Different generations of HMXBs: clues about their formation efficiency from Magellanic Clouds studies. (arXiv:1812.11070v1 [astro-ph.HE])

Different generations of HMXBs: clues about their formation efficiency from Magellanic Clouds studies. (arXiv:1812.11070v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Antoniou_V/0/1/0/all/0/1">Vallia Antoniou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zezas_A/0/1/0/all/0/1">Andreas Zezas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drake_J/0/1/0/all/0/1">Jeremy J. Drake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Badenes_C/0/1/0/all/0/1">Carles Badenes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haberl_F/0/1/0/all/0/1">Frank Haberl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hong_J/0/1/0/all/0/1">Jaesub Hong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plucinsky_P/0/1/0/all/0/1">Paul P. Plucinsky</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Team_SMC_XVP_Collaboration/0/1/0/all/0/1">SMC XVP Collaboration Team</a>

Nearby star-forming galaxies offer a unique environment to study the
populations of young ($<$100 Myr) accreting binaries. These systems are tracers of past populations of massive stars that heavily affect their immediate environment and parent galaxies. Using a Chandra X-ray Visionary program, we investigate the young neutron-star binary population in the low metallicity of the Small Magellanic Cloud (SMC) by reaching quiescent X-ray luminosity levels ($sim$few times $10^{32}$ 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 $sim$40-60 Myr, and then gradually decreases.

Nearby star-forming galaxies offer a unique environment to study the
populations of young ($<$100 Myr) accreting binaries. These systems are tracers
of past populations of massive stars that heavily affect their immediate
environment and parent galaxies. Using a Chandra X-ray Visionary program, we
investigate the young neutron-star binary population in the low metallicity of
the Small Magellanic Cloud (SMC) by reaching quiescent X-ray luminosity levels
($sim$few times $10^{32}$ 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
$sim$40-60 Myr, and then gradually decreases.

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