Stellar population of the superbubble N206 in the LMC II. Parameters of
  the OB and WR stars, and the total massive star feedback
  Clusters or associations of early-type stars are often associated with a
'superbubble' of hot gas. The formation of such superbubbles is caused by the
feedback from massive stars. The complex N206 in the Large Magellanic Cloud
exhibits a superbubble and a rich massive star population. We observed these
massive stars using the FLAMES multi-object spectrograph at ESO-VLT. Available
UV spectra from HST, IUE, and FUSE are also used. The spectral analysis is
performed with Potsdam Wolf-Rayet (PoWR) model atmospheres. We present the
stellar and wind parameters of the OB stars and the two WR binaries in the N206
complex. Twelve percent of the sample show Oe/Be type emission lines, although
most of them appear to rotate far below critical. We found eight runaway stars
based on their radial velocity. The wind-momentum luminosity relation of our OB
sample is consistent with the expectations. The HRD of the OB stars reveals a
large age spread (1-30 Myr), suggesting different episodes of star formation in
the complex. The youngest stars are concentrated in the inner part of the
complex, while the older OB stars are scattered over outer regions. We derived
the present day mass function for the entire N206 complex as well as for the
cluster NGC2018. Three very massive Of stars are found to dominate the feedback
among 164 OB stars in the sample. The two WR winds alone release about as much
mechanical luminosity as the whole OB star sample. The cumulative mechanical
feedback from all massive stellar winds is comparable to the combined
mechanical energy of the supernova explosions that likely occurred in the
complex. Accounting also for the WR wind and supernovae, the mechanical input
over the last five Myr is ~$2.3\times10^{52}$ erg, which exceeds the current
energy content of the complex by more than a factor of five. The morphology of
the complex suggests a leakage of hot gas from the superbubble.
