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We study the multiple populations of $\omega$ Cen by using the abundances ofFe, C, N, O, Mg, Al, Si, K, Ca, and Ce from the high-resolution, highsignal-to-noise (S/N$>$70) spectra of 982 red giant stars observed by theSDSS-IV/APOGEE-2 survey. We find that the shape of the Al-Mg and N-Canticorrelations changes as a function of metallicity, continuous for themetal-poor groups, but bimodal (or unimodal) at high metallicities. There arefour Fe populations, similar to what has been found in previously publishedinvestigations, but we find seven populations based on Fe, Al, and Mgabundances. The evolution of Al in $\omega$ Cen is compared to its evolution inthe Milky Way and in five representative globular clusters. We find that thedistribution of Al in metal-rich stars of $\omega$ Cen closely follows what isobserved in the Galaxy. Other $\alpha-$elements and C, N, O, and Ce are alsocompared to the Milky Way, and significantly elevated abundances are observedover what is found in the thick disk for almost all elements. However, we alsofind some stars with high metallicity and low [Al/Fe], suggesting that $\omega$Cen could be the remnant core of a dwarf galaxy, but the existence of thesepeculiar stars needs an independent confirmation. We also confirm the increasein the sum of CNO as a function of metallicity previously reported in theliterature and find that the [C/N] ratio appears to show opposite correlationsbetween Al-poor and Al-rich stars as a function of metallicity.

Homogeneous Analysis of Globular Clusters from the APOGEE Survey with the BACCHUS Code $-$ III. $\omega$ Cen