Velocity Dispersions and Cluster Properties in the Southern Abell Redshift Survey Clusters. II.

Muriel, H.; Quintana, H.; Infante, L.; Lambas, D. García; Way, Michael

doi:10.1086/342854

Cited by 17 publications

(18 citation statements)

References 22 publications

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“…Most of them conclude that, for large radii (r > 1 Mpc), the VDPs are flat (Girardi & Mezzetti 2001;Rines & Diaferio 2006;Fadda et al 1996;Muriel et al 2002). This is consistent with the mild decrease that we have found in our clusters.…”

Section: Velocity Dispersion Profilessupporting

confidence: 92%

A study of catalogued nearby galaxy clusters in the SDSS-DR4

Aguerri

Sánchéz-Janssen

Muñoz–Tuñón

2007

A&A

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Context. Large surveys such as the Sloan Digital Sky Survey have made large amounts of spectroscopic and photometric data of galaxies available, thereby providing important information for studying galaxy evolution in dense environments. Aims. We have selected a sample of 88 nearby (z < 0.1) galaxy clusters from the SDSS-DR4 with redshift information for the cluster members. In particular, we focus on the galaxy morphological distribution, the velocity dispersion profiles, and the fraction of blue galaxies in clusters. Methods. Cluster membership was determined using the available velocity information. We derived global properties for each cluster, such as their mean recessional velocity, velocity dispersion, and virial radii. Cluster galaxies were grouped into two families according to their u − r colours. Results. The total sample consists of 10 865 galaxies. As expected, the highest fraction of galaxies (62%) turned out to be early-type (red) ones, located at smaller distances from the cluster centre and showing lower velocity dispersions than late-type (blue) ones. The brightest cluster galaxies are located in the innermost regions and show the smallest velocity dispersions. Early-type galaxies also show constant velocity dispersion profiles inside the virial radius and a mild decline in the outermost regions. In contrast, late-type galaxies show ever decreasing velocity dispersions profiles. No correlation has been found between the fraction of blue galaxies and cluster global properties,such as cluster velocity dispersion or galaxy concentration. In contrast, we find a correlation between the X-ray luminosity and the fraction of blue galaxies. Conclusions. These results indicate that early-and late-type galaxies may have had different evolutions. Thus, blue galaxies are located in more anisotropic and radial orbits than early-type ones. Their star formation seems to be independent of the cluster global properties in low-mass clusters, but not for the most massive ones. We consider that it is unlikely that the whole blue population consists of recent arrivals to the cluster. These observational results suggest that the global environment could be important for driving the evolution of galaxies in the most massive cluster (σ > 800 km s −1 ). However, the local environment could play a key role in the galaxy evolution for low-mass clusters.

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Section: Velocity Dispersion Profilessupporting

confidence: 92%

A study of catalogued nearby galaxy clusters in the SDSS-DR4

Aguerri

Sánchéz-Janssen

Muñoz–Tuñón

2007

A&A

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“…We measured a location of C BI = 27 281 ± 103 km s −1 and a scale of S BI = 682 ± 65 km s −1 (Table 2). Our estimate of velocity location is significantly lower (∼400 km s −1 ) than that found by Muriel et al (2002). These differences may be caused by variations in sampling.…”

Section: Galaxy Velocity Distributioncontrasting

confidence: 88%

“…A2933 was included in the Southern Abell Redshift Survey (SARS, Way et al 2005), and on the basis of 53 redshifts Muriel et al (2002) estimated the cluster global velocity and velocity dispersion (27 709 ± 105 km s −1 and 759 ± 72 km s −1 , respectively); they also showed that the velocity dispersion as a function of radius appears to be constant to 5 Mpc/h from the cluster center. Their data, however, sample the cluster and its environment on large scales and at relatively bright magnitudes.…”

Section: Galaxy Velocity Distributionmentioning

confidence: 99%

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Merging history of three bimodal clusters

Maurogordato

Sauvageot

Bourdin

et al. 2010

A&A

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We present a combined X-ray and optical analysis of three bimodal galaxy clusters selected as merging candidates at z ∼ 0.1. These targets are part of MUSIC (MUlti-Wavelength Sample of Interacting Clusters), which is a general project designed to study the physics of merging clusters by means of multi-wavelength observations. Observations include spectro-imaging with XMM-Newton EPIC camera, multi-object spectroscopy (260 new redshifts), and wide-field imaging at the ESO 3.6 m and 2.2 m telescopes. We build a global picture of these clusters using X-ray luminosity and temperature maps together with galaxy density and velocity distributions. Idealized numerical simulations were used to constrain the merging scenario for each system. We show that A2933 is very likely an equal-mass advanced pre-merger ∼200 Myr before the core collapse, while A2440 and A2384 are post-merger systems (∼450 Myr and ∼1.5 Gyr after core collapse, respectively). In the case of A2384, we detect a spectacular filament of galaxies and gas spreading over more than 1 h −1 Mpc, which we infer to have been stripped during the previous collision. The analysis of the MUSIC sample allows us to outline some general properties of merging clusters: a strong luminosity segregation of galaxies in recent post-mergers; the existence of preferential axes -corresponding to the merging directions -along which the BCGs and structures on various scales are aligned; the concomitance, in most major merger cases, of secondary merging or accretion events, with groups infalling onto the main cluster, and in some cases the evidence of previous merging episodes in one of the main components. These results are in good agreement with the hierarchical scenario of structure formation, in which clusters are expected to form by successive merging events, and matter is accreted along large-scale filaments.

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“…Cluster velocity dispersions are known to depend on radius, hence on the aperture used to measure them Rines & Diaferio 2006;Muriel et al 2002;Girardi & Mezzetti 2001;Aguerri et al 2007). However, the dependence is very mild for galaxy clusters in the range of apertures considered here, i.e.…”

Section: Cluster Assignment and Redshift Histogramsmentioning

confidence: 99%

WINGS-SPE Spectroscopy in the WIde-field Nearby Galaxy-cluster Survey

Cava

Bettoni

Poggianti

et al. 2009

A&A

152

227

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Aims. We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. Methods. Using multi-object fiber-fed spectrographs, we observed our sample of WINGS cluster galaxies at an intermediate resolution of 6-9 Å and, using a cross-correlation technique, we measured redshifts with a mean accuracy of ∼45 km s −1 . Results. We present redshift measurements for 6137 galaxies and their first analyses. Details of the spectroscopic observations are reported. The WINGS-SPE has ∼30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. Conclusions. Using our redshifts, we calculate the velocity dispersion for all the clusters in the WINGS-SPE sample. We almost triple the number of member galaxies known in each cluster with respect to previous works. We also investigate the X-ray luminosity vs. velocity dispersion relation for our WINGS-SPE clusters, and find it to be consistent with the form L x ∝ σ 4 v .

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Velocity Dispersions and Cluster Properties in the Southern Abell Redshift Survey Clusters. II.

Cited by 17 publications

References 22 publications

A study of catalogued nearby galaxy clusters in the SDSS-DR4

A study of catalogued nearby galaxy clusters in the SDSS-DR4

Merging history of three bimodal clusters

WINGS-SPE Spectroscopy in the WIde-field Nearby Galaxy-cluster Survey

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