  We explore the kinematic and chemical properties of Monoceros stellar
overdensity by combining data from 2MASS, WISE, APOGEE, and $\text{Gaia}$.
Monoceros is a structure located towards the Galactic anticenter and close to
the disk. We identified that its stars have azimuthal velocity in the range of
$200 < v_{\phi}\,{\rm(km\,s^{-1})}< 250$. Combining their kinematics and
spatial distribution, we designed a new method to select stars from this
overdensity. This method allows us to easily identify the structure in both
hemispheres and estimate their distances. Our analysis was supported by
comparison with simulated data from the entire sky generated by
$\texttt{Galaxia}$ code. Furthermore, we characterized, for the first time, the
Monoceros overdensity in several chemical-abundance spaces. Our results confirm
its similarity to stars found in the thin disk of the Galaxy and suggest an
$\textit{in situ}$ formation. Furthermore, we demonstrate that the southern
(Mon-S) and northern (Mon-N) regions of Monoceros exhibit indistinguishable
chemical compositions.
