The X-ray spectrum of the newly discovered accreting millisecond pulsar IGR J17511-3057

Details The X-ray spectrum of the newly discovered accreting millisecond pulsar IGR J17511-3057 The X-ray spectrum of the newly discovered accreting millisecond pulsar IGR J17511-3057

2010-05-26

arxiv.org/abs/1005.4827v1

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

16 pages, 10 figures, 4 tables, accepted for publication in MNRAS

Scientific paper

We report on an XMM-Newton observation of the accreting millisecond pulsar, IGR J17511-3057. Pulsations at 244.8339512(1) Hz are observed with an RMS pulsed fraction of 14.4(3)%. A precise solution for the P_orb=12487.51(2)s binary system is derived. The measured mass function indicates a main sequence companion with a mass between 0.15 and 0.44 Msun. The XMM-Newton spectrum of the source can be modelled by at least three components, multicoloured disc emission, thermal emission from the NS surface and thermal Comptonization emission. Spectral fit of the XMM-Newton data and of the RXTE data, taken in a simultaneous temporal window, constrain the Comptonization parameters: the electron temperature, kT_e=51(+6,-4) keV, is rather high, while the optical depth (tau=1.34(+0.03,-0.06)) is moderate. The energy dependence of the pulsed fraction supports the interpretation of the cooler thermal component as coming from the accretion disc, and indicates that the Comptonizing plasma surrounds the hot spots on the NS surface, which provide the seed photons. Signatures of reflection, such as a broadened iron K-alpha emission line and a Compton hump at 30 keV ca., are also detected. We derive from the smearing of the reflection component an inner disc radius of ~> 40 km for a 1.4 Msun neutron star, and an inclination between 38{\deg} and 68{\deg}. XMM-Newton also observed two type-I X-ray bursts, probably ignited in a nearly pure helium environment. No photospheric radius expansion is observed, thus leading to an upper limit on the distance to the source of 10 kpc. A lower limit of 6.5 kpc can be also set if it is assumed that emission during the decaying part of the burst involves the whole neutron star surface. Pulsations observed during the burst decay are compatible with being phase locked, and have a similar amplitude, than pre-burst pulsations.

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