The clusters Abell 222 and Abell 223: a multi-wavelength view

Durret, F.; Laganá, T. F.; Adami, C.; Bertin, E.

doi:10.1051/0004-6361/201014566

Cited by 23 publications

(24 citation statements)

References 43 publications

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“…The Gaussian components are in both cases important at bright magnitudes. An excess at very bright magnitudes seems to be quite a general phenomenon, as already noted for example in Abell 223 (Durret et al 2010), Abell 1758 (Durret et al 2011) or Abell 3376 (Durret et al 2013). But all these clusters were mergers, so we did not expect to find such a large gaussian component in Ophiuchus, which is believed from previous studies to be quite relaxed.…”

Section: The Global Galaxy Luminosity Functionsupporting

confidence: 56%

The optical properties of galaxies in the Ophiuchus cluster

Durret

Wakamatsu

Adami

et al. 2018

A&A

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Context. Ophiuchus is one of the most massive clusters known, but due to its low Galactic latitude its optical properties remain poorly known. Aims. We investigate the optical properties of Ophiuchus to obtain clues on the formation epoch of this cluster, and compare them to those of the Coma cluster, which is comparable in mass to Ophiuchus but much more disturbed dynamically. Methods. Based on a deep image of the Ophiuchus cluster in the r band obtained at the Canada France Hawaii Telescope with the MegaCam camera, we have applied an iterative process to subtract the contribution of the numerous stars that pollute the image, due to the low Galactic latitude of the cluster, and obtained a photometric catalogue of 2818 galaxies fully complete at r = 20.5 mag and still 91% complete at r = 21.5 mag. We use this catalogue to derive the cluster Galaxy Luminosity Function (GLF) for the overall image and for a region (hereafter the "rectangle" region) covering exactly the same physical size as the region in which the GLF of the Coma cluster was studied by Adami et al. (2007). We then compute density maps based on an adaptive kernel technique, for different magnitude limits, and define three circular regions covering 0.08, 0.08 and 0.06 deg 2 respectively centered on the cluster (C), northwest (NW) and southeast (SE) of the cluster, in which we compute the GLFs. Results. The GLF fits are much better when a Gaussian is added to the usual Schechter function, to account for the excess of very bright galaxies. Compared to Coma, Ophiuchus shows a strong excess of bright galaxies. Conclusions. The properties of the two nearby very massive clusters Ophiuchus and Coma are quite comparable, though they seem embedded in different large scale environments. Our interpretation is that Ophiuchus has built up long ago, as confirmed by its relaxed state (see paper I) while Coma is still in the process of forming.

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Section: The Global Galaxy Luminosity Functionsupporting

confidence: 56%

The optical properties of galaxies in the Ophiuchus cluster

Durret

Wakamatsu

Adami

et al. 2018

A&A

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“…We resort to the method devised by Serna & Gerbal (1996, hereafter Htree-method; see, e.g., Durret et al 2010 for a recent application). This method uses a hierarchical clustering analysis to determine the relationship between galaxies according to their relative binding energies.…”

Section: Identifying Subclusters With the Htree Methodsmentioning

confidence: 99%

Internal dynamics of Abell 2254: a merging galaxy cluster with a clumpy, diffuse radio emission

Girardi

Bardelli

Barrena

et al. 2011

A&A

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Context. The mechanisms giving rise to diffuse radio emission in galaxy clusters and, in particular, their connection with cluster mergers are still being debated. Aims. We explore the internal dynamics of Abell 2254, which has been shown to host a very clumpy and irregular radio halo. Methods. Our analysis is mainly based on redshift data for 128 galaxies acquired at the Telescopio Nazionale Galileo. We combined galaxy velocities and positions to select 110 cluster galaxies and analyze its internal dynamics. We also used new (g , r , i ) photometric data acquired at the Isaac Newton Telescope, and (V, i ) photometric data available in the Subaru Archive. X-ray data from the XMM-Newton Science Archive were analyzed to study the hot gas component. Results. We estimate the cluster redshift z = 0.177, a high line-of-sight (LOS) velocity dispersion, σ V ∼ 1350 km s −1 , and the X-ray temperature kT ∼ 6.4 keV. Both our optical and X-ray analyses reveal complex dynamical activity. The analysis of the 2D galaxy distribution reveals the presence of two density peaks, one to the east and the other to the west (E and W peaks). Using the full 3D information we detect a high-velocity (ΔV rf,LOS ∼ 3000 km s −1 ), low-mass (σ V ∼ 200-500 km s −1 ) group at the position of the 2D E peak. For the main system we compute a velocity dispersion σ V ∼ 1000-1200 km s −1 . In the assumption of a bimodal system we estimate a mass M sys = 1.5-2.9 ×10 15 h −1 70 M . The X-ray morphological analysis, which is based on power ratios, centroid shifts, and concentration parameter, confirms that Abell 2254 is a dynamically disturbed cluster. The X-ray isophotes are elongated in the east direction, in agreement with a merger in the post core-crossing phase. A simple bimodal model finds that data are consistent with a bound, outgoing subcluster observed a few fractions of Gyr after the core crossing. However, both optical and X-ray analyses suggest that the main system is, in turn, a nonrelaxed structure, indicating north-south as a possible direction for a past accretion. Conclusions. We conclude that Abell 2254, for its mass and merging structure, fits well among the typical clusters with radio halos. We briefly discuss how the particular irregularity of the radio halo might be linked to the complexity of the Abell 2254 structure.

