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Deep Chandra survey of the Small Magellanic Cloud. III. Formation efficiency of High-Mass X-ray binaries | | Vallia Antoniou
; Andreas Zezas
; Jeremy J. Drake
; Carles Badenes
; Frank Haberl
; Nicholas J. Wright
; Jaesub Hong
; Rosanne Di Stefano
; Terrance J. Gaetz
; Knox S. Long
; Paul P. Plucinsky
; Manami Sasaki
; Benjamin F. Williams
; P. Frank Winkler
; | | Date: |
4 Jan 2019 | | Abstract: | We have compiled the most complete census of High-Mass X-ray Binaries (HMXBs)
in the Small Magellanic Cloud with the aim to investigate the formation
efficiency of young accreting binaries in its low metallicity environment. In
total, we use 127 X-ray sources with detections in our chandra X-ray Visionary
Program (XVP), supplemented by 14 additional (likely and confirmed) HMXBs
identified by cite{2016A&A...586A..81H} that fall within the XVP area, but are
not either detected in our survey (9 sources) or matched with any XVP source
that has at least one OB counterpart in the OGLE-III catalog (5 sources).
Specifically, we examine the number ratio of the HMXBs [N(HMXBs)] to {it (a)}
the number of OB stars, {it (b)} the local star-formation rate (SFR), and {it
(c)} the stellar mass produced during the specific star-formation burst, all as
a function of the age of their parent stellar populations. Each of these
indicators serves a different role, but in all cases we find that the HMXB
formation efficiency increases as a function of time (following a burst of star
formation) up to $sim$40--60,Myr, and then gradually decreases. The peak
formation efficiency N(HMXB)/SFR is (49 $pm$ 14) $[10^{-5}~{
m
M_{odot}/yr}]^{-1}$, in good agreement with previous estimates of the average
formation efficiency in the broad $sim$20--60,Myr age range. The frequency of
HMXBs is a factor of 8$ imes$ higher than at $sim$10,Myr, and 4$ imes$
higher than at $sim$260,Myr, i.e. at earlier and later epochs, respectively. | | Source: | arXiv, 1901.1237 | | Services: | Forum | Review | PDF | Favorites | |
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