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Some of the Wolf-Rayet stars are found to have very high bolometricluminosities (more than 1 solar). We employ the Potsdam Wolf-Rayet (PoWR)model atmospheres for their spectral analysis, which yields the bolometriccorrections. Distance and interstellar reddening also enter the luminosityestimates. Among the Galactic stars, there is a group of very luminous WNLstars (i.e. WR stars of late subtype from nitrogen sequence with hydrogen beingdepleted in their atmospheres, but not absent). Their distances are often themajor source of uncertainty. From K-band spectroscopy we found a very luminousstar ($\log L/L_\odot = 6.5$) in the Galactic center region, which we termedthe Peony Star because of the form of its surrounding dusty nebula. A similargroup of very luminous WNL stars is found in the Large Magellanic Cloud (LMC).In the Small Magellanic Cloud (SMC) the majority of WR stars resides in binarysystems. The single WNL stars in the SMC are not very luminous. We concludethat a significant number of very luminous WNL stars exist in the Galaxy andthe LMC. With initial masses above 60$M_\odot$, they apparently evolveddirectly to the WNL stage without a prior excursion to the red side of the HRD.At the low metallicity of the SMC, the binary channel may be dominant for theformation of WR stars.

The most luminous stars in the Galaxy and the Magellanic Clouds