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

  title={Spatial distribution of Galactic Wolf-Rayet stars and implications for the global population},
  author={C. Rosslowe and P. Crowther},
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
Unlocking Galactic Wolf–Rayet stars with Gaia DR2 – II. Cluster and association membership
Galactic Wolf-Rayet (WR) star membership of star forming regions can be used to constrain the formation environments of massive stars. Here, we utilise $\textit{Gaia}$ DR2 parallaxes and properExpand
Evolutionary map of the Universe (EMU): Compact radio sources in the scorpio field towards the galactic plane
We present observations of a region of the Galactic plane taken during the Early Science Program of the Australian Square Kilometre Array Pathfinder (ASKAP). In this context, we observed the ScorpioExpand
Carina High-contrast Imaging Project for massive Stars (CHIPS)
Context. Massive stars like company. However, low-mass companions have remained extremely difficult to detect at angular separations (ρ) smaller than 1′′ (approx. 1000–3000 au, considering theExpand
X-ray emission from BH+O star binaries expected to descend from the observed galactic WR+O binaries
In the Milky Way, $\sim$18 Wolf-Rayet+O (WR+O) binaries are known with estimates of their stellar and orbital parameters. Whereas black hole+O (BH+O) binaries are thought to evolve from the former,Expand
Binary fraction indicators in resolved stellar populations and supernova-type ratios
The binary fraction of a stellar population can have pronounced effects on its properties, and in particular the number counts of different massive star types, and the relative subtype rates of theExpand
Estimating the core compactness of massive stars with Galactic supernova neutrinos
We suggest the future detection of neutrinos from a Galactic core-collapse supernova can be used to infer the progenitor's inner mass density structure. We present the results from 20 axisymmetricExpand
Analysis of physical processes in eruptive YSOs with near-infrared spectra and multiwavelength light curves
The decade-long Vista Variables in the Via Lactea (VVV) survey has detected numerous highly variable young stellar objects (YSOs). We present a study of 61 highly variable VVV YSOs (ΔKs = 1–5 mag),Expand
Hunting for Dark Matter and New Physics with (a) GECCO
We outline the science opportunities in the areas of searches for dark matter and new physics offered by a proposed future MeV gamma-ray telescope, the Galactic Explorer with a Coded Aperture MaskExpand
Grown-up stars physics with MATISSE
MATISSE represents a great opportunity to image the environment around massive and evolved stars. This will allow one to put constraints on the circumstellar structure, on the mass ejection of dustExpand
A New Transition Wolf–Rayet WN/C Star in the Milky Way
We report the discovery of a new transition type Wolf-Rayet (WR) WN/C star in the Galaxy. According to its coordinates (R.A., Dec)J2000 = 18h51m39.7s, -05d34m51.1s, and the distance (7.11 kpc awayExpand


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