Volume 509, January 2010
|Number of page(s)||4|
|Published online||12 January 2010|
Letter to the Editor
Swift monitoring of the new accreting millisecond X-ray pulsar IGR J17511-3057 in outburst
ISDC data centre for astrophysics, University of Geneva,
Chemin d'Écogia 16, 1290 Versoix, Switzerland e-mail: Enrico.Bozzo@unige.ch
2 IAAT, Abt. Astronomie, Universität Tübingen Sand 1, 72076 Tübingen, Germany
3 International Space Science Institute (ISSI) Hallerstrasse 6, 3012 Bern, Switzerland
4 INAF – Osservatorio Astronomico di Brera, via Emilio Bianchi 46, 23807 Merate (LC), Italy
5 Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA
6 Universitá degli Studi di Cagliari, Dipartimento di Fisica, SP Monserrato-Sestu, KM 0.7, 09042 Monserrato, Italy
7 INAF – Osservatorio Astronomico di Cagliari, Poggio dei Pini, Strada 54, 09012 Capoterra (CA), Italy
Accepted: 28 November 2009
Context. A new accreting millisecond X-ray pulsar, IGR J17511-3057, was discovered in outburst on 2009 September 12 during the INTEGRAL Galactic bulge monitoring programme.
Aims. To study the evolution of the source X-ray flux and spectral properties during the outburst, we requested a Swift monitoring of IGR J17511-3057.
Methods. In this paper we report on the results of the first two weeks of monitoring the source.
Results. The persistent emission of IGR J17511-3057 during the outburst is modelled well with an absorbed blackbody ( keV) and a power-law component (Γ–2), similar to what has been observed from other previously known millisecond pulsars. Swift also detected three type-I Xray bursts from this source. By assuming that the peak luminosity of these bursts is equal to the Eddington value for a pure helium type-I X-ray burst, we derived an upper limit to the source distance of ~10 kpc. The theoretically expected recurrence time of the bursts according to the helium burst hypothesis is 0.2–0.9 days, in agreement with the observations.
Key words: X-rays: binaries / pulsars: individual: IGR J17511-3057
© ESO, 2010
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