@article{0004-637X-856-2-180,
  author={F. Camilo and P. Scholz and M. Serylak and S. Buchner and M. Merryfield and V. M. Kaspi and R. F. Archibald and M. Bailes and A.
Jameson and W. van Straten and J. Sarkissian and J. E. Reynolds and S. Johnston and G. Hobbs and T. D. Abbott and R. M. Adam and G.
B. Adams and T. Alberts and R. Andreas and K. M. B. Asad and D. E. Baker and T. Baloyi and E. F. Bauermeister and T. Baxana and T.
G. H. Bennett and G. Bernardi and D. Booisen and R. S. Booth and D. H. Botha and L. Boyana and L. R. S. Brederode and J. P.
Burger and T. Cheetham and J. Conradie and J. P. Conradie and D. B. Davidson and G. De Bruin and B. de Swardt and C. de
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Hoorn and D. Horn and J. Horrell and B. Hugo and A. Isaacson and O. Jacobs and J. P. Jansen van Rensburg and J. L. Jonas and B.
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Rasivhaga and S. Ratcliffe and H. C. Reader and R. Renil and L. Richter and A. Robyntjies and D. Rosekrans and A. Rust and S.
Salie and N. Sambu and C. T. G. Schollar and L. Schwardt and S. Seranyane and G. Sethosa and C. Sharpe and R. Siebrits and S. K.
Sirothia and M. J. Slabber and O. Smirnov and S. Smith and L. Sofeya and N. Songqumase and R. Spann and B. Stappers and D. Steyn and T.
J. Steyn and R. Strong and A. Struthers and C. Stuart and P. Sunnylall and P. S. Swart and B. Taljaard and C. Tasse and G. Taylor and I.
P. Theron and V. Thondikulam and K. Thorat and A. Tiplady and O. Toruvanda and J. van Aardt and T. van Balla and L. van den
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Young and S. Zitha},
  title={Revival of the Magnetar PSR J1622–4950: Observations with MeerKAT, Parkes, XMM-Newton , Swift , Chandra , and NuSTAR},
  journal={The Astrophysical Journal},
  volume={856},
  number={2},
  pages={180},
  url={http://stacks.iop.org/0004-637X/856/i=2/a=180},
  year={2018},
  abstract={New radio (MeerKAT and Parkes) and X-ray ( XMM-Newton , Swift , Chandra , and NuSTAR ) observations of PSR J1622–4950 indicate that the magnetar, in a quiescent state since at least early 2015, reactivated between 2017 March 19 and April 5. The radio flux density, while variable, is approximately 100× larger than during its dormant state. The X-ray flux one month after reactivation was at least 800× larger than during quiescence, and has been decaying exponentially on a 111 ± 19 day timescale. This high-flux state, together with a radio-derived rotational ephemeris, enabled for the first time the detection of X-ray pulsations for this magnetar. At 5%, the 0.3–6 keV pulsed fraction is comparable to the smallest observed for magnetars. The overall pulsar geometry inferred from polarized radio emission appears to be broadly consistent with that determined 6–8 years earlier. However, rotating vector model fits suggest that we are now seeing radio emission from a different location in the magnetosphere than previously. This indicates a novel way in which radio emission from magnetars can differ from that of ordinary pulsars. The torque on the neutron star is varying rapidly and unsteadily, as is common for magnetars following outburst, having changed by a factor of 7 within six months of reactivation.}
}