The<i>Herschel</i> view of clusters of galaxies

Edge, A. C.; Oonk, J. B. R.; Mittal, R.

doi:10.1002/asna.201211862

Cited by 3 publications

(3 citation statements)

References 34 publications

(26 reference statements)

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“…Many of them exhibit exceptional properties, with emission in the UV and FIR, as well as H α lines, suggesting the presence of multiphase gas and ongoing star formation (e.g. O'Dea et al 2008, Haarsma et al 2010, Edge et al 2010, O'Dea et al 2010, Liu et al 2012.…”

Section: Introductionmentioning

confidence: 99%

Brightest cluster galaxies in the extended GMRT radio halo cluster sample

Kale

Venturi

Cassano

et al. 2015

A&A

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Aims. First-ranked galaxies in clusters, usually referred to as brightest cluster galaxies (BCGs), show exceptional properties over the whole electromagnetic spectrum. They are the most massive elliptical galaxies and show the highest probability to be radio loud. Moreover, their special location at the centres of galaxy clusters raises the question of the role of the environment in shaping their radio properties. In the attempt to separate the effect of the galaxy mass and of the environment on their statistical radio properties, we investigate the possible dependence of the occurrence of radio loudness and of the fractional radio luminosity function on the dynamical state of the hosting cluster. Methods. We studied the radio properties of the BCGs in the Extended GMRT Radio Halo Survey (EGRHS), which consists of 65 clusters in the redshift range 0.2-0.4, with X-ray luminosity L X ≥ 5 × 10 44 erg s −1 , and quantitative information on their dynamical state from high-quality Chandra imaging. We obtained a statistical sample of 59 BCGs, which we divided into two classes, depending on whether the dynamical state of the host cluster was merging (M) or relaxed (R). Results. Of the 59 BCGs, 28 are radio loud and 31 are radio quiet. The radio-loud sources are favourably located in relaxed clusters (71%), while the reverse is true for the radio-quiet BCGs, which are mostly located in merging systems (81%). The fractional radio luminosity function for the BCGs in merging and relaxed clusters is different, and it is considerably higher for BCGs in relaxed clusters, where the total fraction of radio loudness reaches almost 90%, to be compared to the ∼30% in merging clusters. For relaxed clusters, we found a positive correlation between the radio power of the BCGs and the strength of the cool core, consistent with previous studies on local samples. Conclusions. Our study suggests that the radio loudness of the BCGs strongly depends on the cluster dynamics; their fraction is considerably higher in relaxed clusters. We compare our results with similar investigations and briefly discuss them in the framework of AGN feedback.

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Section: Introductionmentioning

confidence: 99%

Brightest cluster galaxies in the extended GMRT radio halo cluster sample

Kale

Venturi

Cassano

et al. 2015

A&A

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“…Bîrzan et al (2013) and Kapińska & Uttley (2013) relate the feedback to radio observations and Pike et al (2013) look how feedback influences pressure profiles of the ICM. The field has been moving from showing the evidence of feedback to getting a global statistical picture of this effect for an increasing sample of objects and to studies at many wavelengths including also recent observations with ESA's Herschel Infrared Space Observatory, which have been reviewed by Edge et al (2013). The new results show a tight correlation of many features in cool core clusters where the X-ray cooling power, the energy output of the central AGN inferred from the observation of X-ray cavities, optical and infrared line emission, and radio radiation go hand in hand.…”

Section: Thermal Structure Of the Icmmentioning

confidence: 99%

X‐ray galaxy cluster studies for astro‐physics and cosmology

Böhringer

Schartel

2013

Astron Nachr

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The field of research on galaxy clusters has received an enormous increase in attention in the last years, since galaxy clusters have been more and more recognized as very important laboratories for astrophysical studies and observational probes for testing cosmological models. X-ray observations of these largest clearly defined objects in our Universe have been by far the most fruitful approach that has provided us with rich astrophysical and cosmological insights. ESA's XMM-Newton and NASA's Chandra observatories have been the powerhorses of this research. In this article we therefore like to summarize the major advances made in the field of galaxy cluster research primarily by these two instruments. We will touch the progress in understanding the structure of galaxy clusters and its statistics, the AGN feedback processes in the center of clusters, cosmic evolution of clusters, cluster mass measurements, the thermodynamic structure of the intracluster medium and its chemistry, X-ray surveys of clusters, and the use of galaxy clusters for cosmological tests.

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“…Figure 2 shows the "horseshoe", a filament with extensive spectroscopy. X-ray [6], optical [7]; Spitzer [4], Herschel [8], and radio [9] observations reveal a wide range of ionization, from O VII in the X-ray, to low-ionization optical lines (…”

Section: Introductionmentioning

confidence: 99%

Powering the intra-cluster filaments in cool-core clusters of galaxies

Ferland¹

2012

AIP Conference Proceedings

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Abstract. The first radio surveys of the sky discovered that some large clusters of galaxies contained powerful sources of synchrotron emission. Optical images showed that long linear filaments with bizarre emission-line spectra permeated the intra-cluster medium. Recent observations in the infrared and radio show that these filaments have very strong emission lines of molecular hydrogen and carbon monoxide. The mass of molecular material is quite large, the gas is quite warm, and the filaments have not formed stars despite their ~Gyr age. I will discuss the general astrophysical context of large clusters of galaxies and how large masses of molecular gas can be heated to produce what we observe. The unique properties of the filaments are a result of the unique environment. Magnetically confined molecular filaments are surrounded by the hot intra-cluster medium. Thermal particles with keV energies enter atomic and molecular regions and produce a shower of secondary nonthermal electrons. These secondaries collisionally heat, excite, dissociate, and ionize the cool gas. While ionization is dominated by these secondary particles, recombination is controlled by charge exchange, which produces the unusual optical emission line spectrum. I will describe some of the physical processes that are unique to this environment and outline some of the atomic physics issues.

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TheHerschel view of clusters of galaxies

Cited by 3 publications

References 34 publications

Brightest cluster galaxies in the extended GMRT radio halo cluster sample

Brightest cluster galaxies in the extended GMRT radio halo cluster sample

X‐ray galaxy cluster studies for astro‐physics and cosmology

Powering the intra-cluster filaments in cool-core clusters of galaxies

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