X-ray-optical classification of cluster mergers and the evolution of the cluster merger fraction

Mann, Andrew W.; Ebeling, H.

doi:10.1111/j.1365-2966.2011.20170.x

Cited by 218 publications

(360 citation statements)

References 109 publications

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“…4. GLOBAL X-RAY PROPERTIES MACS J0416.1-2403 has been previously identified as a merging galaxy cluster at z = 0.396 (Mann & Ebeling 2012). The brightness of the NE subcluster core is significantly more peaked than that of the SW subcluster, which instead has a rather flat brightness distribution ( Figure 1).…”

Section: X-ray Foreground and Background Modelingmentioning

confidence: 97%

“…Here, we present results from Chandra, Jansky Very Large Array (JVLA), and Giant Metrewave Radio Telescope (GMRT) observations of another merging galaxy cluster: the HST Frontier Fields 22 cluster MACS J0416.1-2403 (z = 0.396, Ebeling et al 2001;Mann & Ebeling 2012). Optical and lensing studies of this cluster have been presented recently by, e.g., Zitrin et al (2013Zitrin et al ( , 2015, Schirmer et al (2015), Jauzac et al (2014), Grillo et al (2015).…”

Section: Introductionmentioning

confidence: 95%

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FRONTIER FIELDS CLUSTERS:CHANDRAAND JVLA VIEW OF THE PRE-MERGING CLUSTER MACS J0416.1-2403

Ogrean

Weeren

Jones

et al. 2015

ApJ

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Merging galaxy clusters leave long-lasting signatures on the baryonic and non-baryonic cluster constituents, including shock fronts, cold fronts, X-ray substructure, radio halos, and offsets between the dark matter (DM) and the gas components. Using observations from Chandra, the Jansky Very Large Array, the Giant Metrewave Radio Telescope, and the Hubble Space Telescope, we present a multiwavelength analysis of the merging Frontier Fields cluster MACS J0416.1-2403 (z = 0.396), which consists of NE and SW subclusters whose cores are separated on the sky by ∼250 kpc. We find that the NE subcluster has a compact core and hosts an X-ray cavity, yet it is not a cool core. Approximately 450 kpc south-southwest of the SW subcluster, we detect a density discontinuity that corresponds to a compression factor of ∼1.5. The discontinuity was most likely caused by the interaction of the SW subcluster with a less massive structure detected in the lensing maps SW of the subclusterʼs center. For both the NE and the SW subclusters, the DM and the gas components are well-aligned, suggesting that MACS J0416.1-2403 is a pre-merging system. The cluster also hosts a radio halo, which is unusual for a pre-merging system. The halo has a 1.4 GHz power of (1.3 ± 0.3) × 10 24 W Hz −1 , which is somewhat lower than expected based on the X-ray luminosity of the cluster if the spectrum of the halo is not ultra-steep. We suggest that we are either witnessing the birth of a radio halo, or have discovered a rare ultra-steep spectrum halo.

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Section: X-ray Foreground and Background Modelingmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 95%

FRONTIER FIELDS CLUSTERS:CHANDRAAND JVLA VIEW OF THE PRE-MERGING CLUSTER MACS J0416.1-2403

Ogrean

Weeren

Jones

et al. 2015

ApJ

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“…Z1953 (ZwCl 0847.2+3617) is a hot cluster classified as a merger based on optical and X-ray properties (Mann & Ebeling 2012). Three discrete radio sources (A, B, and C) are located in the central region of the cluster, aligned in the north-south direction (Fig.…”

