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

Authors

  • P. Esposito,

    Corresponding author
    1. INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano, via E. Bassini 15, 20133 Milano, Italy
    2. Istituto Nazionale di Fisica Nucleare, sezione di Pavia, via A. Bassi 6, 27100 Pavia, Italy
      E-mail: paoloesp@iasf-milano.inaf.it
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  • M. Burgay,

    1. INAF/Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, 09012 Capoterra, Italy
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  • A. Possenti,

    1. INAF/Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, 09012 Capoterra, Italy
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  • R. Turolla,

    1. Dipartimento di Fisica, Università degli Studi di Padova, via F. Marzolo 8, 35131 Padova, Italy
    2. Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT
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  • S. Zane,

    1. Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT
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  • A. De Luca,

    1. INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano, via E. Bassini 15, 20133 Milano, Italy
    2. IUSS – Istituto Universitario di Studi Superiori, viale Lungo Ticino Sforza 56, 27100 Pavia, Italy
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  • A. Tiengo,

    1. INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano, via E. Bassini 15, 20133 Milano, Italy
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  • G. L. Israel,

    1. INAF/Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone, Italy
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  • F. Mattana,

    1. Laboratoire AstroParticule et Cosmologie, Université Paris 7 – Denis Diderot, rue A. Domon et L. Duquet 10, 75205 Paris, France
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  • S. Mereghetti,

    1. INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano, via E. Bassini 15, 20133 Milano, Italy
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  • M. Bailes,

    1. Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia
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  • P. Romano,

    1. INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, 90146 Palermo, Italy
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  • D. Götz,

    1. CEA Saclay, DSM/Irfu/Service d'Astrophysique, Orme des Merisiers, Bât. 709, 91191 Gif sur Yvette, France
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  • N. Rea

    1. University of Amsterdam, Astronomical Institute Anton Pannekoek, Kruislaan 403, 1098 SJ Amsterdam, the Netherlands
    2. CSIC – Institut d'Estudis Espacials de Catalunya, Campus UAB, Fac. Ciències, Torre C5 parell 2, 08193 Barcelona, Spain
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E-mail: paoloesp@iasf-milano.inaf.it

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 × 1034 erg s−1 (one of the highest among sources of the same class), and a surface dipole magnetic field strength of ∼2 × 1014 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.

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