  The >100 GeV gamma-ray source, HESS J1713-381, apparently associated with the
shell-type supernova remnant (SNR) CTB 37B, was discovered using H.E.S.S. in
2006. X-ray follow-up observations with Chandra were performed in 2007 with the
aim of identifying a synchrotron counterpart to the TeV source and/or thermal
emission from the SNR shell. These new Chandra data, together with additional
TeV data, allow us to investigate the nature of this object in much greater
detail than was previously possible. The new X-ray data reveal thermal emission
from a ~4' region in close proximity to the radio shell of CTB 37B. The
temperature of this emission implies an age for the remnant of ~5000 years and
an ambient gas density of ~0.5 cm-3. Both these estimates are considerably
uncertain due to the asymmetry of the SNR and possible modifications of the
kinematics due to efficient cosmic ray (CR) acceleration. A bright (~7x10-13erg
cm-2s-1) and unresolved (<1'') source (CXOU J171405.7-381031) with a soft
(\Gamma ~3.3) non-thermal spectrum is also detected in coincidence with the
radio shell. Absorption indicates a column density consistent with the thermal
emission from the shell suggesting a genuine association rather than a chance
alignment. The observed TeV morphology is consistent with an origin in the
complete shell of CTB 37B. The lack of diffuse non-thermal X-ray emission
suggests an origin of the gamma-ray emission via the decay of neutral pions
produced in interactions of protons and nuclei, rather than inverse Compton
(IC) emission from relativistic electrons.
