SIMBAD references

2014AJ....147..115F - Astron. J., 147, 115 (2014/May-0)

Characterizing Wolf-Rayet stars in the near- and mid-infrared.


Abstract (from CDS):

We present refined color-color selection criteria for identifying Wolf-Rayet (WR) stars using available mid-infrared (MIR) photometry from WISE in combination with near-infrared (NIR) photometry from the Two Micron All Sky Survey. Using a sample of spectrally classified objects, we find that WR stars are well distinguished from the field stellar population in the (W1 - W2) versus (J - Ks) color-color diagram, and further distinguished from other emission line objects such as planetary nebulae, Be, and cataclysmic variable stars using a combination of NIR and MIR color constraints. As proof of concept we applied the color constraints to a photometric sample in the Galactic plane, located WR star candidates, and present five new spectrally confirmed and classified WC (1) and WN (4) stars. Analysis of the 0.8-5.0 µm spectral data for a subset of known, bright WC and WN stars shows that emission lines (primarily He I) extend into the 3.0-5.0 µm spectral region, although their strength is greatly diminished compared to the 0.8-2.5 µm region. The WR population stands out relative to background field stars at NIR and MIR colors due to an excess continuum contribution, likely caused by free-free scattering in dense winds. Mean photometric properties of known WRs are presented and imply that reddened late-type WN and WC sources are easier to detect than earlier-type sources at larger Galactic radii. WISE W3 and W4 images of 10 WR stars show evidence of circumstellar shells linked to mass ejections from strong stellar winds.

Abstract Copyright:

Journal keyword(s): Galaxy: disk - Galaxy: stellar content - planetary nebulae: general - stars: emission-line, Be - stars: Wolf-Rayet - surveys

Nomenclature: Table 5: [FSZ2014] WR1343-193E N=1, [FSZ2014] WRNNNN-ANN N=3, [FSZ2014] WR1361-1583 N=1, [FSZ2014] WR1327-14AF N=1, [FSZ2014] WR1373-1FBA N=1.

Simbad objects: 28

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