Spectroscopy of Star Cluster Candidates and H [CSC]ii[/CSC] Regions in NGC 6822

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Abstract
We present optical spectroscopy of four star clusters and six H II regions in the nearby, dwarf irregular galaxy NGC 6822. From the data, we estimate ages of 2.5 × 107, 2.0 × 108, 1.4 × 109, and 10 ± 2 × 109 yr for clusters H VI, C21, H VIII, and H VII, respectively. For clusters H VI and H VII we estimate [Fe/H] ≈ -1.46 ± 0.26 and ~-2.0, lower than Large and Small Magellanic Cloud clusters at similar ages. Mass estimates for H VI, H VII, and H VIII demonstrate that clusters with typical globular cluster masses (>104 M⊙) have formed over the lifetime of NGC 6822. For six H II regions, ionic abundances are derived for element species of N, O, S, and Ne. These show that there is a correlation of abundance with position, the highest oxygen abundance H II regions being located off the main body of the galaxy.

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