Abstract
Using Chandra, XMM-Newton, and optical photometric catalogs we study the young X-ray binary (XRB) populations of the Small Magellanic Cloud. We find that the Be/X-ray binaries (Be-XRBs) are observed in regions with star formation rate bursts ∼25-60 Myr ago. The similarity of this age with the age of maximum occurrence of the Be phenomenon (∼40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range. We also find that regions with strong but more recent star formation (e.g., the Wing) are deficient in Be-XRBs. By correlating the number of observed Be-XRBs with the formation rate of their parent populations, we measure a Be-XRB production rate of ∼1 system per 3 × 10-3 M ȯyr-1. Finally, we use the strong localization of the Be-XRB systems in order to set limits on the kicks imparted on the neutron star during the supernova explosion.
| Original language | English (US) |
|---|---|
| Pages (from-to) | L140-L145 |
| Journal | Astrophysical Journal Letters |
| Volume | 716 |
| Issue number | 2 PART 2 |
| DOIs | |
| State | Published - 2010 |
Keywords
- Magellanic Clouds
- X-rays: binaries
- pulsars: general
- stars: early-type
- stars: emission-line, Be
- stars: formation
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science