THE YOUNG INTERCLOUD POPULATION - I - DISTANCES AND AGES

Deep BV CCD photometry has been used to characterize the properties of the young stellar population in the outer Small Magellanic Cloud (SMC ) wing and in the bridge between the Magellanic Clouds. Our observatio ns include targets that have not been previously observed and reach 2 mag fainter than data presented in a recent article by Grondin et al. They permit us to determine simultaneously, for an assumed abundance, the color excess and the distance of each association. Distances decre ase from west to east and are compatible with a stellar bridge stretch ing from the SMC wing to the Large Magellanic Cloud. We confirm earlie r findings that two associations, close in the sky, are indeed at a di stance of similar to 5 kpc apart along the line of sight. The ages of the observed main sequences indicate that a burst of star formation oc curred between 10 and 25 Myr ago. The star formation started earlier i n the SMC Ring, where evolved main-sequence stars of some 60 Myr are s een. No age gradient is seen across the 10 kpc bridge. Magnitude and c olor of many more bright main-sequence stars would be needed to better define the turnoffs and to determine ages more reliably.