Dynamical state and star formation properties of the merging galaxy cluster Abell 3921

Ferrari, C.; Benoist, Christophe; Maurogordato, S.; Cappi, A.; Slezak, E.

doi:10.1051/0004-6361:20041811

Cited by 68 publications

(108 citation statements)

References 74 publications

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“…One of the variants of this method establishes a relationship between the total mass M of the bimodal cluster and the angle α between the plane of the sky and the collision axis of the two clumps (Barrena et al 2002;Ferrari et al 2005). The input parameters derived from the observations are the relative radial velocity between the two subclusters V r and their projected spatial separation R p .…”

Section: Two-body Analysismentioning

confidence: 99%

“…The aims of the program are to characterize the merging scenario (epoch of collision, geometry, and mass ratios) and to test the impact of the merging process on the properties of galaxies, in particular the star formation. For example, the combined X-ray and optical analysis allowed us to determine the merging scenario of the first two clusters (a premerger for A1750, Belsole et al 2004; and a recent post-merger for A3921, Belsole et al 2005;Ferrari et al 2005).…”

Section: Introductionmentioning

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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Section: Two-body Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Merging history of three bimodal clusters

Maurogordato

Sauvageot

Bourdin

et al. 2010

A&A

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“…We produced density maps of the bi-dimensional galaxy distribution of each observed cluster on the basis of a multi-scale approach, as described in Ferrari et al (2005). To avoid projection effects as much as possible, we selected galaxies lying on the cluster red-sequence and brighter than L * + 3.…”

Section: New Detections Of Diffuse Radio Emissionmentioning

confidence: 99%

Detection of diffuse radio emission in the galaxy clusters A800, A910, A1550, and CL 1446+26

Govoni¹,

Ferrari²,

Feretti³

et al. 2012

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Context. Radio halos are elusive sources located at the center of merging galaxy clusters. To date, only about 40 radio halos are known, thus the discovery of new halos provides important insights into this class of sources. Aims. To improve the quality of the statistics of radio halos, we investigate the radio continuum emission of a sample of galaxy clusters. Methods. We analyzed archival Very Large Array observations at 1.4 GHz, with a resolution of 1 . These observations were complemented by X-ray, optical, and higher-resolution radio data, leading to the detection of a new radio halo in the central region of A800 and A1550. We discovered a radio relic in the periphery of A910, and finally revealed both a halo and a relic in CL1446+26. Results. The clusters hosting these new halos show an offset between the radio and the X-ray peak. By analyzing this offset statistically, we find that radio halos can be quite asymmetric with respect to the X-ray gas distribution, with an average radio-X-ray displacement of about 180 kpc. When the offsets are normalized by the halo size, there is a tendency for smaller halos to have larger displacements.

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“…We produced a multi-scale galaxy density map (see Ferrari et al 2005 for more details) using the 550 spectroscopically confirmed cluster members obtained by Owers et al (2009). In Fig.…”

Section: Dynamical Statementioning

confidence: 99%

Metallicity map of the galaxy cluster A3667

Lovisari¹,

Kapferer²,

Schindler³

et al. 2009

A&A

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We use XMM-Newtondata of the merging cluster Abell 3667 to analyze its metallicity distribution. A detailed abundance map of the central 1.1 × 1.1 Mpc region indicates that metals are inhomogeneously distributed in the cluster showing a non-uniform and very complex metal pattern. The highest peak in the map corresponds to a cold region, slightly offset South of the X-ray center. This could be interpreted as stripped gas due to a merger between a group moving from NW towards the SE and the main cluster. We note several clumps of high metallicity also in the opposite direction with respect to the X-ray peak. Furthermore we determined abundances for 5 elements (O, Si, S, Ar, Fe) in four different regions of the cluster. Comparisons between these observed abundances and theoretical supernovae yields allow to get constraints on the relative number of SN Ia and II contributing to the enrichment of the intra-cluster medium. To reproduce the observed abundances of the best determined elements (Fe, O and Si) in a region of 7 around the X-ray center, 65-80% of SN II are needed. The comparison between the metal map, a galaxy density map obtained using 550 spectroscopically confirmed cluster members and, our simulations suggest a recent merger between the main cluster and the group in the SE.

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Dynamical state and star formation properties of the merging galaxy cluster Abell 3921

Cited by 68 publications

References 74 publications

Merging history of three bimodal clusters

Merging history of three bimodal clusters

Detection of diffuse radio emission in the galaxy clusters A800, A910, A1550, and CL 1446+26

Metallicity map of the galaxy cluster A3667

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