Diffuse light in the young cluster of galaxies CL J1449+0856 at<i>z</i>= 2.07

Adami, C.; Durret, F.; Guennou, L.; Rocha, C. Da

doi:10.1051/0004-6361/201220282

Cited by 37 publications

(40 citation statements)

References 32 publications

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“…Even the very high concentration of ICL detected at z ∼ 2.1 in the CL J1449+0856 cluster (Adami et al 2013) is far from being at the same level. Moreover, ICL in the XLSSC 116 cluster is clearly visible up to 130 kpc from the cluster centre, a feature that is also quite rare in clusters.…”

Section: Diffuse Light Detectionmentioning

confidence: 93%

“…To detect the diffuse light, we applied the same tool as in Adami et al (2013) and Guennou et al (2012). This is a wavelet-based method (the OV_WAV package, see e.g.…”

Section: Diffuse Light Detectionmentioning

confidence: 99%

“…These sources were visually inspected to remove obvious numerical residuals of bright saturated Galactic stars or defects due to image cosmetics. These numerical residuals are described in Adami et al (2013); briefly, they can be modelled by Sinc functions, which are negligible in intensity in the present case because the considered point sources are faint.…”

Section: Diffuse Light Detectionmentioning

confidence: 99%

“…We have previously carried out several simulations (presented in Guennou et al 2012 andAdami et al 2013) to be reasonably sure that our data are not heavily polluted by the underlying BCG. However, we perform an additional test in this paper by analysing the BCG in the same way as the ICL (see Table 2 and Fig.…”

Section: Sed Fittingmentioning

confidence: 99%

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The XXL Survey

Adami

Pompei

Sadibekova

et al. 2016

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Aims. Within a cluster, gravitational effects can lead to the removal of stars from their parent galaxies and their subsequent dispersal into the intracluster medium. Gas hydrodynamical effects can additionally strip gas and dust from galaxies; both gas and stars contribute to intracluster light (ICL). The properties of the ICL can therefore help constrain the physical processes at work in clusters by serving as a fossil record of the interaction history. Methods. The present study is designed to characterise this ICL for the first time in a ∼10 14 M and z ∼ 0.53 cluster of galaxies from imaging and spectroscopic points of view. By applying a wavelet-based method to CFHT Megacam and WIRCAM images, we detect significant quantities of diffuse light and are able to constrain their spectral energy distributions. These sources were then spectroscopically characterised with ESO Multi Unit Spectroscopic Explorer (MUSE) spectroscopic data. MUSE data were also used to compute redshifts of 24 cluster galaxies and search for cluster substructures.Results. An atypically large amount of ICL, equivalent in i to the emission from two brightest cluster galaxies, has been detected in this cluster. Part of the detected diffuse light has a very weak optical stellar component and apparently consists mainly of gas emission, while other diffuse light sources are clearly dominated by old stars. Furthermore, emission lines were detected in several places of diffuse light. Our spectral analysis shows that this emission likely originates from low-excitation parameter gas. Globally, the stellar contribution to the ICL is about 2.3 × 10 9 yr old even though the ICL is not currently forming a large number of stars. On the other hand, the contribution of the gas emission to the ICL in the optical is much greater than the stellar contribution in some regions, but the gas density is likely too low to form stars. These observations favour ram pressure stripping, turbulent viscous stripping, or supernovae winds as the origin of the large amount of intracluster light. Since the cluster appears not to be in a major merging phase, we conclude that ram pressure stripping is the most plausible process that generates the observed ICL sources. Conclusions. This is one of the first times that we are able to spectroscopically study diffuse light in such a distant and massive cluster, and it demonstrates the potential of MUSE observations for such studies.

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Section: Diffuse Light Detectionmentioning

confidence: 93%

“…To detect the diffuse light, we applied the same tool as in Adami et al (2013) and Guennou et al (2012). This is a wavelet-based method (the OV_WAV package, see e.g.…”

Section: Diffuse Light Detectionmentioning

confidence: 99%

Section: Diffuse Light Detectionmentioning

confidence: 99%

Section: Sed Fittingmentioning

confidence: 99%

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The XXL Survey

Adami

Pompei

Sadibekova

et al. 2016

A&A

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“…Cosmological models of cluster mass assembly predict the most intense mass growth of clusters at redshifts earlier than z ∼ 0.8 to 1 (e.g. Adami et al (2013) from the Millennium simulation). In this redshift interval, clusters grow through accretion of major groups, and this already provides a pre-processed galaxy population formed by the cited "environment quenching".…”

Section: Evolution Of Cluster Galaxy Types With Redshiftmentioning

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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Galaxy Alignments: Observations and Impact on Cosmology

et al. 2015

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Galaxy shapes are not randomly oriented, rather they are statistically aligned in a way that can depend on formation environment, history and galaxy type. Studying the alignment of galaxies can therefore deliver important information about the physics of galaxy formation and evolution as well as the growth of structure in the Universe. In this review paper we summarise key measurements of galaxy alignments, divided by galaxy type, scale and environment. We also cover the statistics and formalism necessary to understand the observations in the literature. With the emergence of weak gravitational lensing as a precision probe of cosmology, galaxy alignments have taken on an added importance because they can mimic cosmic shear, the effect of gravitational lensing by large-scale structure on observed galaxy shapes. This makes galaxy alignments, commonly referred to as intrinsic alignments, an important systematic effect in weak lensing studies. We quantify the impact of intrinsic alignments on cosmic shear surveys and finish by reviewing practical mitigation techniques which attempt to remove contamination by intrinsic alignments.

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Diffuse light in the young cluster of galaxies CL J1449+0856 atz= 2.07

Cited by 37 publications

References 32 publications

The XXL Survey

The XXL Survey

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

Galaxy Alignments: Observations and Impact on Cosmology

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