Issue |
A&A
Volume 493, Number 2, January II 2009
|
|
---|---|---|
Page(s) | 409 - 424 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:200810225 | |
Published online | 20 November 2008 |
Chemical enrichment in the cluster of galaxies Hydra A
1
Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstr, 85748, Garching, Germany e-mail: aurora@mpe.mpg.de
2
SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
3
University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA
4
Jacobs University Bremen, Campus Ring 1, 28759 Bremen, Germany
5
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
Received:
20
May
2008
Accepted:
3
November
2008
We analyzed global properties, radial profiles, and 2D maps of the metal abundances and temperature in the cool core cluster of galaxies Hydra A using a deep ~120 ks XMM-Newton exposure.
The best fit among the available spectral models is provided by a Gaussian distribution of the emission measure (gdem).
We can accurately determine abundances for 7 elements in the cluster core with EPIC (O, Si, S, Ar, Ca, Fe, Ni) and 3 elements (O, Ne, Fe) with RGS.
The gdem model gives lower Fe abundances than a single-temperature model. Based on this, we explain why simulations show that the best-fit Fe abundance in clusters with intermediate temperatures is overestimated.
The abundance profiles for Fe, Si, S, but also O are centrally peaked. Combining the Hydra A results with 5 other clusters for which detailed chemical abundance studies are available, we find a significant decrease in O with radius, while the increase in the O/Fe ratio with radius is small within 0.1 r200, where the O abundances can be accurately determined, with d.
We compare the observed abundance ratios with the mixing of various supernova
type Ia and core-collapse yield models in different relative amounts.
Producing the estimated O, Si, and S peaks in Hydra A requires either the amount of metals ejected by stellar winds to be 3–8 times higher than predicted by available models or the initial enrichment by core-collapse supernovae in the protocluster phase not to be as well mixed on large scales as previously thought.
The temperature map shows cooler gas extending in arm-like structures towards the north and south. These structures, and especially the northern one, appear to be richer in metals than the ambient medium and spatially correlated with the large-scale radio lobes.
With different sets of assumptions, we estimate the mass of cool gas, which was probably uplifted by buoyant bubbles of relativistic plasma produced by the AGN, to
, and the energy associated with this uplift to
erg. The best estimate of the mass of Fe uplifted together with the cool gas is
, 15% of the total mass of Fe in the central 0.5′ region.
Key words: X-rays: galaxies: clusters / galaxies: clusters: individual: Hydra A / galaxies: abundances / galaxies: cooling flows / galaxies: intergalactic medium
© ESO, 2009
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