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Massive stars are the key agents of feedback. Consequently, quantitativeanalysis of massive stars are required to understand how the feedback of theseobjects shapes/ creates the large scale structures of the ISM. The giant HIIregion N206 in the Large Magellanic Cloud contains an OB association thatpowers a X-ray superbubble, serving as an ideal laboratory in this context. Weobtained optical spectra with the muti-object spectrograph FLAMES at theESO-VLT. When possible, the optical spectroscopy was complemented by UV spectrafrom the HST, IUE, and FUSE archives. Detailed spectral classifications arepresented for our sample Of-type stars. For the quantitative spectroscopicanalysis we use the Potsdam Wolf-Rayet (PoWR) model atmosphere code. Thephysical parameters and nitrogen abundances of our sample stars are determinedby fitting synthetic spectra to the observations. The stellar and windparameters of nine Of-type stars are used to construct wind momentum,luminosityrelationship. We find that our sample follows a relation close to thetheoretical prediction, assuming clumped winds. The most massive star in theN206 association is an Of supergiant which has a very high mass-loss rate. Twoobjects in our sample reveal composite spectra, showing that the Of primarieshave companions of late O subtype. All stars in our sample have an evolutionaryage less than 4 million years, with the O2-type star being the youngest. Allthese stars show a systematic discrepancy between evolutionary andspectroscopic masses. All stars in our sample are nitrogen enriched. Nitrogenenrichment shows a clear correlation with increasing projected rotationalvelocities. The mechanical energy input from the Of stars alone is comparableto the energy stored in the N206 superbubble as measured from the observedX-ray and H alpha emission.

Stellar population of the superbubble N206 in the LMC I. Analysis of the Of-type stars