Spatial distribution of Galactic Wolf-Rayet stars and implications for the global population

@inproceedings{Rosslowe2014SpatialDO,
  title={Spatial distribution of Galactic Wolf-Rayet stars and implications for the global population},
  author={C. Rosslowe and P. Crowther},
  year={2014}
}
We construct revised near-infrared absolute magnitude calibrations for 126 Galactic Wolf-Rayet (WR) stars at known distances, based in part upon recent large scale spectroscopic surveys. Application to 246 WR stars located in the field, permits us to map their galactic distribution. As anticipated, WR stars generally lie in the thin disk (∼40 pc half width at half maximum) between galactocentric radii 3.5–10 kpc, in accordance with other star formation tracers. We highlight 12 WR stars located… Expand
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References

SHOWING 1-7 OF 7 REFERENCES
Located only ∼2.3 from the Danks 1 cluster, WR48–4 is the faintest WR star located within G305
  • Mauerhan et al
  • 2011
WR stars discovered since the van der Hucht (2006) updated catalogue (up to March 2014). Distances are indicated for the stars that feature in this study
  • WR Alias
  • 2014
2013), and are converging on 8 kpc. Acknowledging the spread in measurements that still remains, we assume a distance of 8.0± 0.25kpc for these three clusters
  • 2013
giving a distance of 7.9±
  • 2009
giving a distance of 7.9±
  • 2009
2005), we see that best agreement with the isochrones is found at a distance modulus of 11.5±
  • 2005
b)P.A. Crowther, (priv
  • Vreux
  • 1990