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Searching for Wolf-Rayet Stars in M101

Published online by Cambridge University Press:  05 September 2012

J. L. Bibby
Affiliation:
Dept. of Astrophysics, American Museum of Natural HistoryCentral ParkWest @ 79th St, New York, NY 10024, USA email: [email protected]
P. A. Crowther
Affiliation:
Dept. of Physics & Astronomy, University of Sheffield, Hounsfield Rd, Sheffield, S3 7RH, UK
A. F. J. Moffat
Affiliation:
Dépt. de physique, Université de Montréal, C.P. 6128, Succursale Centre-Ville, Montréal, QC, H3C 3J7, Canada
M. M. Shara
Affiliation:
Dept. of Astrophysics, American Museum of Natural HistoryCentral ParkWest @ 79th St, New York, NY 10024, USA email: [email protected]
D. Zurek
Affiliation:
Dept. of Astrophysics, American Museum of Natural HistoryCentral ParkWest @ 79th St, New York, NY 10024, USA email: [email protected]
L. Drissen
Affiliation:
Dépt. de physique, Université de Montréal, C.P. 6128, Succursale Centre-Ville, Montréal, QC, H3C 3J7, Canada
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Abstract

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Wolf-Rayet (WR) stars are the evolved descendants of massive O-type stars and are considered to be progenitor candidates for Type Ib/c core-collapse supernovae (SNe). Recent results of our HST/WFC3 survey of Wolf-Rayet stars in M101 are summarised based on the detection efficiency of narrow-band optical imaging compared to broad-band methods. We show that on average 42% of WR stars, increasing to ~85% in central regions, are only detected in the narrow-band imaging. Hence, the non-detection of a WR star at the location of ~10 Type Ib/c SNe in broad-band imaging is no longer strong evidence for a non-WR progenitor channel.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2012

References

Bibby, J. L. & Crowther, P. A. 2012, MNRAS, 420, 3091CrossRefGoogle Scholar
Bibby, J. L. & Crowther, P. A. 2010, MNRAS, 405, 2737Google Scholar
Crowther, P. A. 2007, ARA&A, 54, 177Google Scholar
Crowther, P. A. & Hadfield, L. J. 2006, A&A, 449, 895Google Scholar
Lee, J. C., Gil de Paz, A., Tremonti, C., Kennicutt, R. C. Jr., Salim, S., Bothwell, M., Calzetti, D., Dalcanton, J., et al. 2009, ApJ, 706, 599CrossRefGoogle Scholar
Moffat, A. F. J. & Shara, M. M. 1983, ApJ, 273, 544CrossRefGoogle Scholar
Shappee, B. J. & Stanek, K. Z. 2011, ApJ, 733, 124CrossRefGoogle Scholar
Smartt, S. J. 2009, ARA&A, 47, 63Google Scholar