The Magellanic Bridge, stretching between the Small and the Large Magellanic Cloud (SMC and LMC), is the nearest tidally stripped intergalactic environment, with a significantly low average metallicity of one-tenth of solar. This Bridge of neutral hydrogen gas is associated with a young population that mainly consists of B-type or late stars. Recently we discovered three hot massive O binaries in the Magellanic Bridge using ESO VLT spectroscopy. Clear evidence for on-going star formation in the Bridge and tidally stripped galactic tails containing low-density dynamical gas are capable of producing massive O stars. We analyze the spectra of each star using the state-of-the-art stellar atmosphere models, which provide the physical parameters, ionizing photon fluxes, and surface abundances.see more details..
One of the largest structure in the Wing is the only one Hα “supergiant shell” (SGS) in the Small Magellanic Cloud (SMC), which also coincides with a H I supergiant shell. The Wing of the SMC has a lower content of gas, dust, allows us to investigate the influence of metallicity of the interstellar medium (ISM) on the role of star formation, stellar evolution and feedback. We observed the massive stars in the SMC-SGS 1 using the FLAMES multi-object spectrograph at ESO-VLT.see more details..
The giant H II region N 206 in the Large Magellanic Cloud (LMC) contains an OB association that powers a superbubble filled with hot X-ray emitting gas. We observed the massive stars in the N 206 complex using the multi-object spectrograph FLAMES at ESO’s Very Large Telescope (VLT). Available ultra-violet (UV) spectra from archives are also used. The spectral analysis is performed with Potsdam Wolf-Rayet (PoWR) model atmospheres by reproducing the observations with the synthetic spectra.see more details..