Magnetar twists: fermi/gamma-ray burst monitor detection of SGR J1550-5418

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Official URL: http://dx.doi.org/10.1088/0004-637X/710/2/1335

SGR J1550-5418 (previously known as AXP 1E 1547.0-5408 or PSR J1550-5418) went into three active bursting episodes in 2008 October and in 2009 January and March, emitting hundreds of typical soft gamma repeater bursts in soft gamma rays. The second episode was especially intense, and our untriggered burst search on Fermi/Gamma-ray Burst Monitor (GBM) data (8-1000 keV) revealed similar to 450 bursts emitted over 24 hr during the peak of this activity. Using the GBM data, we identified a similar to 150 s long enhanced persistent emission during 2009 January 22 that exhibited intriguing timing and spectral properties: (1) clear pulsations up to similar to 110 keV at the spin period of the neutron star (P similar to 2.07 s, the fastest of all magnetars); (2) an additional (to a power-law) blackbody component required for the enhanced emission spectra with kT similar to 17 keV; and (3) pulsed fraction that is strongly energy dependent and highest in the 50-74 keV energy band. A total isotropic-equivalent energy emitted during this enhanced emission is estimated to be 2.9x10(40)(D/5 kpc)(2) erg. The estimated area of the blackbody emitting region of approximate to 0.046(D/5 kpc)(2) km(2) (roughly a few x 10(-5) of the neutron star area) is the smallest "hot spot" ever measured for a magnetar and most likely corresponds to the size of magnetically confined plasma near the neutron star surface.