The Galactic Bulge Survey (GBS)

The predicted number of sources as a function of the limiting X-ray flux. The limit of our proposed Chandra

survey is 3.5E-14 erg cm-2 s-1. This is indicated with the vertical dashes. Deeper X-ray images are not necessary since the ratio between the number of LMXBs and cataclysmic variables such as intermediate polars will decrease. This would make it harder to pick out the LMXBs (i.e. much more optical classification spectra would have to be obtained).