X-ray sources in clusters of galaxies

McHardy, I. M.

doi:10.1093/mnras/184.4.783

Cited by 26 publications

(15 citation statements)

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“…This confirms previous results that found similar trends between morphological fractions and L X (Bahcall 1977, McHardy 1978, Edge & Stewart 1991. We note that our correlations are less steep with L X than in these previous works, possibly due to the fact that we limit our analysis to a fixed fraction of R 200 , while previous studies included all galaxies within a plate field-of-view.…”

Section: Trends With X-ray Luminositysupporting

confidence: 93%

The Evolution of Spiral, S0, and Elliptical Galaxies in Clusters

Poggianti

Fasano

Bettoni

et al. 2009

ApJ

125

155

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We quantify the evolution of the spiral, S0 and elliptical fractions in galaxy clusters as a function of cluster velocity dispersion (σ) and X-ray luminosity (L X ) using a new database of 72 nearby clusters from the WIde-Field Nearby Galaxy-cluster Survey (WINGS) combined with literature data at z = 0.5 − 1.2. Most WINGS clusters have σ between 500 and 1100 km s −1 , and L X between 0.2 and 5 × 10 44 erg/s. The S0 fraction in clusters is known to increase with time at the expense of the spiral population. We find that the spiral and S0 fractions have evolved more strongly in lower σ, less massive clusters, while we confirm that the proportion of ellipticals has remained unchanged. Our results demonstrate that morphological evolution since z = 1 is not confined to massive clusters, but is actually more pronounced in low mass clusters, and therefore must originate either from secular (intrinsic) evolution and/or from environmental mechanisms that act preferentially in lowmass environments, or both in low-and high-mass systems. We also find that the evolution of the spiral fraction perfectly mirrors the evolution of the fraction of star-forming galaxies. Interestingly, at low-z the spiral fraction anticorrelates with L X . Conversely, no correlation is observed with σ. Given that both σ and L X are tracers of the cluster mass, these results pose a challenge for current scenarios of morphological evolution in clusters.

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Section: Trends With X-ray Luminositysupporting

confidence: 93%

The Evolution of Spiral, S0, and Elliptical Galaxies in Clusters

Poggianti

Fasano

Bettoni

et al. 2009

ApJ

125

155

View full text Add to dashboard Cite

show abstract

“…3). Edge & Stewart (1991) investigate observational data of nearby clusters and (z [ 0.1) found that the spiral fraction decreases and the S0 fraction increases with the X-ray temperature and luminosity (see also Bahcall 1977 ;McHardy 1978). The clusters with high X-ray temperature and luminosity are generally massive ones (see, e.g., Horner et al 1999).…”

Section: Discussionmentioning

confidence: 95%

Ram‐Pressure Stripping of Galaxies in High‐Redshift Clusters and the Influence of Intracluster Medium Heating

Fujita¹

2001

ApJ

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We have investigated the ram-pressure stripping of disk galaxies in clusters at various redshifts and in cluster progenitors ; the clusters are formed via a hierarchical clustering scenario. We consider a radially infalling galaxy whose initial position and velocity are given by a spherical collapse model of structure formation. Moreover, since observations show that the intracluster medium (ICM) of nearby clusters is nongravitationally heated, we study the e †ect of the nongravitational heating on the ram-pressure stripping. For a given redshift, we Ðnd that ram-pressure stripping has more inÑuence on galaxies in more massive clusters. On the other hand, for a given mass, it has more inÑuence on galaxies in clusters at higher redshifts. In particular, we predict that in rich clusters at most of the galaxies are a †ected z Z 1, by ram-pressure stripping. While the nongravitational heating signiÐcantly reduces the inÑuence of rampressure stripping on galaxies in clusters with a mass smaller than (1È5) ] 1013 it does not a †ect M _ , the inÑuence in richer clusters. If the ICM is heated nongravitationally at z ? 1, ram-pressure stripping does not occur at z D 1È2 in the progenitors of clusters observed at because the heat makes 0 [ z [ 0.5 the ICM fraction of the cluster progenitors small. On the other hand, if the ICM is heated nongravitationally at z D 0 for the Ðrst time, the ram-pressure stripping occurs even at z D 3. We compare the results with the observations of galaxies in clusters at various redshifts.

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“…Conclusions range from the cluster morphology having equal importance (DFJ99; Bahcall 1977) in determining L X to only a very weak dependence (Johnson et al 1983;Jones & Forman 1978). In common to these studies, however, is the finding that the early-type cluster morphologies (BM type I, I-II and RS type cD, B) may have an independent influence on the luminosity, presumably because of the presence of a cD-like galaxy and correspondingly deeper gravitational potential (McHardy 1978). McHardy found, however, that cD-like galaxies in poorer clusters (such as Albert, White, & Morgan 1977, Morgan, Kayser, & White 1975, and White 1978 have a much lower probability of X-ray emission as compared with Bautz-Morgan type I Abell clusters.…”

Section: Detection Statistics and Optical Cluster Propertiesmentioning

confidence: 96%

The X-Ray Properties of Nearby Abell Clusters from theROSATAll-Sky Survey: The Sample and Correlations with Optical Properties

et al. 2003

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We present an analysis of the X-ray emission for a complete sample of 288 Abell clusters spanning the redshift range 0:016 z 0:09 from the ROSAT All-Sky Survey. This sample is based on our 20 cm VLA survey of nearby Abell clusters. We find an X-ray detection rate of 83%. We report cluster X-ray fluxes and luminosities and two different flux ratios indicative of the concentration and extent of the emission. We examine correlations between the X-ray luminosity, Abell richness, and Bautz-Morgan and Rood-Sastry cluster morphologies. We find a strong correlation between L X and cluster richness coupled with a dependence on the optical morphological type. These results are consistent with the observed scatter between X-ray luminosity and temperature and a large fraction of cooling flows. For each cluster field, we also report the positions, peak X-ray fluxes, and flux ratios of all X-ray peaks above 3 significance within a box of 2 Â 2 h À1 75 Mpc centered on Abell's position.

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X-ray sources in clusters of galaxies

Cited by 26 publications

References 0 publications

The Evolution of Spiral, S0, and Elliptical Galaxies in Clusters

The Evolution of Spiral, S0, and Elliptical Galaxies in Clusters

Ram‐Pressure Stripping of Galaxies in High‐Redshift Clusters and the Influence of Intracluster Medium Heating

The X-Ray Properties of Nearby Abell Clusters from theROSATAll-Sky Survey: The Sample and Correlations with Optical Properties

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