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The X-ray binary populations of M81 and M82

Published online by Cambridge University Press:  30 December 2019

Paul H. Sell Open the ORCID record for Paul H. Sell [Opens in a new window] ,
Andreas Zezas ,
Stephen J. Williams ,
Jeff J. Andrews Open the ORCID record for Jeff J. Andrews [Opens in a new window] ,
Kosmas Gazeas ,
John S. Gallagher  and
Andrew Ptak
Paul H. Sell
Affiliation:
Department of Physics, University of Crete, Heraklion, Greece email: [email protected] Foundation for Research and Technology Hellas (FORTH), Heraklion, Greece
Andreas Zezas
Affiliation:
Department of Physics, University of Crete, Heraklion, Greece email: [email protected] Foundation for Research and Technology Hellas (FORTH), Heraklion, Greece
Stephen J. Williams
Affiliation:
Department of Physics, University of Crete, Heraklion, Greece email: [email protected] Foundation for Research and Technology Hellas (FORTH), Heraklion, Greece
Jeff J. Andrews
Affiliation:
Department of Physics, University of Crete, Heraklion, Greece email: [email protected] Foundation for Research and Technology Hellas (FORTH), Heraklion, Greece
Kosmas Gazeas
Affiliation:
Department of Astrophysics, University of Athens, Zografos, Athens, Greece
John S. Gallagher
Affiliation:
Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA
Andrew Ptak
Affiliation:
NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771, USA
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Abstract

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We use deep Chandra and HST data to uniquely classify the X-ray binary (XRB) populations in M81 on the basis of their donor stars and local stellar populations (into early-type main sequence, yellow giant, supergiant, low-mass, and globular cluster). First, we find that more massive, redder, and denser globular clusters are more likely to be associated with XRBs. Second, we find that the high-mass XRBs (HMXBs) overall have a steeper X-ray luminosity function (XLF) than the canonical star-forming galaxy XLF, though there is some evidence of variations in the slopes of the sub-populations. On the other hand, the XLF of the prototypical starburst M82 is described by the canonical powerlaw (αcum ∼ 0.6) down to LX ∼ 1036 erg s−1. We attribute variations in XLF slopes to different mass transfer modes (Roche-lobe overflow versus wind-fed systems).

Keywords

accretionstars: neutrongalaxies: star clustersgalaxies: individual (M81, M82)galaxies: spiralgalaxies: starburstX-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 344 - 349
Copyright
© International Astronomical Union 2019 

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