Rotation and Hα Emission in a Young SMC Cluster: A Spectroscopic View of NGC 330

We present an analysis of high-resolution optical spectra recorded for 30 stars of the split extended main-sequence turnoff of the young (∼40 Myr) Small Magellanic Cloud globular cluster NGC 330. Spectra were obtained with the Michigan/Magellan Fiber System and Magellan Inamori Kyocera Echelle spectrographs located on the Magellan-Clay 6.5 m telescope. These spectra revealed the presence of Be stars, occupying primarily the cool side of the split main sequence. Rotational velocity ( $v\sin i$ ) measurements for most of the targets are consistent with the presence of two populations of stars in the cluster: one made up of rapidly rotating Be stars ( $\langle v\sin i\rangle \approx 200$ km s ^−1 ) and the other consisting of warmer stars with slower rotation ( $\langle v\sin i\rangle \approx 50$ km s ^−1 ). Core emission in the H δ photospheric lines was observed for most of the H α emitters. The shell parameter computed for the targets in our sample indicates that most of the observed stars should have inclinations below 75°. These results confirm the detection of Be stars obtained through photometry but also reveal the presence of narrow H α and H δ features for some targets that cannot be detected with low-resolution spectroscopy or photometry. Asymmetry variability of H α line profiles on the timescales of a few years is also observed and could provide information on the geometry of the decretion disks. Observations revealed the presence of nebular H α emission, strong enough in faint targets to compromise the extraction of spectra and to impact narrow-band photometry used to assess the presence of H α emission.