[ITAL]Chandra[/ITAL] Observation of the Radio Source/X-Ray Gas Interaction in the Cooling Flow Cluster Abell 2052

Blanton, E. L.; Sarazin, Craig L.; McNamara, B. R.; Wise, Michael

doi:10.1086/323269

Cited by 263 publications

(297 citation statements)

References 16 publications

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“…In the densest central region with high cooling rate, the hot gas atmosphere continues to loose energy in the form of radiation (mostly in X-rays). The inferred short radiative cooling time towards (or at) the centre (shorter than the age of the cluster) indicates that the gas located at the centre cools faster than the gas in the outer part of the cluster and hence gas flows towards the core to maintain hydrostatic equilibrium (Fabian 1994;Blanton et al 2001a). The excess gas in the central region of the cluster subsonically flows towards the core and leads to the for-studies of cool core clusters using Chandra and XMM-Newton observatories revealed that the interaction of radio jets originating from the core of the cluster with the ICM results in formation of cavities, shocks, ripples etc.…”

Section: Introductionmentioning

confidence: 99%

Detection of a pair of prominent X-ray cavities in Abell 3847

Vagshette

Naik

Patil

et al. 2016

Mon. Not. R. Astron. Soc.

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We present results obtained from a detailed analysis of a deep Chandra observation of the bright FRII radio galaxy 3C 444 in Abell 3847 cluster. A pair of huge X-ray cavities are detected along North and South directions from the centre of 3C 444. X-ray and radio images of the cluster reveal peculiar positioning of the cavities and radio bubbles. The radio lobes and X-ray cavities are apparently not spatially coincident and exhibit offsets by ∼ 61 kpc and 77 kpc from each other along the North and South directions, respectively. Radial temperature and density profiles reveal the presence of a cool core in the cluster. Imaging and spectral studies showed the removal of substantial amount of matter from the core of the cluster by the radio jets. A detailed analysis of the temperature and density profiles showed the presence of a rarely detected elliptical shock in the cluster. Detection of inflating cavities at an average distance of ∼ 55 kpc from the centre implies that the central engine feeds a remarkable amount of radio power (∼6.3 ×10 44 erg s −1 ) into the intra-cluster medium over ∼ 10 8 yr, the estimated age of cavity. The cooling luminosity of the cluster was estimated to be ∼ 8.30 × 10 43 erg s −1 , which confirms that the AGN power is sufficient to quench the cooling. Ratios of mass accretion rate to Eddington and Bondi rates were estimated to be ∼ 0.08 and 3.5 × 10 4 , respectively. This indicates that the black hole in the core of the cluster accretes matter through chaotic cold accretion.

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Section: Introductionmentioning

confidence: 99%

Detection of a pair of prominent X-ray cavities in Abell 3847

Vagshette

Naik

Patil

et al. 2016

Mon. Not. R. Astron. Soc.

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“…By examining the density profiles of two clusters, Abell 2052 ( fig. 2 of Blanton et al 2001), and Hydra A ( fig. 3 of David et al 2001), I find that condition (9) for instability at the outermost segment of the shell is fulfilled under the following conditions.…”

Section: Clustersmentioning

confidence: 96%

Bubbles in planetary nebulae and clusters of galaxies: instabilities at bubble’ fronts

Soker¹

2004

New Astronomy

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“…Finally, less gas cools to low temperatures at the centers of cool core clusters, groups, and individual ellipticals than expected unless something heats the gas, and AGNs are the leading candidates. In cool core clusters, X-ray deficits ("radio bubbles") have been found at the locations of the lobes of the radio sources associated with the brightest cluster galaxies (BCGs; Fabian et al 2006;Blanton et al 2001); similar radio bubbles are seen in groups and individual elliptical galaxies. "Ghost bubbles"' at larger radii are also seen which lack high frequency radio emission.…”

Section: Agn Feedback In Early-type Galaxiesmentioning

confidence: 99%

Feedback and environmental effects in elliptical galaxies

Sarazin¹

2009

Proc. IAU

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Abstract. The role of the environment of an elliptical galaxy on its hot interstellar gas is discussed. In general, the X-ray halos of early-type galaxies tend to be smaller and fainter in denser environments, with the exception of group-central galaxies. X-ray observations show many examples of nearby galaxies which are undergoing gas stripping. On the other hand, most bright galaxies in clusters do manage to retain small coronae of X-ray emission. Recent theoretical and observational results on the role of feedback from AGN at the centers of elliptical galaxies on their interstellar gas are reviewed. X-ray observations show many examples of X-ray holes in the central regions of brightest-cluster galaxies; in many cases, the X-ray holes are filled with radio lobes. Similar radio bubbles are seen in groups and individual early-type galaxies. "Ghost bubbles" are often seen at larger radii in clusters and galaxies; these bubbles are faint in high radio frequencies, and are believed to be old radio bubbles which have risen buoyantly in the hot gas. Low frequency radio observations show that many of the ghost bubbles have radio emission; in general, these long wavelength observations show that radio sources are much larger and involve greater energies than had been previously thought. The radio bubbles can be used to estimate the total energy output of the radio jets. The total energies deposited by radio jets exceed the losses from the gas due to radiative cooling, indicating that radio sources are energetically capable of heating the cooling core gas and preventing rapid cooling.

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[ITAL]Chandra[/ITAL] Observation of the Radio Source/X-Ray Gas Interaction in the Cooling Flow Cluster Abell 2052

Cited by 263 publications

References 16 publications

Detection of a pair of prominent X-ray cavities in Abell 3847

Detection of a pair of prominent X-ray cavities in Abell 3847

Bubbles in planetary nebulae and clusters of galaxies: instabilities at bubble’ fronts

Feedback and environmental effects in elliptical galaxies

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