Issue |
A&A
Volume 462, Number 2, February I 2007
|
|
---|---|---|
Page(s) | 657 - 666 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20065406 | |
Published online | 13 November 2006 |
XMM-Newton and INTEGRAL spectroscopy of the microquasar GRO J1655–40 during its 2005 outburst
1
Astrophysics Mission Division, Research and Scientific Support Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands e-mail: mdiaz@sciops.esa.int
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
Received:
11
April
2006
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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