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ABSTRACT  Using  Chandra  data taken in 2008 June, we detected pulsations at 2.594 39(4) s in the soft gamma‐ray repeater SGR  1627− 41. This is the second measurement of the source spin period and allows us to derive for the first time a long‐term spin‐down rate of  (1.9 ± 0.4) × 10 −11  s s −1  . From this value, we infer for SGR  1627− 41 a characteristic age of ∼2.2 kyr, a spin‐down luminosity of  ∼4 × 10 34  erg s −1   (one of the highest among sources of the same class), and a surface dipole magnetic field strength of  ∼2 × 10 14   G. These properties confirm the magnetar nature of SGR  1627− 41; however, they should be considered with caution since they were derived on the basis of a period derivative measurement made using two epochs only, and magnetar spin‐down rates are generally highly variable. The pulse profile, double‐peaked and with a pulsed fraction of  13 ± 2  per cent in the 2–10 keV range, closely resembles that observed by  XMM–Newton  in 2008 September. Having for the first time a timing model for this soft gamma‐ray repeater (SGR), we also searched for a pulsed signal in archival radio data collected with the Parkes radio telescope 9 months after the previous X‐ray outburst. No evidence for radio pulsations was found, down to a luminosity level ∼10–20 times fainter (for a 10 per cent duty cycle and a distance of 11 kpc) than the peak luminosity shown by the known radio magnetars.

Spin‐down rate and inferred dipole magnetic field of the soft gamma‐ray repeater SGR 1627–41