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Nearby star-forming galaxies offer a unique environment to study thepopulations of young ($<$100 Myr) accreting binaries. These systems are tracersof past populations of massive stars that heavily affect their immediateenvironment and parent galaxies. Using a Chandra X-ray Visionary program, weinvestigate the young neutron-star binary population in the low metallicity ofthe Small Magellanic Cloud (SMC) by reaching quiescent X-ray luminosity levels($\sim$few times $10^{32}$ erg/s). We present the first measurement of theformation efficiency of high-mass X-ray binaries (HMXBs) as a function of theage of their parent stellar populations by using 3 indicators: the number ratioof HMXBs to OB stars, to the SFR, and to the stellar mass produced during thespecific star-formation burst they are associated with. In all cases, we findthat the HMXB formation efficiency increases as a function of time up to$\sim$40-60 Myr, and then gradually decreases.

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