Abstract
The discovery of the very‐high‐energy γ‐ray source, HESS J1713‐381, apparently associated with the shell‐type supernova remnant (SNR) CTB 37B, was announced by the H.E.S.S. Collaboration in 2006. X‐ray follow‐up observations with Chandra were performed in 2007 with the aim of identifying the origin of the observed emission and improving our knowledge of this SNR. The new Chandra data reveal thermal emission from a 4’ region close to the radio shell of CTB 37B. We discuss the implications of the thermal X‐ray data for the age and environment of the SNR, and revisit the TeV emission of HESS J1713‐381 using new data from H.E.S.S. In addition we discuss the distance to CTB 37B, using recent CO and HI data.
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