TY - JOUR
T1 - Swift monitoring of the new accreting millisecond X-ray pulsar IGR J17511-3057 in outburst
AU - Bozzo, E.
AU - Ferrigno, C.
AU - Falanga, M.
AU - Campana, S.
AU - Kennea, J. A.
AU - Papitto, A.
N1 - Copyright:
Copyright 2016 Elsevier B.V., All rights reserved.
PY - 2010/1
Y1 - 2010/1
N2 - 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 IGRJ17511-3057. Methods: In this paper we report on the results of the first two weeks of monitoring the source. Results. The persistent emission of IGRJ17511-3057 during the outburst is modelled well with an absorbed blackbody (kT ∼ 0.9 keV) and a power-law component (Τ∼ 1-2), 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.
AB - 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 IGRJ17511-3057. Methods: In this paper we report on the results of the first two weeks of monitoring the source. Results. The persistent emission of IGRJ17511-3057 during the outburst is modelled well with an absorbed blackbody (kT ∼ 0.9 keV) and a power-law component (Τ∼ 1-2), 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.
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U2 - 10.1051/0004-6361/200913517
DO - 10.1051/0004-6361/200913517
M3 - Article
AN - SCOPUS:76349118751
SN - 0004-6361
VL - 509
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
IS - 1
M1 - L3
ER -