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We present the results of our 8 year X-ray monitoring campaign on CXOUJ171405.7-381031, the magnetar associated with the faint supernova remnant(SNR) CTB 37B. It is among the youngest by inferred spin-down age, and mostenergetic in spin-down power of magnetars, and may contribute, at leastpartially, to the GeV and TeV emission coincident with the SNR. We use a seriesof Chandra, XMM-Newton, and NuSTAR observations to characterize the timing andspectral properties of the magnetar. The spin-down rate of the pulsar almostdoubled in <1 year and then decreased slowly to a more stable value. Its X-rayflux varied by approx, 50%, possibly correlated with the spin down rate. The1-79 keV spectrum is well-characterized by an absorbed blackbody plus power-lawmodel with an average temperature of kT=0.62+/-0.04 keV and photon indexGamma=0.92+/-0.16, or by a Comptonized blackbody with kT=0.55+/-0.04 keV and anadditional hard power law with Gamma=0.70+/-0.20, In contrast with mostmagnetars, the pulsed signal is found to decrease with energy up to 6 keV,which is apparently caused by mixing with the hard spectral component that ispulse-phase shifted by approx. 0.43 cycles from the soft X-rays. We alsoanalyze the spectrum of the nearby, diffuse nonthermal source XMMUJ171410.8-381442, whose relation to the SNR is uncertain.

X-ray Monitoring of the Magnetar CXOU J171405.7-381031 in SNR CTB 37B