Quiescent low-mass X-ray binaries ( qLMXBs ) containing neutron stars have been identified in several globular clusters using { \it Chandra } or XMM X-ray observations , using their soft thermal spectra .
We report a complete census of the qLMXB population in these clusters , identifying three additional probable qLMXBs in NGC 6440 .
We conduct several analyses of the qLMXB population , and compare it with the harder , primarily CV , population of low-luminosity X-ray sources with 10 ^ { 31 } < L _ { X } < 10 ^ { 32.5 } 
ergs s ^ { -1 } .
The radial distribution of our qLMXB sample suggests an average system mass of 1.5 ^ { +0.3 } _ { -0.2 } { M _ { \odot } } , consistent with a neutron star and low-mass companion .
Spectral analysis reveals that no globular cluster qLMXBs , other than the transient in NGC 6440 , require an additional hard power-law component as often observed in field qLMXBs .
We identify an empirical lower luminosity limit of 10 ^ { 32 } ergs s ^ { -1 } among globular cluster qLMXBs .
The bolometric luminosity range of qLMXBs implies ( in the deep crustal heating model of Brown and collaborators ) low time-averaged mass transfer rates , below the disk stability criterion .
The X-ray luminosity functions of the CV populations alone in NGC 6397 and 47 Tuc are shown to differ .
The distribution of qLMXBs among globular clusters is consistent with their dynamical formation by either tidal capture or exchange encounters , allowing us to estimate that seven times more qLMXBs than bright LMXBs reside in globular clusters .
The distribution of harder sources ( primarily CVs ) has a weaker dependence upon density than that of the qLMXBs .
Finally , we discuss possible effects of core collapse and globular cluster destruction upon X-ray source populations .