Volume 462, Number 2, February I 2007
|Page(s)||657 - 666|
|Section||Interstellar and circumstellar matter|
|Published online||13 November 2006|
XMM-Newton and INTEGRAL spectroscopy of the microquasar GRO J1655–40 during its 2005 outburst
Astrophysics Mission Division, Research and Scientific Support Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands e-mail: email@example.com
2 Department of Astronomy, University of Michigan, 500 Church Street, Dennison 814, Ann Arbor, MI 48109, USA
3 Integral Science Operations Centre, Science Operations and Data Systems Division, Research and Scientific Support Department of ESA, ESAC, Apartado 50727, 28080 Madrid, Spain
4 Laboratorio de Astrofísica Espacial y Física Fundamental, INTA, Apartado 50727, 28080 Madrid, Spain
Accepted: 20 October 2006
We report on two simultaneous XMM-Newton and INTEGRAL observations of the microquasar GRO J1655-40during the 2005 outburst when the source was in its high-soft state. The 0.3–200 keV spectra are complex with an overall continuum which may be modeled using an absorbed blackbody together with a weak, steep, power-law component. In addition, there is evidence for the presence of both a relativistically broadened Fe K line and a highly photo-ionized absorber. The photo-ionized absorber is responsible for strong K absorption lines of and in the EPIC pn spectra and blue-shifted ( ± 120 km s-1) and features in the RGS spectra. The parameters of the photo-ionized absorber were different during the two observations with the ionization parameter, , decreasing from 3.60 ± 0.04 to 3.30 ± 0.04 erg cm s-1and the column density decreasing from 1022 atom cm-2to 1022 atom cm-2 during the first and second observations as the 0.5–200 keV GRO J1655-40 luminosity decreased by around a half. At 90% confidence the INTEGRAL data show no evidence of a break in the power-law component up to energies of 380 keV and 90 keV for the first and second observations, respectively.
Key words: X-rays: binaries / accretion, accretion disks / X-rays: individuals: GRO J1655-40
© ESO, 2007
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