Abstract
Context. Young massive clusters are usually deeply embedded in dust and gas. They represent excellent astrophysical laboratories for the study of massive stars. Clusters with Wolf-Rayet (WR) stars are of special importance, since this enables us to study a coeval WR population at a uniform metallicity and known age. Aims. We started a long-term project to search the inner Milky Way for hidden star clusters and to study them in detail. GLIMPSE 30 (G30) is one of these clusters. It is situated near the Galactic plane (l = 298. ◦ 756, b = −0. 408) and we determine its physical parameters and investigate its high-mass stellar content especially WR stars. Methods. Our analysis is based on SOFI/NTT JSHKS imaging and low resolution (R ∼ 2000) spectroscopy of the brightest cluster members in the K atmospheric window. For the age determination we applied isochrone fits for MS and Pre-MS stars. We derived stellar parameters of the WR stars candidates using a full nonLTE modeling of the observed spectra. Results. Using a variety of techniques we found that G30 is very young cluster, with age t ≈ 4 Myr. The cluster is located in the Carina spiral arm, it is deeply embedded in dust and suffers reddening of AV ∼ 10.5 ± 1.1 mag. The distance to the object is d = 7.2 ± 0.9 kpc. ?
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