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We obtained a second Chandra timing measurement of the 3.82 s pulsar CXOUJ171405.7-381031 in the supernova remnant (SNR) CTB 37B, which shows that it isspinning down rapidly. The average period derivative of (5.88+/-0.08)E-11 overthe 1 year time span corresponds to a dipole magnetic field strength B = 4.8E14G, well into the magnetar range. The spin-down power E-dot = 4.2E34 erg/s isamong the largest for magnetars, and the corresponding characteristic age Tau =P/2P-dot = 1030 years is comparable to estimates of the age of the SNR. Theperiod derivative enables us to recover probable pulsations in an ASCAobservation taken in 1996, which yields a mean characteristic age of 860 yearsover the longer 13 year time span. The source is well detected up to 10 keV,and its composite spectrum is typical of a magnetar. CTB 37B hosts HESSJ1713-381, the first TeV source that is coincident with a magnetar. While theTeV emission has been attributed to the SNR shell, it is possibly centrallypeaked, and we hypothesize that this particularly young, energetic magnetar maycontribute to the HESS source. We also searched for pulsations from anothersource in a HESS SNR, XMMU J173203.3-344518 in HESS J1731-347/G353.6-0.7 butcould not confirm pulsations or long-term flux variability, making it morelikely that this source is a weakly magnetized central compact object.

An Energetic Magnetar in HESS J1713-381/CTB 37B