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A Survey of X-ray Point Sources in the Magellanic Clouds

Published online by Cambridge University Press:  25 May 2016

A. P. Cowley ,
P. C. Schmidtke ,
V. A. Taylor ,
T.K. McGrath ,
J. B. Hutchings  and
D. Crampton
A. P. Cowley
Affiliation:
Dept. of Physics & Astronomy, Arizona State University, Tempe, AZ 85287-1504
P. C. Schmidtke
Affiliation:
Dept. of Physics & Astronomy, Arizona State University, Tempe, AZ 85287-1504
V. A. Taylor
Affiliation:
Dept. of Physics & Astronomy, Arizona State University, Tempe, AZ 85287-1504
T.K. McGrath
Affiliation:
Dept. of Physics & Astronomy, Arizona State University, Tempe, AZ 85287-1504
J. B. Hutchings
Affiliation:
Dominion Astrophysical Observatory, HIA/NRC, Victoria BC, V8X 4M6 Canada
D. Crampton
Affiliation:
Dominion Astrophysical Observatory, HIA/NRC, Victoria BC, V8X 4M6 Canada

Abstract

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In this study we compare the global populations of stellar X-ray sources in the LMC, SMC, and the Galaxy. After removing foreground stars and background AGN from the samples, the relative numbers of the various types of X-ray point sources within the LMC and SMC are similar, but differ markedly from those in the Galaxy. The Magellanic Clouds are rich in high-mass X-ray binaries (HMXB), especially those containing rapidly rotating Be stars. However, the LMC and SMC both lack the large number of low-mass X-ray binaries (LMXB) found in the Milky Way, which are known to represent a very old stellar population based on their kinematics, chemical composition, and spatial distribution.

Type
Part 2: The Database
Information
Symposium - International Astronomical Union , Volume 192: The Stellar Content of Local Group Galaxies , 1999 , pp. 100 - 103
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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