Volume 493, Number 1, January I 2009
|Page(s)||13 - 21|
|Section||Cosmology (including clusters of galaxies)|
|Published online||27 October 2008|
Non-thermal emission in the core of Perseus: results from a long XMM-Newton observation
IASF-Milano, INAF, via Bassini 15, 20133 Milano, Italy e-mail: firstname.lastname@example.org
2 Dip. di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: email@example.com
3 INAF, Osservatorio Astronomico di Bologna, via Ranzani 1, Bologna 40127, Italy
4 Department of Physics and Astronomy, University of California at Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
Accepted: 21 July 2008
We employ a long XMM-Newton observation of the core of the Perseus cluster to validate claims of a non-thermal component discovered with Chandra. From a meticulous analysis of our dataset, which includes a detailed treatment of systematic errors, we find the 2–10 keV surface brightness of the non-thermal component to be less than about 5 10-16 erg cm-2 s-1 arcsec-2. The most likely explanation for the discrepancy between the XMM-Newton and Chandra estimates is a problem in the effective area calibration of the latter. Our EPIC-based magnetic field lower limits do not disagree with Faraday rotation measure estimates on a few cool cores and with a minimum energy estimate on Perseus. In the not too distant future Simbol-X may allow detection of non-thermal components with intensities more than 10 times lower than those that can be measured with EPIC; nonetheless even the exquisite sensitivity within reach for Simbol-X might be insufficient to detect the IC emission from Perseus.
Key words: galaxies: clusters: general / galaxies: clusters: individual: Perseus / X-rays: galaxies: clusters
© ESO, 2008
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