We report on data obtained with the Chandra , XMM-Newton , Suzaku and Swift X-ray observatories , following the 2006 outburst of the Anomalous X-ray Pulsar CXOU J164710.2 - 455216 .
We find no evidence for the very large glitch and rapid exponential decay as was reported previously for this source .
We set a 3 \sigma upper limit on any fractional frequency increase at the time of the outburst of \Delta \nu / \nu < 1.5 \times 10 ^ { -5 } .
Our timing analysis , based on the longest time baseline yet , yields a spin-down rate for the pulsar that implies a surface dipolar magnetic field of \sim 9 \times 10 ^ { 13 } G , although this could be biased high by possible recovery from an undetected glitch .
We also present an analysis of the source flux and spectral evolution , and find no evidence for long-term spectral relaxation post-outburst as was previously reported .