Context : 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 N 206 in the Large Magellanic Cloud exhibits a superbubble and a rich massive star population .

Aims : Our goal is to perform quantitative spectral analyses of all massive stars associated with the N 206 superbubble in order to determine their stellar and wind parameters .
We compare the superbubble energy budget to the stellar energy input and discuss the star formation history of the region .

Methods : 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 .

Results : We present the stellar and wind parameters of the OB stars and the two Wolf-Rayet ( WR ) binaries in the N 206 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 Hertzsprung-Russell diagram ( 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 N 206 complex as well as for the cluster NGC 2018 .
The total ionizing photon flux produced by all massive stars in the N 206 complex is Q _ { 0 } \approx 5 \times 10 ^ { 50 } { s ^ { -1 } } , and the mechanical luminosity of their stellar winds amounts to L _ { mec } = 1.7 \times 10 ^ { 38 } { erg s ^ { -1 } } .
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 \approx 2.3 \times 10 ^ { 52 } erg .

Conclusions : The N206 complex in the LMC has undergone star formation episodes since more than 30 Myr ago .
From the spectral analyses of its massive star population , we derive a current star formation rate of 2.2 \times 10 ^ { -3 } M _ { \odot } \mathrm { yr } ^ { -1 } .
From the combined input of mechanical energy from all stellar winds , only a minor fraction is emitted in the form of X-rays .
The corresponding input accumulated over a long time also 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 .