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The massive Wolf-Rayet type star WR 102c is located near the QuintupletCluster - one of the three massive star clusters in the Galactic Center region.Previous studies indicated that WR 102c may have a dusty circumstellar nebulaand is among the main ionizing sources of the Sickle Nebula associated with theQuintuplet cluster. We obtained observations with the ESO's VLT integral fieldspectrograph SINFONI in the K-band, extracted the stellar spectra, and analyzedthem by means of stellar atmosphere models. Our new analysis supersedes theresults reported for WR 102c previously. We significantly revise down itsbolometric luminosity and hydrogen content. We detect four early OB type starsclose to WR 102c. These stars have radial velocities similar to that of WR102c. We suggest that together with WR 102c these stars belong to a distinctstar cluster with a total mass of about 1000 M_sun. We identify a new WR nebulaaround WR 102c in the SINFONI map of the diffuse Br$\gamma$ emission and in theHST's Pa$\alpha$ images. The Br$\gamma$ line at different locations is notsignificantly broadened and similar to the width of nebular emission elsewherein the H II region around WR 102c. The massive star WR 102c located in theGalactic Center region resides in a star cluster containing further early typestars. The stellar parameters of WR 102c are typical for hydrogen-free WN6stars. We newly identify a nebula surrounding WR 102c that has a morphologysimilar to other nebulae around hydrogen-free WR stars, and propose that theformation of this nebula is linked to interaction of the fast stellar wind withthe matter ejected at previous evolutionary stage of WR 102c.

Analysis of the WN star WR 102c, its WR nebula, and the associated cluster of massive stars in the Sickle Nebula