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Different generations of HMXBs: clues about their formation efficiency from Magellanic Clouds studies

Published online by Cambridge University Press:  30 December 2019

Vallia Antoniou Open the ORCID record for Vallia Antoniou [Opens in a new window] ,
Andreas Zezas ,
Jeremy J. Drake ,
Carles Badenes ,
Frank Haberl ,
Jaesub Hong ,
Paul P. Plucinsky  and
the SMC XVP Collaboration Team
Vallia Antoniou
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA,USA email: vantoniou@cfa.harvard.edu Texas Tech University, Department of Physics & Astronomy, Lubbock, TX, USA
Andreas Zezas
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA,USA email: vantoniou@cfa.harvard.edu University of Crete, Department of Physics, Heraklion, Greece IESL, Foundation for Research and Technology-Hellas, Heraklion, Greece
Jeremy J. Drake
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA,USA email: vantoniou@cfa.harvard.edu
Carles Badenes
Affiliation:
University of Pittsburgh, Department of Physics & Astronomy, Pittsburgh, PA, USA
Frank Haberl
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany
Jaesub Hong
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA,USA email: vantoniou@cfa.harvard.edu Harvard University, Department of Astronomy, Cambridge, MA, USA
Paul P. Plucinsky
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA,USA email: vantoniou@cfa.harvard.edu
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Abstract

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Nearby star-forming galaxies offer a unique environment to study the populations of young (<100 Myr) accreting binaries. These systems are tracers of past populations of massive stars that heavily affect their immediate environment and parent galaxies. Using a Chandra X-ray Visionary program, we investigate the young neutron-star binary population in the low metallicity of the Small Magellanic Cloud (SMC) by reaching quiescent X-ray luminosity levels (~few times 1032 erg/s). We present the first measurement of the formation efficiency of high-mass X-ray binaries (HMXBs) as a function of the age of their parent stellar populations by using 3 indicators: the number ratio of HMXBs to OB stars, to the SFR, and to the stellar mass produced during the specific star-formation burst they are associated with. In all cases, we find that the HMXB formation efficiency increases as a function of time up to ~40–60 Myr, and then gradually decreases.

Keywords

X-rays: binaries(galaxies:) Magellanic Clouds(stars:) pulsars: generalstars: neutronstars: emission-lineBestars: early-typestars: formation
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. 316 - 321
Copyright
© International Astronomical Union 2019 

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