Volume 508, Number 3, December IV 2009
|Page(s)||1161 - 1171|
|Section||Cosmology (including clusters of galaxies)|
|Published online||21 October 2009|
XMM-Newton and INTEGRAL analysis of the Ophiuchus cluster of galaxies
Observatory, University of Helsinki, Finland e-mail: Jukka.H.Nevalainen@helsinki.fi
2 ISDC Data Centre for Astrophysics, Geneva Observatory, University of Geneva, Switzerland
3 SRON Netherlands Institute for Space Research, The Netherlands
4 University of Alabama in Huntsville, Huntsville, USA; NASA National Space and Technology Center, Huntsville, USA
Accepted: 7 October 2009
Aims. We investigated the non-thermal hard X-ray emission in the Ophiuchus cluster of galaxies. Our aim is to characterise the physical properties of the non-thermal component and its interaction with the cosmic microwave background.
Methods. We performed spatially resolved spectroscopy and imaging using XMM-Newton data to model the thermal emission. Combining this with INTEGRAL ISGRI data, we modelled the 0.6-140 keV band total emission in the central 7 arcmin region.
Results. The models that best describe both PN and ISGRI data contain a power-law component with a photon index in a range 2.2-2.5. This component produces ~10% of the total flux in the 1-10 keV band. The pressure of the non-thermal electrons is ~1% of that of the thermal electrons. Our results support the scenario whereby a relativistic electron population, which produces the recently detected radio mini-halo in Ophiuchus, also produces the hard X-rays via inverse compton scattering of the CMB photons. The best-fit models imply a differential momentum spectrum of the relativistic electrons with a slope of 3.4-4.0 and a magnetic field strength μG. The lack of evidence for a recent major merger in the Ophiuchus centre allows the possibility that the relativistic electrons are produced by turbulence or hadronic collisions.
Key words: galaxies: clusters: individual: Ophiuchus / X-rays: galaxies: clusters / techniques: spectroscopic
© ESO, 2009
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