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The young star cluster NGC 602 and its associated HII region, N90, formed ina relatively isolated and diffuse environment in the Wing of the SmallMagellanic Cloud. Its isolation from other regions of massive star formationand the relatively simple surrounding HI shell structure allows us to constrainthe processes that may have led to its formation and to study conditionsleading to massive star formation. We use images from Hubble Space Telescopeand high resolution echelle spectrographic data from the Anglo-AustralianTelescope along with 21-cm neutral hydrogen (HI) spectrum survey data and theshell catalogue derived from it to establish a likely evolutionary scenarioleading to the formation of NGC 602. We identify a distinct HI cloud componentthat is likely the progenitor cloud of the cluster and HII region whichprobably formed in blister fashion from the cloud's periphery. We also findthat the past interaction of HI shells can explain the current location andradial velocity of the nebula. The surrounding Interstellar Medium is diffuseand dust-poor as demonstrated by a low visual optical depth throughout thenebula and an average HI density of the progenitor cloud estimated at 1 cm^-3.These conditions suggest that the NGC 602 star formation event was produced bycompression and turbulence associated with HI shell interactions. It thereforerepresents a single star forming event in a low gas density region.

NGC 602 Environment, Kinematics and Origins