Stacking Star Clusters in M51: Searching for Faint X-Ray Binaries
  The population of low-luminosity (< 10^35 erg/s) X-Ray Binaries (XRBs) has
been investigated in our Galaxy and M31 but not further. To address this
problem, we have used data from the Chandra X-Ray Observatory and the Hubble
Space Telescope to investigate the faint population of XRBs in the grand-design
spiral galaxy M51. A matching analysis found 25 star clusters coincident with
20 X-ray point sources within 1.5" (60 pc). From X-ray and optical color-color
plots we determine that this population is dominated by high-mass XRBs. A
stacking analysis of the X-ray data at the positions of optically-identified
star clusters was completed to probe low-luminosity X-ray sources. No cluster
type had a significant detection in any X-ray energy band. An average globular
cluster had the largest upper limit, 9.23 x 10^34 erg/s, in the full-band (0.3
- 8 keV) while on average the complete sample of clusters had the lowest upper
limit, 6.46 x 10^33 erg/s in the hard-band (2 - 8 keV). We determined average
luminosities of the young and old star cluster populations and compared the
results to those from the Milky Way. We conclude that deeper X-ray data is
required to identify faint sources with a stacking analysis.
