Observed cumulative log 𝒩–log S distribution of our sample of FXRTs as a function of fluence (in units of Crab^† × second). Also shown are two PL models, N(> S)∝S^−γ, with slopes γ  =  0.5 (red line) and 1.0 (blue line). The γ  =  0.5 line denotes the best fit to the CSC2 sample. The γ  =  1 line represents the best fit and 1σ error of Arefiev et al. (2003) based on bright FXRTs. The brightest sources in our sample appear to be consistent with this bright-end extrapolation, although our fainter sources fall ∼1 dex below, implying a break. For comparison with Arefiev et al. (2003), we convert the fluence to 2–10 keV. †A Crab is a standard astrophotometric unit for measurement of the intensity of celestial X-ray sources.