of the Galactic plane. We can see velocity($V_{Z}$) gradient along Y-axis
especially for the south GASS members. Our GASS members have similar energy and
angular momentum distributions to thin disk stars. Their location in
[$\alpha$/M] vs. [M/H] space is more metal poor than typical thin disk stars,
with [$\alpha$/M] \textbf{lower} than the thick disk. We infer that our GASS
members are part of the outer metal-poor disk stars, and the outer-disk extends
to 30 kpc. Considering the distance range and $\alpha$-abundance features, GASS
could be formed after the thick disk was formed due to the molecular cloud
density decreased in the outer disk where the SFR might be less efficient than
the inner disk.
