Radio Observations of NGC1275 at 90 and 20cm

Pedlar, A.; Ghataure, H.; Davies, R. D.; Harrison, B.; Perley, R. A.; Crane, P. C.

doi:10.1007/978-94-009-2953-1_17

Cited by 116 publications

(183 citation statements)

References 11 publications

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“…Perseus (Pedlar et al 1990;Burns et al 1992), A2199 (Owen & Eilek 1998), A133, A2052, A2626 (Rizza et al 2000;Zhao et al 1993), the scenario described above for M 87 should apply similarly to these cooling flow clusters.…”

Section: Heating Modelmentioning

confidence: 94%

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The new emerging model for the structure of cooling cores in clusters of galaxies

Böhringer

Matsushita

Churazov

et al. 2002

A&A

173

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Abstract. New X-ray observations with XMM-Newton show a lack of spectral evidence for large amounts of cooling and condensing gas in the centers of galaxy clusters believed to harbour strong cooling flows. This paper re-explores the cooling flow scenario in the light of the new observations. We explore the diagnostics of the temperature structure of cooling cores with XMM-spectroscopy, tests for intracluster X-ray absorption towards central AGN, the effect of metal abundance inhomogeneities, and the implications of high resolution images in the centers of clusters. We find no evidence of intrinsic absorption in the center of the cooling flows of M 87 and the Perseus cluster. We further consider the effect of cluster rotation in cooling flow regions in the frame of cosmic structure evolution models. Also, the heating of the core regions of clusters by jets from a central AGN is reconsidered. We find that the power of the AGN jets as estimated by their interaction effects with the intracluster medium in several examples is more then sufficient to heat the cooling flows and to reduce the mass deposition rates. We explore in more detail which requirements such a heating model has to fulfill to be consistent with all observations, point out the way such a model could be constructed, and argue that such model building seems to be successful. In summary, it is argued that most observational evidence points towards much lower mass deposition rates than previously inferred in the central region of clusters thought to contain strong cooling flows.

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Section: Heating Modelmentioning

confidence: 94%

“…Pedlar et al 1990;Tabor & Binney 1993;McNamara et al 2000;Soker et al 2001); -heating by heat conduction from the hotter gas outside the cooling flow (e.g. Tucker & Rosner 1983;Bertschinger & Meiksin 1986); -heating by magnetic fields, basically through some form of reconnection (e.g.…”

Section: Heating Modelmentioning

confidence: 99%

The new emerging model for the structure of cooling cores in clusters of galaxies

Böhringer

Matsushita

Churazov

et al. 2002

A&A

173

171

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“…As one of the brightest compact radio sources in the sky, 3C 84 has been studied in some detail (Vermeulen et al 1994;Taylor & Vermeulen 1996;Silver et al 1998;Walker et al 2000). The radio source 3C 84 is well known to contain jets which have been studied on a variety of scales (Pedlar et al 1990;Dhawan et al 1998;Silver et al 1998;Walker et al 2000). Taylor et al (2006a) detect linear polarization from the bright jet component S1 in 3C 84 at 5, 8, 15, and 22 GHz at a level of 0.8 to 7.5% that increases with frequency.…”

Section: Notes On Individual Sourcesmentioning

confidence: 99%

“…At lower frequency and resolution, there is a clear equivalence between the parsec-scale structure and jets on a kiloparsec scale (Pedlar et al 1990). Looking through VLBA images from 22 GHz to 5 GHz, the two-sided structure starts out appearing more symmetric and then at lower frequencies it becomes asymmetric.…”

Section: Notes On Individual Sourcesmentioning

confidence: 99%

“…Their radio morphology often also shows evidence of a strong interaction with the surrounding medium: some BCGs have a wide angle tail structure (WAT) that is either extended on the kiloparsec-scale (e.g., 3C 465 in A2634, Sakelliou & Merrifield 1999), or of small size (e.g. NGC 4874 in Coma cluster, Feretti & Giovannini 1985); others are diffuse and amorphous sources, either extended (3C 84 in Perseus, Pedlar et al 1990) or of small size (e.g., the BCG in A154, ). These last two sources are rare in the general radio population, but frequently present in BCGs and in particular in BCGs located in cooling core clusters of galaxies.…”

Section: Introductionmentioning

confidence: 99%

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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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The Formation of Dark Matter in Cooling Flows

Fabian

1990

Baryonic Dark Matter

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Radio Observations of NGC1275 at 90 and 20cm

Cited by 116 publications

References 11 publications

The new emerging model for the structure of cooling cores in clusters of galaxies

The new emerging model for the structure of cooling cores in clusters of galaxies

Parsec-scale properties of brightest cluster galaxies

The Formation of Dark Matter in Cooling Flows

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