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“…Durret et al 2010). Finally, De Propris et al (2003) and Boué et al (2008) find different GLFs for cluster cores and outskirts.…”

Section: Introductionmentioning

confidence: 92%

“…We know that the merging of galaxy clusters can strongly affect the slope of the GLF, as illustrated by studies of cluster pairs or violently merging clusters (e.g. Durret et al 2010Durret et al , 2011Durret et al , 2013. Hence we would expect that substructured clusters present a variation of their faint-end slope compared to others.…”

Section: Dependence On Environmentmentioning

confidence: 99%

The evolution of the cluster optical galaxy luminosity function betweenz= 0.4 and 0.9 in the DAFT/FADA survey

Martinet

Durret

Guennou

et al. 2015

A&A

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Context. There is some disagreement about the abundance of faint galaxies in high-redshift clusters, with contradictory results in the literature arising from studies of the optical galaxy luminosity function (GLF) for small cluster samples. Aims. We compute GLFs for one of the largest medium-to-high-redshift (0.4 ≤ z < 0.9) cluster samples to date in order to probe the abundance of faint galaxies in clusters. We also study how the GLF depends on cluster redshift, mass, and substructure and compare the GLFs of clusters with those of the field. We separately investigate the GLFs of blue and red-sequence (RS) galaxies to understand the evolution of different cluster populations. Methods. We calculated the GLFs for 31 clusters taken from the DAFT/FADA survey in the B, V, R, and I rest-frame bands. We used photometric redshifts computed from BVRIZ J images to constrain galaxy cluster membership. We carried out a detailed estimate of the completeness of our data. We distinguished the red-sequence and blue galaxies using a V − I versus I colour−magnitude diagram. We studied the evolution of these two populations with redshift. We fitted Schechter functions to our stacked GLFs to determine average cluster characteristics. Results. We find that the shapes of our GLFs are similar for the B, V, R, and I bands with a drop at the red GLF faint ends that is more pronounced at high redshift: α red ∼ −0.5 at 0.40 ≤ z < 0.65 and α red > 0.1 at 0.65 ≤ z < 0.90. The blue GLFs have a steeper faint end (α blue ∼ −1.6) than the red GLFs, which appears to be independent of redshift. For the full cluster sample, blue and red GLFs meet at M V = −20, M R = −20.5, and M I = −20.3. A study of how galaxy types evolve with redshift shows that late-type galaxies appear to become early types between z ∼ 0.9 and today. Finally, the faint ends of the red GLFs of more massive clusters appear to be richer than less massive clusters, which is more typical of the lower redshift behaviour. Conclusions. Our results indicate that these clusters form at redshifts higher than z = 0.9 from galaxy structures that already have an established red sequence. Late-type galaxies then appear to evolve into early types, enriching the red sequence between this redshift and today. This effect is consistent with the evolution of the faint-end slope of the red sequence and the galaxy type evolution that we find. Finally, faint galaxies accreted from the field environment at all redshifts might have replaced the blue late-type galaxies that converted into early types, explaining the lack of evolution in the faint-end slopes of the blue GLFs.

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The clusters Abell 222 and Abell 223: a multi-wavelength view

Cited by 23 publications

References 43 publications

The optical properties of galaxies in the Ophiuchus cluster

The optical properties of galaxies in the Ophiuchus cluster

Internal dynamics of Abell 2254: a merging galaxy cluster with a clumpy, diffuse radio emission

The evolution of the cluster optical galaxy luminosity function betweenz= 0.4 and 0.9 in the DAFT/FADA survey

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