PhD Thesis (PDF) - Department of Astronomy - University of Virginia

Fig. 6.5.— Scatter plot of estimated GC size (rh,cor) versus GC magnitude (Z850),
where the symbols follow that of Figure 6.1. Overlaid are lines of constant binary
encounter rate that decrease by 0.5 dex starting at log Γh = 9.0 (lower left). The
Galactic version of this plot for V -band is displayed in BIS+2006, Figure 3. GCs
with larger encounter rates are more likely to contain LMXBs.
are more likely to contain LMXBs, then the Γh we calculate will underpredict the
binary interaction rate for GCs with LMXBs. We plot rh,cor versus Z850 for GCs
in our sample, overlaying lines of constant Γh, in Figure 6.5 for comparison with
BIS+2006, Figure 3.
6.2.4 Matching LMXBs And GCs
To determine the relative astrometry between CXO and HST observations for each
galaxy, we convolved the X-ray and optical positions with a σ = 0. ′′ 5 2-dimensional
Gaussian, and cross-correlated the two images with an offset in RA and Dec. The
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