Massive stars in the young cluster VVV CL074
  We obtained K-band spectroscopy of the brightest members of the cluster VVV
CL074 in order to identify the massive star population. We also determined the
stellar properties of the cluster's massive stars to better quantify the
evolutionary sequences linking different types of massive stars. We collected
integral field spectroscopy of selected fields in the cluster VVV CL074 with
SINFONI on the ESO/VLT. We performed a spectral classification based on the
K-band spectra and comparison to infrared spectral atlases. We determined the
stellar parameters of the massive stars from analysis with atmosphere models
computed with the code CMFGEN. We uncover a population of 25 early-type (OB and
Wolf-Rayet) stars, 19 being newly discovered by our observations out of which
15 are likely cluster members. The cluster's spectrophotometric distance is
10.2+/-1.6 kpc, placing it close to the intersection of the galactic bar and
the Norma arm, beyond the galactic center. This makes VVV CL074 one the
farthest young massive clusters identified so far. Among the massive stars
population, three objects are Wolf-Rayet stars, the remaining are O and B
stars. From the Hertzsprung-Russell diagram we find that most stars have an age
between 3 and 6 Myr according to the Geneva evolutionary tracks. WN8 and WC8-9
stars are the descendants of stars with initial masses between 40 and 60 Msun.
The massive star population of VVV CL074 is very similar to that of the cluster
DBS2003-179 and to a lesser extent to that of the Quintuplet cluster,
indicating the same age. The central cluster of the Galaxy is ~3 Myr older.
From the comparison of the massive stars populations in these four clusters,
one concludes that galactic stars with an initial mass in the range 40 to 60
Msun likely go through a WN8-9 phase.
