  Previous results in the literature have found the young inner-disk open
cluster NGC 6705 to be mildly $\alpha$-enhanced. We examined this possibility
via an independent chemical abundance analysis for 11 red-giant members of NGC
6705. The analysis is based on near-infrared APOGEE spectra and relies on LTE
calculations using spherical model atmospheres and radiative transfer. We find
a mean cluster metallicity of $\rm [Fe/H] = +0.13 \pm 0.04$, indicating that
NGC 6705 is metal-rich, as may be expected for a young inner-disk cluster. The
mean $\alpha$-element abundance relative to iron is $\rm \langle
[\alpha/Fe]\rangle =-0.03 \pm 0.05$, which is not at odds with expectations
from general Galactic abundance trends. NGC 6705 also provides important probes
for studying stellar mixing, given its turn-off mass of M$\sim$3.3 M$_\odot$.
Its red giants have low $^{12}$C abundances ([$^{12}$C/Fe]=$-$0.16) and
enhanced $^{14}$N abundances ([$^{14}$N/Fe]=+0.51), which are key signatures of
the first dredge-up on the red giant branch. An additional signature of
dredge-up was found in the Na abundances, which are enhanced by [Na/Fe]=+0.29,
with a very small non-LTE correction. The $^{16}$O and Al abundances are found
to be near-solar. All of the derived mixing-sensitive abundances are in
agreement with stellar models of approximately 3.3 M$_{\odot}$ evolving along
the red giant branch and onto the red clump. As found in young open clusters
with similar metallicities, NGC 6705 exhibits a mild excess in the s-process
element cerium, with $\rm [Ce/Fe] = +0.13\pm0.07$.
