Issue |
A&A
Volume 493, Number 1, January I 2009
|
|
---|---|---|
Page(s) | 13 - 21 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:200810138 | |
Published online | 27 October 2008 |
Non-thermal emission in the core of Perseus: results from a long XMM-Newton observation
1
IASF-Milano, INAF, via Bassini 15, 20133 Milano, Italy e-mail: silvano@iasf-milano.inaf.it
2
Dip. di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: fabio.gastaldello@unibo.it
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
Received:
6
May
2008
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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