Section: Z1953: a Diffuse Sourcementioning

confidence: 99%

The Extended GMRT Radio Halo Survey

Kale¹,

Venturi²,

Giacintucci³

et al. 2015

A&A

134

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The intra-cluster medium contains cosmic rays and magnetic fields that are manifested through the large scale synchrotron sources, termed radio haloes, relics, and mini-haloes. The Extended Giant Metrewave Radio Telescope (GMRT) Radio Halo Survey (EGRHS) is an extension of the GMRT Radio Halo Survey (GRHS) designed to search for radio haloes using GMRT 610/235 MHz observations. The GRHS and EGRHS consists of 64 clusters in the redshift range 0.2−0.4 that have an X-ray luminosity larger than 5 × 10 44 erg s −1 in the 0.1−2.4 keV band and declination, δ > −31 • in the REFLEX and eBCS X-ray cluster catalogues. In this second paper in the series, GMRT 610/235 MHz data on the last batch of 11 galaxy clusters and the statistical analysis of the full sample are presented. A new mini-halo in RX J2129.6+0005 and candidate diffuse sources in Z5247, A2552, and Z1953 have been discovered. A unique feature of this survey are the upper limits on the detections of 1 Mpc sized radio haloes; 4 new are presented here, making a total of 31 in the survey. Of the sample, 58 clusters with adequately sensitive radio information were used to obtain the most accurate occurrence fractions so far. The occurrence fractions of radio haloes, mini-haloes and relics in our sample are ∼22%, ∼16% and ∼5%, respectively. The P 1.4 GHz − L X diagrams for the radio haloes and mini-haloes are presented. The morphological estimators -centroid shift (w), concentration parameter (c), and power ratios (P 3 /P 0 ) derived from the Chandra X-ray images -are used as proxies for the dynamical states of the GRHS and EGRHS clusters. The clusters with radio haloes and mini-haloes occupy distinct quadrants in the c− w, c− P 3 /P 0 and w− P 3 /P 0 planes, corresponding to the more and less morphological disturbance, respectively. The non-detections span both the quadrants.Key words. galaxies: clusters: general -radio continuum: galaxies IntroductionThe intra-cluster medium (ICM) is the diffuse matter that pervades the space between the galaxies in galaxy clusters. It is dominated by hot (∼10 7 −10 8 K) thermal plasma that emits thermal Bremsstrahlung that is detectable in soft X-ray bands and is also responsible for the thermal Sunyaev-Zel'dovich (SZ) effect. It has been found that the ICM also contains magnetic fields (0.1−1 μG) and relativistic electrons (Lorentz factors 1000) distributed over the entire cluster volume. The most direct evidence of this are the cluster-wide diffuse synchrotron sources detected in radio bands (see Feretti et al. 2012;Brunetti & Jones 2014, for reviews). They occur in a variety of morphologies and sizes and are classified into three main types, namely, radio haloes, radio relics, and mini-haloes.Radio haloes (RHs) are Mpc-sized sources found in massive, merging galaxy clusters. They typically trace the morphology of the X-ray surface brightness, show negligible polarisation, and Appendices are available in electronic form at http://www.aanda.org have synchrotron spectral indices 1 , α ≥ 1. The emitting relativistic electro...

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“…Mohr et al 1995;Schuecker et al 2001;Jeltema et al 2005;Santos et al 2008;Böhringer et al 2010;Chon et al 2012b;Mann & Ebeling 2012), optical (e.g. Plionis & Basilakos 2002;Flin & Krywult 2006;Ramella et al 2007;Einasto et al 2012;Foëx et al 2013;Wen & Han 2013), lensing (e.g.…”

Section: Introductionmentioning

confidence: 99%

From the core to the outskirts: structure analysis of three massive galaxy clusters

Foëx

Chon

Böhringer

2017

A&A

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Aims. The hierarchical model of structure formation is a key prediction of the Λ cold dark matter model, which can be tested by studying the large-scale environment and the substructure content of massive galaxy clusters. We present here a detailed analysis of the clusters RXCJ0225.9-4154, RXCJ0528.9-3927, and RXCJ2308.3-0211, as part of a sample of massive X-ray luminous clusters located at intermediate redshifts.Methods. We used a multiwavelength analysis, combining WFI photometric observations, VIMOS spectroscopy, and the X-ray surface brightness maps. We investigated the optical morphology of the clusters, we looked for significant counterparts in the residual X-ray emission, and we ran several statistical tests to assess their dynamical state. We correlated the results to define various substructure features, to study their properties, and to quantify their influence on simple dynamical mass estimators. Results. RXCJ0225.9-4154 has a bi-modal core, and two massive galaxy groups are located in its immediate surroundings; they are aligned in an elongated structure that is also detected in X-rays at the 1σ level. RXCJ0528.9-3927 is located in a poor environment; an X-ray centroid shift and the presence of two central BCGs provide mild evidence for a recent and active dynamical history. RXCJ2308.3-0211 has complex central dynamics, and it is found at the core of a superstes-cluster. Conclusions. The complexity of the cluster's central dynamics reflects the richness of its large-scale environment: RXCJ0225 and RXCJ2308 present a mass fraction in substructures larger than the typical 5% − 15%, whereas the isolated cluster RXCJ0528 does not have any major substructures within its virial radius. The largest substructures are found in the cluster outskirts. The optical morphology of the clusters correlates with the orientation of their BCG, and with the position of the main axes of accretion.

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X-ray-optical classification of cluster mergers and the evolution of the cluster merger fraction

Cited by 218 publications

References 109 publications

FRONTIER FIELDS CLUSTERS:CHANDRAAND JVLA VIEW OF THE PRE-MERGING CLUSTER MACS J0416.1-2403

FRONTIER FIELDS CLUSTERS:CHANDRAAND JVLA VIEW OF THE PRE-MERGING CLUSTER MACS J0416.1-2403

The Extended GMRT Radio Halo Survey

From the core to the outskirts: structure analysis of three massive galaxy clusters

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