  We present detailed elemental abundances and radial velocities of stars in
the metal-poor globular cluster (GC) NGC 2298, based on near-infrared
high-resolution ($R\sim$ 22,500) spectra of twelve members obtained during the
second phase of the Apache Point Observatory Galactic Evolution Experiment
(APOGEE-2) at Las Campanas Observatory as part of the seventeenth Data Release
(DR 17) of the Sloan Digital Sky Survey IV (SDSS-IV). We employ the Brussels
Automatic Code for Characterizing High accuracy Spectra (\texttt{BACCHUS})
software to investigate abundances for a variety of species including
$\alpha$-elements (Mg, Si, and Ca), the odd-Z element Al, and iron-peak
elements (Fe and Ni) located in the innermost regions of NGC 2298. We find a
mean and median metallicity [Fe/H] $ = -1.76$ and $-1.75$, respectively, with a
star-to-star spread of 0.14 dex, compatible with the internal measurement
errors. Thus, we find no evidence for an intrinsic Fe abundance spread in NGC
2298. The typical $\alpha-$element enrichment in NGC 2298 is overabundant
relative to the Sun, and follows the trend of other metal-poor GCs. We confirm
the existence of an Al-enhanced population in this cluster, which is clearly
anti-correlated with Mg, indicating the prevalence of the multiple-population
phenomenon in NGC 2298.
