A High‐Resolution Study of the Hydra A Cluster with<i>Chandra</i>: Comparison of the Core Mass Distribution with Theoretical Predictions and Evidence for Feedback in the Cooling Flow

David, L. P.; Nulsen, P. E. J.; McNamara, B. R.; Forman, W.; Jones, C.; Ponman, T. J.; Robertson, Brant; Wise, Michael

doi:10.1086/322250

Cited by 273 publications

(411 citation statements)

References 58 publications

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“…As we can see, this value is very similar to the power output from the radio source, which implies that the energy produced by the radio source is sufficient to offset the cooling flow. A similar result has been found for many other clusters with radio bubbles (e.g., David et al 2001;Blanton et al 2003;Bîrzan et al 2004). Using the parameters from the best-fitting single-temperature model of the spectrum of the northern shell, we determined the isobaric cooling time of the shell.…”

Section: X-ray/ Radio Interactions In the Cluster Coresupporting

confidence: 74%

ChandraObservation of the Interaction of the Radio Source and Cooling Core in Abell 2063

Kanov

Sarazin

Hicks

2006

ApJ

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We present the results of a Chandra observation of the cooling core cluster Abell 2063. Spectral analysis shows that there is cool gas (2 keV ) associated with the cluster core, which is more than a factor of 2 cooler than the outer cluster gas (4.1 keV). There also is spectral evidence for a weak cooling flow,Ṁ % 20 M yr À1 . The cluster exhibits a complex structure in the center that consists of several bright knots of emission, a depression in the emission to the north of the center of the cluster, and a shell of emission surrounding it. The depression in the X-ray emission is coincident with the position of the northeastern radio lobe of the radio source associated with the cluster central galaxy. The shell surrounding this region appears to be hotter, which may be the result of a shock that has been driven into the gas by the radio source. The power output of the radio source appears to be sufficient to offset the cooling flow, and heating of the gas through shocks is a possible explanation of how the energy transfer is established.

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Section: X-ray/ Radio Interactions In the Cluster Coresupporting

confidence: 74%

ChandraObservation of the Interaction of the Radio Source and Cooling Core in Abell 2063

Kanov

Sarazin

Hicks

2006

ApJ

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“…The central electron density is n e ð0Þ ¼ 0:08 cm À3 , and the temperature is T in ¼ 3:11 keV at the center and Tð190 kpcÞ ¼ 4:04 keV at 190 kpc. In Figure 5 we show the temperature profile as inferred from Chandra observations (David et al 2001) together with our best fit for f ¼ 0:5 (L ¼ 4:0 Â 10 45 ergs s À1 ). As is readily seen, the inclusion of the heating term produces a good fit to the data without having to invoke an abnormally high conductivity.…”

Section: Resultsmentioning

confidence: 99%

Equilibrium Models of Galaxy Clusters with Cooling, Heating, and Conduction

Brüggen

2003

ApJ

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It is generally argued that most clusters of galaxies host cooling flows in which radiative cooling in the center causes a slow inflow. However, recent observations by Chandra and XMM conflict with the predicted cooling flow rates. Among other mechanisms, heating by a central active galactic nucleus and thermal conduction have been invoked in order to account for the small mass deposition rates. Here we present a family of hydrostatic models for the intracluster medium where radiative losses are exactly balanced by thermal conduction and heating by a central source. We describe the features of this simple model and fit its parameters to the density and temperature profiles of Hydra A.

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“…If this cooled gas fuels a nuclear outburst that deposits energy close to the nucleus, the presence of the dense disk would channel the energy and produce shocks like those observed in NGC 4636. Thus, NGC 4636 appears to demonstrate the energy feedback process invoked to prevent the deposition of large quantities of cooled gas in the centers of galaxies and clusters (Tabor & Binney 1993;Churazov et al 2001;David et al 2001) as well as generate AGN cycles (e.g., Ciotti & Ostriker 1997). In a galaxy with the X-ray luminosity of NGC 4636, outbursts would need to occur every ∼ yr to prevent the accumulation of a significant 7 5 # 10 amount of cooled gas.…”

Section: Discussionmentioning

confidence: 99%

Chandra Observations of NGC 4636--an Elliptical Galaxy in Turmoil

Jones

Forman

Vikhlinin

et al. 2002

ApJ

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176

175

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Chandra images show symmetric, 8 kpc long, armlike features in the X-ray halo surrounding NGC 4636. The leading edges of these features are sharp and are accompanied by temperature increases of ∼30%. These properties suggest that the armlike structures are produced by shocks, driven by symmetric off-center outbursts. We interpret these observations as part of a cycle in which the cooling gas originally fueled a nuclear outburst about 3 # yr ago that led to shocks reheating the cooling gas and thus preventing the accumulation of significant 6 10 amounts of cooled gas in the galaxy center and temporarily starving the central active galactic nucleus.

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A High‐Resolution Study of the Hydra A Cluster withChandra: Comparison of the Core Mass Distribution with Theoretical Predictions and Evidence for Feedback in the Cooling Flow

Cited by 273 publications

References 58 publications

ChandraObservation of the Interaction of the Radio Source and Cooling Core in Abell 2063

ChandraObservation of the Interaction of the Radio Source and Cooling Core in Abell 2063

Equilibrium Models of Galaxy Clusters with Cooling, Heating, and Conduction

Chandra Observations of NGC 4636--an Elliptical Galaxy in Turmoil

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