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

## TL;DR

This study investigates how the formation efficiency of high-mass X-ray binaries (HMXBs) in the Small Magellanic Cloud varies with the age of their parent stellar populations, revealing an increase up to 40-60 Myr followed by a decline.

## Contribution

First measurement of HMXB formation efficiency as a function of stellar population age in the SMC using multiple indicators.

## Key findings

- HMXB formation efficiency peaks at 40-60 Myr after star formation
- Efficiency increases with time up to peak, then declines
- Provides new insights into HMXB formation timescales

## Abstract

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.