The Luminosity-Temperature Relation for Groups and Clusters of Galaxies

Cavaliere, A.; Menci, Nicola; Tozzi, P.

doi:10.1086/310767

Cited by 110 publications

(130 citation statements)

References 26 publications

(41 reference statements)

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“…10 for a non-evolving cluster population, and that 0 & 0:1 if the cluster population evolves with 1 n 1. Similar conclusions can bedrawn from the results given by Cavaliere et al (1991).…”

Section: Contributions To the Cmbr Spectrumsupporting

confidence: 85%

The Sunyaev–Zel'dovich effect

1999

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The Sunyaev-Zel'dovich e ect causes a change in the apparent brightness of the Cosmic Microwave Background Radiation towards a cluster of galaxies or any other reservoir of hot plasma. Measurements of the e ect provide distinctly di erent information about cluster properties than X-ray imaging data, while combining X-ray and Sunyaev-Zel'dovich e ect data leads to new insights into the structures of cluster atmospheres. The e ect is redshift-independent, and so provides a unique probe of the structure of the Universe on the largest scales. The present review discusses the theory of the Sunyaev-Zel'dovich e ect and collects published results for many clusters, presents the overall conclusions that may bedrawn from the detections so far, and discusses the prospects for future research on the Sunyaev-Zel'dovich e ects.Subject headings: Sunyaev-Zel'dovich E ect; Clusters; Microwave Background Radiation Astrophysical ContextCompton scattering is one of the major physical processes that couples matter and radiation. Its importance is often stressed in highly relativistic environments where large energy transfers occur: for example, in the synchrotron self-Compton process that may beresponsible for much of the X-radiation from active galactic nuclei (e.g., Fabian et al. 1986). However, the Compton process also has observable consequences in low-energy environments, where small energy transfers occur. The Sunyaev-Zel'dovich e ect, which arises from the scattering of electrons in clusters of galaxies on the cosmic microwave 1 Also Smithsonian Institution Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA { 2 { background radiation eld, is perhaps the most important astrophysical example. The e ect provides a cosmological probe, it has been used to measure the properties of gas in clusters of galaxies, and it has been discussed as a means of measuring the motions of clusters of galaxies and hence studying the evolution of structure in the Universe.The purpose of this review is to provide a comprehensive introduction to the SunyaevZel'dovich e ect. I aim to provide both a theoretical treatment that can befollowed by non-specialists, and an introduction to the observation of the e ect with a critical review of data in the literature. The latter is more di cult today than it would have been ve years ago because of the rapid increase in the number of papers on the Sunyaev-Zel'dovich e ect, and the improvement i n t h e quality o f t h e results that are being gained.

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“…10 for a non-evolving cluster population, and that 0 & 0:1 if the cluster population evolves with 1 n 1. Similar conclusions can bedrawn from the results given by Cavaliere et al (1991).…”

Section: Contributions To the Cmbr Spectrumsupporting

confidence: 85%

The Sunyaev–Zel'dovich effect

1999

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“…1 of Xue & Wu 2000). Whether the high temperature of source 6 is due to pointsource contamination or nongravitational heating mechanisms, such as star formation from individual group members or shock heating of the infalling gas (e.g., Metzler & Evrard 1994;Ponman et al 1996;Cavaliere, Menci, & Tozzi 1997), cannot be resolved with our current X-ray data.…”

Section: Basic Nature Of the Extended X-ray Sourcesmentioning

confidence: 84%

The Chandra Deep Field North Survey. IX. Extended X-Ray Sources

Bauer¹,

Alexander²,

Brandt³

et al. 2002

The Astronomical Journal

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The %1 Ms Chandra Deep Field North observation is used to study the extended X-ray sources in the region surrounding the Hubble Deep Field North (HDF-N), yielding the most sensitive probe of extended X-ray emission at cosmological distances to date. A total of six such sources are detected, the majority of which align with small numbers of optically bright galaxies. Their angular sizes, band ratios, and X-ray luminosities-assuming they lie at the same distances as the galaxies coincident with the X-ray emission-are generally consistent with the properties found for nearby groups of galaxies. One source is notably different and is likely to be a poor-to-moderate X-ray cluster at high redshift (i.e., z & 0.7). This source has a large angular extent, a double-peaked X-ray morphology, and an overdensity of unusual objects [very red objects, optically faint (I ! 24) radio and X-ray sources]. Another of the six sources is coincident with several z % 1.01 galaxies located within the HDF-N itself, including the FR I radio galaxy VLA J123644+621133, and is likely to be a group or poor cluster of galaxies at that redshift. We are also able to place strong constraints on the optically detected cluster of galaxies ClG 1236+6215 at z = 0.85 and the wide-angle-tailed radio galaxy VLA J123725+621128 at z $ 1-2; both sources are expected to have considerable associated diffuse X-ray emission, and yet they have rest-frame 0.5-2.0 keV X-ray luminosities of .3 Â 10 42 and .(3-15) Â 10 42 ergs s À1 , respectively. The environments of both sources are either likely to have a significant deficit of hot intracluster gas compared with local clusters of galaxies, or they are X-ray groups. We find the surface density of extended X-ray sources in this observation to be 167 þ97 À67 deg À2 at a limiting soft-band flux of %3 Â 10 À16 ergs cm À2 s À1 . No evolution in the X-ray luminosity function of clusters is needed to explain this value.

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“…This nongravitational heating would decrease the central density and, because the X-ray emissivity is proportional to the density squared, reduce the luminosity. Because of the lower pressures in smaller clusters and groups, this would preferentially affect them, steepening the relation (Cavaliere, Menci, & Tozzi 1997). This view-L -T X point was strengthened by the discovery of an apparent entropy "floor" in the centers of groups and clusters (Ponman, Cannon, & Navarro 1999).…”

Section: Introductionmentioning

confidence: 99%

“…This is consistent with the idea of a source of heat that raises the entropy of the gas to a fixed, minimum level; smaller clusters have lower entropies and so are more affected than large clusters. This model has been developed in some detail in a number of papers (Balogh, Babul, & Patton 1999;Loewenstein 2000;Wu, Fabian, & Nulsen 1999;Cavaliere, Menci, & Tozzi 1999;Valageas & Silk 1999) and appears to be capable of explaining the observations naturally.…”

Section: Introductionmentioning

confidence: 99%

Explaining the Entropy Excess in Clusters and Groups of Galaxies without Additional Heating

Bryan¹

2000

The Astrophysical Journal

138

172

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The X-ray luminosity and temperature of clusters and groups of galaxies do not scale in a self-similar manner. This has often been interpreted as a sign that the intracluster medium has been substantially heated by nongravitational sources. In this Letter, we propose a simple model that instead uses the properties of galaxy formation to explain the available observations. Drawing on available observations, we show that there is evidence that the efficiency of galaxy formation was higher in groups than in clusters. If confirmed, this would deplete the low-entropy gas in groups, increase their central entropy, and decrease their X-ray luminosity. A simple, empirical, hydrostatic model appears to match both the luminosity-temperature relation of clusters and the properties of their internal structure.

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The Luminosity-Temperature Relation for Groups and Clusters of Galaxies

Cited by 110 publications

References 26 publications

The Sunyaev–Zel'dovich effect

The Sunyaev–Zel'dovich effect

The Chandra Deep Field North Survey. IX. Extended X-Ray Sources

Explaining the Entropy Excess in Clusters and Groups of Galaxies without Additional Heating

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