  IC 166 is an intermediate-age open cluster ($\sim 1$ Gyr) which lies in the
transition zone of the metallicity gradient in the outer disc. Its location,
combined with our very limited knowledge of its salient features, make it an
interesting object of study. We present the first high-resolution spectroscopic
and precise kinematical analysis of IC 166, which lies in the outer disc with
$R_{GC} \sim 12.7$ kpc. High resolution \textit{H}-band spectra were analyzed
using observations from the SDSS-IV Apache Point Observatory Galactic Evolution
Experiment (APOGEE) survey. We made use of the Brussels Automatic Stellar
Parameter (BACCHUS) code to provide chemical abundances based on a line-by-line
approach for up to eight chemical elements (Mg, Si, Ca, Ti, Al, K, Mn and Fe).
The $\alpha-$element (Mg, Si, Ca and whenever available Ti) abundances, and
their trends with Fe abundances have been analysed for a total of 13
high-likelihood cluster members. No significant abundance scatter was found in
any of the chemical species studied. Combining the positional, heliocentric
distance, and kinematic information we derive, for the first time, the probable
orbit of IC 166 within a Galactic model including a rotating boxy bar, and
found that it is likely that IC 166 formed in the Galactic disc, supporting its
nature as an unremarkable Galactic open cluster with an orbit bound to the
Galactic plane.
