A deep Chandra observation of the Perseus cluster: shocks and ripples

Fabian, A. C.; Sanders, J. S.; Allen, S. W.; Crawford, C. S.; Iwasawa, K.; Johnstone, R. M.; Schmidt, R. W.; Taylor, G. B.

doi:10.1046/j.1365-8711.2003.06902.x

Cited by 548 publications

(356 citation statements)

References 47 publications

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“…If this were indeed the case, it would imply that AGN heating is achieved via mechanisms such as weak shocks (e.g., Fabian et al 2003), or buoyant bubbles (e.g., Churazov et al 2001), rather than via catastrophic explosions.…”

Section: Maintaining the Distribution Of Central Entropiesmentioning

confidence: 99%

Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction

Pratt

Arnaud²,

Piffaretti³

et al. 2010

A&A

309

410

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We examine the radial entropy distribution and its scaling using 31 nearby galaxy clusters from the representative XMM-Newton cluster structure survey (REXCESS), a sample in the temperature range 2−9 keV selected in X-ray luminosity only, with no bias toward any particular morphological type. The entropy profiles are robustly measured at least out to R 1000 in all systems and out to R 500 in thirteen systems. Compared to theoretical expectations from non-radiative cosmological simulations, the observed distributions show a radial and mass-dependent excess entropy, such that the excess is greater and extends to larger radii in lower mass systems. At R 500 , the mass dependence and entropy excess are both negligible within the large observational and theoretical uncertainties. Mirroring this behaviour, the scaling of gas entropy is shallower than self-similar in the inner regions, but steepens with radius, becoming consistent with self-similar at R 500 . There is a large dispersion in scaled entropy in the inner regions, apparently linked to the presence of cool cores and dynamical activity; at larger radii the dispersion decreases by approximately a factor of two to 30 per cent, and the dichotomy between subsamples disappears. There are two peaks in the distribution of both inner slope and, after parameterising the profiles with a power law plus constant model, in central entropy K 0 . However, we are unable to distinguish between a bimodal or a left-skewed distribution of K 0 with the present data. The distribution of outer slopes is unimodal with a median value of 0.98, and there is a clear correlation of outer slope with temperature. Renormalising the dimensionless entropy profiles by the gas mass fraction profile f gas (

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Section: Maintaining the Distribution Of Central Entropiesmentioning

confidence: 99%

Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction

Pratt

Arnaud²,

Piffaretti³

et al. 2010

A&A

309

410

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“…X-ray cavities in the emitting gas coincident with radio lobes demonstrate the interplay between the radio activity of BCGs and the slowing or arrest of cooling in cluster centers (Bîrzan et al 2008;Dunn et al 2006). Very deep Chandra observations of the Perseus and Virgo clusters (Fabian et al 2003 detected approximately spherical pressure waves in these clusters. These "ripples" are excited by the expanding radio bubbles and the dissipation of their energy can provide a quasi-continuous heating of the X-ray emitting gas (Ruszkowski et al 2004).…”

Section: Introductionmentioning

confidence: 97%

Parsec-scale properties of brightest cluster galaxies

Liuzzo

Giovannini

Giroletti³

et al. 2010

A&A

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We present new VLBI observations at 5 GHz of a complete sample of brightest cluster galaxies (BCGs) in nearby Abell clusters (distance class <3). Combined with data from the literature, we provide parsec-scale information for 34 BCGs. Our analysis of the parsec-scale radio emission of BCGs and the cluster X-ray properties finds a possible dichotomy between BCGs in cool-core clusters and those in non-cool-core clusters. Among resolved sources, those in cool-core clusters tend to have two-sided parsec-scale jets, while those in less relaxed clusters have predominantly one-sided parsec-scale jets. We suggest that this difference is caused by the interplay between the jets and the surrounding medium. The one-sided structure in non-cool-core clusters may be due to Doppler boosting effects in relativistic, intrinsically symmetric jets whereas two-sided morphology in cool core clusters is probably related to the presence of heavy and mildly relativistic jets that have been decelerated on the parsec-scale. Evidence of recurrent activity is also found in BCGs in cool-core clusters.

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“…Fabian et al 2003;Croton et al 2006). To ascertain the effects of AGN feedback, it is necessary to measure not only the jet power, but also the timescales and frequency of the energy release, i.e.…”

Section: Discussionmentioning

confidence: 99%

An optical spectroscopic survey of the 3CR sample of radio galaxies with z < 0.3

Capetti

Buttiglione

Axon

et al. 2011

A&A

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From an optical spectroscopic survey of 3CR radio galaxies with z < 0.3, we discovered a new spectroscopic class of powerful radioloud AGN. The defining characteristics of these galaxies are that compared with radio galaxies of similar radio luminosity they have: a [O III]/Hβ ratio of ∼0.5, indicative of an extremely low level of gas excitation; a large deficit of [O III] emission; and radio core power. We interpret these objects as relic AGN, i.e. sources that experienced a large drop in their level of nuclear activity, causing a decrease in their nuclear and line luminosity. This class opens a novel approach to investigating lifetimes and duty cycles of AGN.

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A deep Chandra observation of the Perseus cluster: shocks and ripples

Cited by 548 publications

References 47 publications

Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction

Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction

Parsec-scale properties of brightest cluster galaxies

An optical spectroscopic survey of the 3CR sample of radio galaxies with z < 0.3

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