We report on an observation of SGR 1627 - 41 made with the Chandra X-ray Observatory on 2011 June 16 .
Approximately three years after its outburst activity in 2008 , the source ’ s flux has been declining , as it approaches its quiescent state .
For an assumed power-law spectrum , we find that the absorbed 2–10 keV flux for the source is 1.0 ^ { +0.3 } _ { -0.2 } \times 10 ^ { -13 } erg cm - 2 s - 1 with a photon index of 2.9 \pm 0.8 ( N _ { H } = 1.0 \times 10 ^ { 23 } cm - 2 ) .
This flux is approximately consistent with that measured at the same time after the source ’ s outburst in 1998 .
With measurements spanning 3 years after the 2008 outburst , we analyze the long-term flux and spectral evolution of the source .
The flux evolution is well described by a double exponential with decay times of 0.5 \pm 0.1 and 59 \pm 6 days , and a thermal cooling model fit suggests that SGR 1627 - 41 may have a hot core ( T _ { c } \sim 2 \times 10 ^ { 8 } { K } ) .
We find no clear correlation between flux and spectral hardness as found in other magnetars .
We consider the quiescent X-ray luminosities of magnetars and the subset of rotation-powered pulsars with high magnetic fields ( B \gtrsim 10 ^ { 13 } { G } ) in relation to their spin-inferred surface magnetic-field strength , and find a possible trend between the two quantities .