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The supergiant ionized shell SMC-SGS 1 (DEM 167), located in the outer Wingof the Small Magellanic Cloud (SMC), resembles structures that originate froman energetic star-formation event and later stimulate star formation as theyexpand into the ambient medium. However, stellar populations within andsurrounding SMC-SGS 1 tell a different story. We present a photometric study ofthe stellar population encompassed by SMC-SGS 1 in order to trace the historyof this structure and its potential influence on star formation within thelow-density, low-metallicity SMC Wing. For a stellar population that isphysically associated with SMC-SGS 1, we combined near-ultraviolet (NUV)photometry from the Galaxy Evolution Explorer (GALEX) with archival optical(V-band) photometry from the ESO Danish 1.54m Telescope. Given their colors andluminosities, we estimated stellar ages and masses by matching observedphotometry to theoretical stellar isochrone models. We find that theinvestigated region supports an active, extended star-formation event spanning$\sim$ 25 - 40 Myr ago, as well as continued star formation into the present.Using a standard initial mass function (IMF), we infer a lower bound on thestellar mass from this period of $\sim 3 \times 10^4 M_{\odot}$, correspondingto a star-formation intensity of $\sim$ 6 $\times$ 10$^{-3}$ M$_{\odot}$kpc$^{-2}$ yr$^{-1}$. The spatial and temporal distributions of young starsencompassed by SMC-SGS 1 imply a slow, consistent progression of star formationover millions of years. Ongoing star formation along the edge of and interiorto SMC-SGS 1 suggests a combined stimulated and stochastic mode of starformation within the SMC Wing. A slow expansion of the shell within thislow-density environment may preserve molecular clouds within the volume of theshell, leaving them to form stars even after nearby stellar feedback expelslocal gas and dust.

Testing massive star evolution, star-formation history, and feedback at low metallicity: Photometric analysis of OB stars in the SMC Wing