  This paper presents the analysis of candidate quiescent low mass xray binarie
(qLMXBs) observed during a short Chandra/ACIS observation of the globular
cluster (GC) NGC 6304. Two out of the three candidate qLMXBs of this cluster,
XMMU 171433-292747 and XMMU 171421-292917, lie within the field of view. This
permits comparison with the discovery observation of these sources. The one in
the GC core -- XMMU 171433-292747 -- is spatially resolved into two separate
X-ray sources, one of which is consistent with a pure H-atmosphere qLMXB, and
the other is an X-ray power-law spectrum source. These two spectral components
separately account for those observed from XMMU 171433-292747 in its discovery
observation. We find that the observed flux and spectral parameters of the
H-atmosphere spectral components are consistent with the previous observation,
as expected from a qLMXB powered by deep crustal heating. XMMU 171421-292917
also has neutron star atmosphere spectral parameters consistent with those in
the XMM-Newton observation and the observed flux has decreased by a factor
0.54^{+0.30}_{-0.24}.
