SGR 1833–0832 was discovered on 2010 March 19 thanks to the Swift  detection of a short hard X-ray burst and follow-up X-ray observations .
Since then , it was repeatedly observed with Swift , Rossi X-ray Timing Explorer , and XMM-Newton .
Using these data , which span about 225 days , we studied the long-term spectral and timing characteristics of SGR 1833–0832 .
We found evidence for diffuse emission surrounding SGR 1833–0832 , which is most likely a halo produced by the scattering of the point source X-ray radiation by dust along the line of sight , and we show that the source X-ray spectrum is well described by an absorbed blackbody , with temperature kT \sim 1.2 keV and absorbing column N _ { H } = ( 10.4 \pm 0.2 ) \times 10 ^ { 22 } cm ^ { -2 } , while different or more complex models are disfavoured .
The source persistent X-ray emission remained fairly constant at \sim 3.7 \times 10 ^ { -12 } erg cm ^ { -2 } s ^ { -1 } Â for the first \sim 20 days after the onset of the bursting episode , then it faded by a factor \sim 40 in the subsequent \sim 140 days , following a power-law trend with index \alpha \simeq - 0.5 .
We obtained a phase-coherent timing solution with the longest baseline ( \sim 225 days ) to date for this source which , besides period P = 7.565 408 4 ( 4 ) s and period derivative \dot { P } = 3.5 ( 3 ) \times 10 ^ { -12 } s s ^ { -1 } , includes higher order period derivatives .
We also report on our search of the counterpart to the SGR at radio frequencies using the Australia Telescope Compact Array and the Parkes radio telescope .
No evidence for radio emission was found , down to flux densities of 0.9 mJy ( at 1.5 GHz ) and 0.09 mJy ( at 1.4 GHz ) for the continuum and pulsed emissions , respectively , consistently with other observations at different epochs .
Finally , the analysis of the field of PSR B1830–08 ( J1833–0827 ) , which was serendipitously imaged by the XMM-Newton  observations , led to the discovery of the X-ray pulsar wind nebula generated by this 85-ms radio pulsar .
We discuss its possible association with the unidentified TeV source HESS J1834–087 .