After nearly a decade of quiescence, the soft gamma-ray repeater SGR 1627-41 reactivated on 2008 May 28 with a bursting episode followed by a slowly decaying enhancement of its persistent emission. To search for the still unknown spin period of this SGR taking advantage of its high flux state, we performed on 2008 September 27-28 a 120 ks long X-ray observation with the XMM-Newton satellite. Pulsations with P = 2.594578(6) s were detected at a higher than 6σ confidence level, with a double-peaked pulse profile. The pulsed fraction in the 2-12 keV range is 19% ± 3% and 24% ± 3% for the fundamental and the second harmonic, respectively. The observed 2-10 keV flux is 3.4 × 10-13 erg cm-2 s-1, still a factor of ~ 5 above the quiescent pre-burst-activation level, and the spectrum is well fitted by an absorbed power law plus blackbody model (photon index Γ sime 0.6, blackbody temperature kT sime 0.5 keV, and absorption N H ≈ 1.2 × 1023 cm-2). We also detected a shell of diffuse soft X-ray emission which is likely associated with the young supernova remnant G337.0-0.1.
XMM-Newtion Discovery of 2.6 s Pulsations in the Soft-Gamma Repeater SGR 1627-41
TUROLLA, ROBERTO;
2009
Abstract
After nearly a decade of quiescence, the soft gamma-ray repeater SGR 1627-41 reactivated on 2008 May 28 with a bursting episode followed by a slowly decaying enhancement of its persistent emission. To search for the still unknown spin period of this SGR taking advantage of its high flux state, we performed on 2008 September 27-28 a 120 ks long X-ray observation with the XMM-Newton satellite. Pulsations with P = 2.594578(6) s were detected at a higher than 6σ confidence level, with a double-peaked pulse profile. The pulsed fraction in the 2-12 keV range is 19% ± 3% and 24% ± 3% for the fundamental and the second harmonic, respectively. The observed 2-10 keV flux is 3.4 × 10-13 erg cm-2 s-1, still a factor of ~ 5 above the quiescent pre-burst-activation level, and the spectrum is well fitted by an absorbed power law plus blackbody model (photon index Γ sime 0.6, blackbody temperature kT sime 0.5 keV, and absorption N H ≈ 1.2 × 1023 cm-2). We also detected a shell of diffuse soft X-ray emission which is likely associated with the young supernova remnant G337.0-0.1.
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