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AGN Feedback in the Hot Halo of NGC 4649

Authors
  • Paggi, Alessandro
  • Fabbiano, Giuseppina
  • Kim, Dong-Woo
  • Pellegrini, Silvia
  • Civano, Francesca
  • Strader, Jay
  • Luo, Bin
Type
Preprint
Publication Date
Apr 21, 2014
Submission Date
Apr 21, 2014
Identifiers
arXiv ID: 1404.5315
Source
arXiv
License
Yellow
External links

Abstract

Using the deepest available $\textit{Chandra}$ observations of NGC 4649 we find strong evidences of cavities, ripples and ring like structures in the hot interstellar medium (ISM) that appear to be morphologically related with the central radio emission. These structures show no significant temperature variations in correspondence with higher pressure regions ($0.5\mbox{kpc}<r<3\mbox{kpc}$). On the same spatial scale, a discrepancy between the mass profiles obtained from stellar dynamic and $\textit{Chandra}$ data represents the telltale evidence of a significant non-thermal pressure component in this hot gas, which is related to the radio jet and lobes. On larger scale we find agreement between the mass profile obtained form $\textit{Chandra}$ data and planetary nebulae and globular cluster dynamics. The nucleus of NGC 4649 appears to be extremely radiatively inefficient, with highly sub-Bondi accretion flow. Consistently with this finding, the jet power evaluated from the observed X-ray cavities implies that a small fraction of the accretion power calculated for the Bondi mass accretion rate emerges as kinetic energy. Comparing the jet power to radio and nuclear X-ray luminosity the observed cavities show similar behavior to those of other giant elliptical galaxies.

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