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We investigate the star formation activity in a young star forming clusterembedded at the edge of the RCW 41 HII region. As a complementary goal, we aimat demonstrating the gain provided by Wide-Field Adaptive Optics instruments tostudy young clusters. We used deep, JHKs images from the newly commissionedGemini-GeMS/GSAOI instrument, complemented with Spitzer IRAC observations, inorder to study the photometric properties of the young stellar cluster. GeMS isan AO instrument, delivering almost diffraction limited images over a field of2' across. The exquisite angular resolution allows us to reach a limitingmagnitude of J = 22 for 98% completeness. The combination of the IRACphotometry with our JHKs catalog is used to build color-color diagrams, andselect Young Stellar Objects (YSOs) candidates. We detect the presence of 80Young Stellar Object (YSO) candidates. Those YSOs are used to infer the clusterage, which is found to be in the range 1 to 5 Myr. We find that 1/3 of the YSOsare in a range between 3 to 5 Myr, while 2/3 of the YSO are < 3 Myr. Whenlooking at the spatial distribution of these two populations, we evidence apotential age gradient across the field, suggesting sequential star formation.We construct the IMF, and show that we can sample the mass distribution wellinto the brown dwarf regime (down to 0.01 Msun). The logarithmic mass functionrises to peak at 0.3 Msun, before turning over and declining into the browndwarf regime. The total cluster mass derived is estimated to be 78 +/- 18 Msun,while the ratio of brown dwarfs to star derived is 18 p/- 5 %. When comparingwith other young clusters, we find that the IMF shape of the young clusterembedded within RCW 41 is consistent with those of Trapezium, IC 348 orChamaeleon I, except for the IMF peak, which happens to be at higher mass. Thischaracteristic is also seen in clusters like NGC 6611 or even Taurus.

Deep near-infrared adaptive optics observations of a young embedded cluster at the edge of the RCW 41 HII region