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Title:
Cool X-ray emitting gas in the core of the Centaurus cluster of galaxies
Authors:
Sanders, J. S.; Fabian, A. C.; Allen, S. W.; Morris, R. G.; Graham, J.; Johnstone, R. M.
Affiliation:
AA(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AC(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305-4060, USA), AD(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305-4060, USA), AE(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AF(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 385, Issue 3, pp. 1186-1200. (MNRAS Homepage)
Publication Date:
04/2008
Origin:
MNRAS
MNRAS Keywords:
X-rays: galaxies , galaxies: clusters: individual: Centaurus , intergalactic medium , cooling flows
DOI:
10.1111/j.1365-2966.2008.12952.x
Bibliographic Code:
2008MNRAS.385.1186S

Abstract

We use a deep XMM-Newton Reflection Grating Spectrometer observation to examine the X-ray emission from the core of the Centaurus cluster of galaxies. We clearly detect FeXVII emission at four separate wavelengths, indicating the presence of cool X-ray emitting gas in the core of the cluster. Fe ions from FeXVII toXXIV are observed. The ratio of the FeXVII 17.1 Å lines to 15.0 Å line and limits on OVII emission indicate a lowest detected temperature in the emitting region of 0.3 to 0.45 keV (3.5 to 5.2 × 106 K). The cluster also exhibits strong NVII emission, making it apparent that the N abundance is supersolar in its very central regions. Comparison of the strength of the FeXVII lines with a solar metallicity cooling flow model in the inner 17 kpc radius gives mass deposition rates in the absence of heating of 1.6-3Msolaryr-1. Spectral fitting implies an upper limit of 0.8 Msolaryr-1 below 0.4 keV, 4 Msolaryr-1 below 0.8 keV and 8 Msolar yr-1 below 1.6 keV. The cluster contains X-ray emitting gas over at least the range of 0.35 to 3.7 keV, a factor of more than 10 in temperature. We find that the best-fitting metallicity of the cooler components is smaller than the hotter ones, confirming that the apparent metallicity does decline within the inner 1 arcmin radius.
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