  We studied the transient neutron-star low-mass X-ray binary GRS 1747-312,
located in the globular cluster Terzan 6, in its quiescent state after its
outburst in August 2004, using an archival XMM-Newton observation. A source was
detected in this cluster and its X-ray spectrum can be fitted with the
combination of a soft, neutron-star atmosphere model and a hard, power-law
model. Both contributed roughly equally to the observed 0.5-10 keV luminosity
(~4.8X10^33 erg/s). This type of X-ray spectrum is typically observed for
quiescent neutron-star X-ray transients that are perhaps accreting in
quiescence at very low rates. Therefore, if this X-ray source is the quiescent
counterpart of GRS 1747-312, then this source is also accreting at low levels
in-between outbursts. Since source confusion a likely problem in globular
clusters, it is quite possible that part, if not all, of the emission we
observed is not related to GRS 1747-312, and is instead associated with another
source or conglomeration of sources in the cluster. Currently, it is not
possible to determine exactly which part of the emission truly originates from
GRS 1747-312, and a Chandra observation (when no source is in outburst in
Terzan 6) is needed to be conclusive. Assuming that the detected emission is
due to GRS 1747-312, we discuss the observed results in the context of what is
known about other quiescent systems. We also investigated the thermal evolution
of the neutron star in GRS 1747-312, and inferred that GRS 1747-312 can be
considered a typical quiescent system under our assumptions.
