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Understanding the evolutionary history of the Magellanic Clouds requires anin-depth exploration and characterization of the stellar content in their outerregions, which ultimately are key to tracing the epochs and nature of pastinteractions. We present new deep images of a shell-like over-density of starsin the outskirts of the Small Magellanic Cloud (SMC). The shell, also detectedin photographic plates dating back to the fifties, is located at ~1.9 degr fromthe center of the SMC in the north-east direction.The structure and stellarcontent of this feature were studied with multi-band, optical data from theSurvey of the MAgellanic Stellar History (SMASH) carried out with the DarkEnergy Camera on the Blanco Telescope at Cerro Tololo Inter-AmericanObservatory. We also investigate the kinematic of the stars in the shell usingthe Gaia Data Release 2. The shell is composed of a young population with anage ~ 150 Myr, with no contribution from an old population. Thus, it is hard toexplain its origin as the remnant of a tidally disrupted stellar system. Thespatial distribution of the young main-sequence stars shows a richsub-structure, with a spiral arm-like feature emanating from the main shell anda separated small arc of young stars close to the globular cluster NGC 362. Wefind that the absolute g-band magnitude of the shell is M_{g,shell} = -10.78+/-0.02, with a surface brightness of mu_{g,shell} = 25.81+/- 0.01 mag/arcsec^{2}.We have not found any evidence that this feature is of tidal origin or a brightpart of a spiral arm-like structure. Instead, we suggest that the shell formedin a recent star formation event, likely triggered by an interaction with theLarge Magellanic Cloud and/or the Milky Way, ~150 Myr ago.

On the nature of a shell of young stars in the outskirts of the Small Magellanic Cloud