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Title:
Feedback through multiple outbursts in the cluster 2A 0335+096
Authors:
Sanders, J. S.; Fabian, A. C.; Taylor, G. B.
Affiliation:
AA(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AC(Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 396, Issue 3, pp. 1449-1459. (MNRAS Homepage)
Publication Date:
07/2009
Origin:
MNRAS
MNRAS Keywords:
galaxies: clusters: individual: 2A 0335+096 , intergalactic medium , X-rays: galaxies
DOI:
10.1111/j.1365-2966.2009.14892.x
Bibliographic Code:
2009MNRAS.396.1449S

Abstract

We examine the core of the X-ray bright galaxy cluster 2A 0335+096 using deep Chandra X-ray imaging and spatially resolved spectroscopy, and include new radio observations. The set of around eight X-ray bright blobs in the core of the cluster, appearing like eggs in a bird's nest, contains multiphase gas from ~0.5 to 2 keV. The morphology of the coolest X-ray emitting gas at 0.5 keV temperature is similar to the Hα emitting nebula known in this cluster, which surrounds the central galaxy. XMM-Newton grating spectra confirm the presence of material at these temperatures, showing reasonable agreement with Chandra emission measures. On scales of 80 to 250 kpc, there is a low temperature, high metallicity, swirl of intracluster medium as seen in other clusters. In the core, we find evidence for a further three X-ray cavities, in addition to the two previously discovered. Enhancements in 1.5 GHz radio emission are correlated with the X-ray cavities. The total 4PV enthalpy associated with the cavities is around 5 × 1059erg. This energy would be enough to heat the cooling region for ~5 × 107yr. We find a maximum pressure discontinuity of 26 per cent (2σ) across the surface brightness edge to the south-west of the cluster core. This corresponds to an upper limit on the Mach number of the cool core with respect to its surroundings of 0.55.
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