Characterizing Wolf-Rayet Stars in the Near and Mid Infrared
  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 2MASS. Using a sample of spectrally classified objects, we find that WR stars are well distinguished from the field stellar population in the (W1-W2) vs. (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 micron 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 micron spectral region, although their strength is greatly diminished compared to the 0.8-2.5 micron 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 Wolf Rayet stars show evidence of circumstellar shells linked to mass ejections from strong stellar winds. 
Jacqueline K. Faherty, Michael M. Shara, David Zurek, Graham Kanarek,   Anthony F. J. Moffat
astro-ph.SR