Properties of nearby clusters of galaxies

Флин, П.; Krywult, J.; Trèvese, D.; Cirimele, G.; Hickson, Paul

doi:10.1051/aas:2000363

Cited by 13 publications

(16 citation statements)

References 10 publications

(14 reference statements)

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“…This cluster exhibits very clumpy, elongated X-ray emission, and a strong X-ray centroid shift (Bliton et al 1998). This elongation is also present in the galaxy distribution, which shows a definite ellipticity, oriented mainly E − W (Flin et al 1995). The BCG of the main condensation, IC 712, has a WAT structure of very small linear size (∼4.6 kpc) with a total flux density at 1.4 GHz of 26.3 mJy .…”

Section: Notes On Individual Sourcesmentioning

confidence: 81%

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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Section: Notes On Individual Sourcesmentioning

confidence: 81%

Parsec-scale properties of brightest cluster galaxies

Liuzzo

Giovannini

Giroletti³

et al. 2010

A&A

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“…For clusters of the Z sample we consider only galaxies Metcalfe et al 1994 ;(11) Willmer et al 1991 ;(12) et al 1992 ; (13) Beers et al Sodre 1984 ;(14) (15) Richter 1989 ;(16) Fabricant et al 1993 ;(17) Mohr et al 1996 ;(18) Flin et al 1995 ;(19) Trevese et al 1997 ;(20) Barmby & Huchra 1998 ;(21) Fabricant, Kent, & Kurtz 1989 ;(22) Malumuth & Kriss 1986 ;(23) Bardelli et al 1998 ; (24) COSMOS catalog ; (25) Tully et al 1996. identiÐed as cluster members : for cluster data in common with G98 we use their member identiÐcation after the peak selection in velocity distribution via the adaptive kernel method and the shifting gapper (see also Fadda et al 1996). For new cluster data we apply this same procedure for cluster member identiÐcation.…”

Section: Other Samplesmentioning

confidence: 99%

Optical Luminosities and Mass‐to‐Light Ratios of Nearby Galaxy Clusters

Girardi

Borgani

Giuricin

et al. 2000

ApJ

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We analyze a sample of 105 clusters having virial mass homogeneously estimated and for which galaxy magnitudes are available with a well-deÐned high degree of completeness. In particular, we consider a subsample of 89 clusters with galaxy magnitudes taken from the COSMOS/UKST B j -band Southern Sky Object Catalog. After suitable magnitude corrections and uniform conversions to band, B j we compute cluster luminosities within several clustercentric distances, 0.5, 1.0, 1.5 h~1 Mpc and L Bj within the virialization radiusIn particular, we use the luminosity function and background counts R vir . estimated by Lumsden et al. on the Edinburgh/Durham Southern Galaxy Catalog, which is the wellcalibrated part of the COSMOS catalog. We analyze the e †ect of several uncertainties connected to photometric data, fore/background removal, and extrapolation below the completeness limit of the photometry, in order to assess the robustness of our cluster luminosity estimates. We draw our results on the relations between luminosity and dynamical quantities from the COSMOS sample by considering mass and luminosities determined within the virialization radius. We Ðnd a very good correlation between cluster luminosity, and galaxy velocity dispersion, with Our estimate of . the typical value for the mass-to-light ratio isWe do not Ðnd any correlation ofwith cluster morphologies, i.e., Rood-Sastry and Bautz-Morgan types, and only a weak signiÐcant M/L Bj correlation with cluster richness. We Ðnd that mass has a slight, but signiÐcant, tendency to increase faster than the luminosity does,We verify the robustness of this relation against a number M P L Bj 1.2h1.3. of possible systematics. We verify that this increasing trend of M/L with cluster mass cannot be entirely due to a higher spiral fraction in poorer clusters, thus suggesting that a similar result would also be found by using R-band galaxy magnitudes.

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“…Thus, the analysis of substructures in galaxy clusters based on projected, i.e. 2D data, can reveal a statistically correct percentage of subclustering, disregarding some differences for individual objects (Flin & Krywult 2002). …”

Section: Introductionmentioning

confidence: 99%

Substructures in Abell clusters of galaxies

Флин

Krywult

2006

A&A

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Aims. We present the results of substructure detection on a large sample of Abell clusters. Methods. We apply the wavelet transform to positions of galaxies in 183 Abell clusters. The significance of the substructuring detected was determined using Monte Carlo simulations on sets of 1000 randomly generated distributions of galaxies for each cluster and wavelet scale. Results. 62 of the investigated clusters are strongly substructured; the frequency of occurrence of substructure is 0.34. The investigated clusters were classified as unimodal, bimodal or complex systems. The clusters were divided into clusters having substructures in the field of the cluster S f or in the core region S c . The Kolmogorov-Smirnov test show no significant differences at the level α = 0.05 in the distribution of clusters having S c and S f substructures with redshift. Using a χ 2 test we found no correlation between the existence of subclustering and the morphological type of galaxy clusters.

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Properties of nearby clusters of galaxies

Cited by 13 publications

References 10 publications

Parsec-scale properties of brightest cluster galaxies

Parsec-scale properties of brightest cluster galaxies

Optical Luminosities and Mass‐to‐Light Ratios of Nearby Galaxy Clusters

Substructures in Abell clusters of galaxies

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