We present results from a 34 ks Chandra/ACIS-S observation of the LMXB population and the hot ISM in the nearby ( d=3.1 Mpc ) lenticular galaxy NGC 5102 , previously shown to have an unusually low X-ray luminosity .
We detect eleven X-ray point sources within the the D _ { 25 } optical boundary of the galaxy ( 93 % of the light ) , one third to one half of which are likely to be background AGN .
One of the X-ray sources is coincident with the optical nucleus and may be a low-luminosity AGN .
Only two sources with an X-ray luminosity greater than 10 ^ { 37 } ergs s ^ { -1 } in the 0.5-5.0 keV band were detected , one of which is statistically likely to be a background AGN .
We expected to detect 7 or 5 such luminous sources if the XRB population scales linearly with the B band or J band magnitudes , respectively , of the host galaxy .
By this measure , NGC 5102 has an unusually low number of XRBs .
The deficit of LMXBs is even more striking because some of these sources may in fact be HMXBs .
NGC 5102 is unusually blue for its morphological type , and has undergone at least two recent bursts of star formation only \sim 1.5 \times 10 ^ { 7 } and \sim 3 \times 10 ^ { 8 } years ago .
We present the results of optical/UV spectral synthesis analysis and demonstrate that a significant fraction ( > 50 % ) of the stars in this galaxy are comparatively young ( < 3 \times 10 ^ { 9 } years old ) .
We discuss the relationship between the XRB population , the globular cluster population , and the relative youth of the majority of stars in this galaxy .
If the lack of X-ray binaries is related to the relative youth of most of the stars , this would support models of LMXB formation and evolution that require wide binaries to shed angular momentum on a timescale of Gyrs .
We have also analyzed archival HST images of NGC 5102 , and find that it has an unusually low specific frequency of globular clusters ( S _ { N } \sim 0.4 ) .
The lack of LMXBs could also be explained by the small number of GCs .
We have also detected diffuse X-ray emission in the central \sim 1 kpc of the galaxy with an X-ray luminosity of 4.1 \times 10 ^ { 37 } ergs s ^ { -1 } in the 0.1-2.0 keV band .
This hot gas is most likely a superbubble created by multiple supernovae of massive stars born during the most recent star burst , and is driving the shock into the ISM which was inferred from previous [ O III ] \lambda 5007 and H _ { \alpha } observations .