  We observed the globular cluster NGC 6652 with Chandra for 47.5 ks, detecting
six known X-ray sources, as well as five previously undetected X-ray sources.
Source A (XB 1832-330) is a well-known bright low-mass X-ray binary (LXMB). The
second brightest source, B, has a spectrum that fits well to either a power-law
model (Gamma ~ 1.3) or an absorbed hot gas emission model (kT ~ 34 keV). Its
unabsorbed 0.5-10 keV luminosity (L_X = 1.6+-0.1*10^34 erg/s) is suggestive of
a neutron star primary; however, Source B exhibits unusual variability for a
LMXB, varying by over an order of magnitude on timescales of ~ 100 s. Source
C's spectrum contains a strong low-energy component below 1 keV. Its spectrum
is well fit to a simplified magnetic cataclysmic variable (CV) model, thus the
soft component may be explained by a hot polar cap of a magnetic CV. Source D
has an average L_X (0.5-10 keV) ~ 9*10^32 erg/s, and its spectrum is well fit
to a neutron star atmosphere model. This is indicative of a quiescent neutron
star LXMB, suggesting Source D may be the third known LMXB in NGC 6652. Source
E has L_X (0.5-10 keV) ~ 3*10^32 erg/s, while Source F has L_X (0.5-10 keV) ~
1*10^32 erg/s. Their relatively hard X-ray spectra are well-fit by power-law or
plasma emission models. Five newly detected fainter sources have luminosities
between 1-5*10^31 erg/s. NGC 6652 has an unusually flat X-ray luminosity
function compared to other globular clusters, which may be connected to its
extremely high central density.
