Obscured clusters IV. The most massive stars in [DBS2003] 179

Aims. We report new results for the massive evolved and main sequence members of the young galactic cluster DBS2003 179. We determine the physical parameters and investigate the high-mass stellar content of the cluster, as well as of its close vicinity. Methods. Our analysis is based on ISAAC/VLT moderate-resolution (R approximate to 4000) infrared spectroscopy of the brightest cluster members. We derive stellar parameters for sixteen of the stellar members, using full non-local thermodynamic equilibrium modeling of the obtained spectra. Results. The cluster contains three late WN or WR/LBV stars (Obj 4, Obj 15, and Obj 20: MDM32) and at least five OIf and five OV stars. According to the Hertzsprung-Russell diagram for DBS2003 179, the WR stars show masses above 85M(circle dot), the OIf stars are between 40 and 80M(circle dot), and the main sequence O stars are >20 M-circle dot. There are indications of binarity for Obj 4 and Obj 11, and Obj 3 shows a variable spectrum. The cluster is surrounded by a continuous protostar formation region most probably triggered by DBS2003 179. Conclusions. We confirm that DBS2003 179 is young massive cluster (2.5 x 10(4) M-circle dot) very close to the Galactic center at the distance of 7.9 +/- 0.8 kpc.