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Massive Stars in M31

Published online by Cambridge University Press:  28 July 2017

Jamie R. Lomax
Affiliation:
Department of Astronomy, University of Washington Box 351580, Seattle, WA 98195, USA
Matthew Peters
Affiliation:
Homer L. Dodge Department of Physics & Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA
John Wisniewski
Affiliation:
Homer L. Dodge Department of Physics & Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA
Julianne Dalcanton
Affiliation:
Department of Astronomy, University of Washington Box 351580, Seattle, WA 98195, USA
Benjamin Williams
Affiliation:
Department of Astronomy, University of Washington Box 351580, Seattle, WA 98195, USA
Julie Lutz
Affiliation:
Department of Astronomy, University of Washington Box 351580, Seattle, WA 98195, USA
Yumi Choi
Affiliation:
Steward Observatory, University of Arizona, Tucson, AZ 85721, USA
Aaron Sigut
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario Canada N6A 3K7
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Abstract

Massive stars are intrinsically rare and therefore present a challenge to understand from a statistical perspective, especially within the Milky Way. We recently conducted follow-up observations to the Panchromatic Hubble Andromeda Treasury (PHAT) survey that were designed to detect more than 10,000 emission line stars, including WRs, by targeting regions in M31 previously known to host large numbers of young, massive clusters and very young stellar populations. Because of the existing PHAT data, we are able to derive an effective temperature, bolarimetric luminosity, and extinction for each of our detected stars. We report on preliminary results of the massive star population of our dataset and discuss how our results compare to previous studies of massive stars in M31.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

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