Cluster and cluster galaxy evolution history from IR to X-ray observations of the young cluster RX J1257.2+4738 at <i>z</i> = 0.866

Ulmer, M. P.; Adami, C.; Neto, G. B. Lima; Durret, F.; Covone, G.; Ilbert, O.; Cypriano, E. S.; Allam, S.; Krön, Richard G.; Mahoney, W. A.; Gavazzi, R.

doi:10.1051/0004-6361/200811021

Cited by 8 publications

(15 citation statements)

References 37 publications

(46 reference statements)

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“…A.1 that a cut seems to appear at z ≥ 1 where infalling haloes are closer to the value of the main system mass. The position of this cut is also in good agreement with the expectations of Ulmer et al (2009), based on the typical relaxation time of a galaxy falling onto a typical cluster. This will obviously have to be confirmed on larger numerical simulations in the future given the relatively small number of massive structures present in the Millenium simulations.…”

Section: Appendix A: Infalling Activity On Clusters In the Millenniumsupporting

confidence: 87%

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

Adami

Durret

Guennou

et al. 2013

A&A

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Context. Cluster properties do not seem to be changing significantly during their mature evolution phase; for example, they do not seem to show any strong dynamical evolution at least up to z ∼ 0.5, their galaxy red sequence is already in place at least up to z ∼ 1.2, and their diffuse light content remains stable up to z ∼ 0.8. The question is now to know if cluster properties can evolve more significantly at redshifts that are notably higher than 1. Aims. We propose here to see how the properties of the intracluster light (ICL) evolve with redshift by detecting and analysing the ICL in the X-ray cluster CL J1449+0856 at z = 2.07, based on deep HST NICMOS H band exposures. Methods. We used the same wavelet-based method as one applied to 10 clusters between z = 0.4 and 0.8. Results. We detect three diffuse light sources with total magnitudes of H = 24.8, 25.5, and 25.9, plus a more compact object with a magnitude H = 25.3. We discuss the significance of our detections and show that they are robust. Conclusions. The three sources of diffuse light indicate an elongation along a north-east south-west axis, similar to that of the distribution of the central galaxies and to the X-ray elongation. This strongly suggests a history of merging events in this direction. While we found a roughly constant amount of diffuse light for clusters between z ∼ 0 and 0.8, we prove at least a 1.5 mag increase between z ∼ 0.8 and 2. If we assume that the amount of diffuse light is directly linked to the infall activity on the cluster, this implies that CL J1449+0856 is still undergoing strong merging events.

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Section: Appendix A: Infalling Activity On Clusters In the Millenniumsupporting

confidence: 87%

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

Adami

Durret

Guennou

et al. 2013

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“…The final optical catalogue includes 1894 sources with completeness levels at 50% of 25.0, 24.3, 24.2, and 23.4 mag for g r i z , respectively. A final check of our photometry was performed against that from Ulmer et al (2009). To that end, we compared the distributions of galaxies in the i − z vs. i colour−magnitude diagram (a direct comparison of individual galaxies was not possible since the referred authors did not publish a source catalogue).…”

Section: Optical Broadband Imagingmentioning

confidence: 99%

“…The photometric cluster sample thus defined, along with a small spectroscopic sample (Ulmer et al 2009), yielded to a cluster sample of 271 + 21 = 292 galaxies. We merged this first cluster catalogue, using the nearest neighbour technique with a maximum error radii of 1.5 , with the [O ii]-emitters sample v LoS complete, and obtained a final cluster catalogue of 315 members.…”

Section: Multi-wavelength Cataloguementioning

confidence: 99%

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Multi-wavelength landscape of the young galaxy cluster RXJ 1257.2+4738 atz= 0.866

Pintos-Castro

Pović

Sánchez‐Portal

et al. 2016

A&A

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Studying the evolution of the morphological distribution of galaxies in different environments can provide important information about the effects of the environment and the physical mechanisms responsible for the morphological transformations. As part of a complete analysis of the young cluster RXJ 1257+4738 at z ∼ 0.9, in this work we study the morphological properties of its galaxies. We used non-parametric methods of morphological classification, as implemented in the galSVM code. The classification with the applied method was possible even using ground-based observations, as the r -band imaging from OSIRIS/GTC. We defined very conservative probability limits, taking into account the probability errors, to obtain a trustworthy classification. In this way we were able to classify ∼30% of all cluster members and to separate between late-type (LT) and early-type (ET) galaxies. Additionally, when analysing the colour-magnitude diagram, we observed a significant population of blue ET galaxies among the classified ones. We discussed possible explanations for finding this population. Moreover, we studied different physical properties of LT, ET, and blue ET galaxies. They turn out to be comparable, with the exception of the stellar mass that shows that the red ET population is more massive. We also analysed the morphology-density and morphology-radius relations observing that, only when considering the morphological separation between ET and LT galaxies, a mild classical behaviour is obtained. RXJ 1257+4738 is a young galaxy cluster, showing a clumpy structure, which is still in the process of formation, and which could explain the lack of some of the standard morphological relations. This makes this cluster a very attractive case for obtaining higher resolution data and for studying the morphological properties of the entire cluster in more detail and their relation to the environment.

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“…Ulmer et al (2009) reported the discovery of the spectroscopically confirmed cluster at z = 0.866, on the basis of an extensive study including Chandra, XMM-Newton, Spitzer, Gemini, Subaru and ARC observations. They detected the diffuse emission of the cluster both in Chandra and XMM-Newton observations, and modelled that emission with an ellipse centered at RA(J2000) = 12h 57m 12.2s Dec(J2000) = +47…”

Section: Introductionmentioning

confidence: 99%

Multi-wavelength landscape of the young galaxy cluster RX J1257.2+4738 atz= 0.866

Pintos-Castro

Sánchez‐Portal

Cepa

et al. 2013

A&A

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Context. Many studies have shown how galaxy properties (e.g. colours, morphology, star-forming (SF) activity, active galactic nuclei population) change not only with redshift, but also with local galaxy density, revealing the important effect of the stellar/halo mass and the environment in the evolution of galaxies. A detailed analysis of the star formation activity in a representative sample of clusters will help us to understand the physical processes that cause the observed changes. Aims. We performed a thorough analysis of the star formation activity in the young massive galaxy cluster RX J1257+4738 at z = 0.866, with emphasis on the relationship between the local environment of the cluster galaxies and their star formation activity. We present an optical and infrared (IR) study that benefited from the large amount of data available for this cluster, including new OSIRIS/GTC and Herschel imaging observations. Methods. Using a multi-wavelength catalogue from the optical to the near-infrared, we measured photometric redshifts through a χ 2 spectral energy distribution fitting procedure. We implemented a reliable and carefully chosen cluster membership selection criterion including Monte Carlo simulations and derived a sample of 292 reliable cluster member galaxies for which we measured the following properties: optical colours, stellar masses, ages, ultraviolet luminosities and local densities. Using the MIPS 24 µm and Herschel data, we measured total IR luminosities and star formation rates (SFRs). Results. Of the sample of 292 cluster galaxies, 38 show far-infrared (FIR) emission with an SFR between 0.5 and 45 M yr −1 . The spatial distribution of the FIR emitters within the cluster density map and the filament-like overdensities observed suggest that RX J1257 is not virialised, but is in the process of assembly. The average star formation as a function of the cluster environment parametrised by the local density of galaxies does not show any clear trend. However, the fraction of SF galaxies unveils that the cluster intermediatedensity regions is preferred for the SF activity to enhance, since we observe a significant increase of the FIR-emitter fraction in this environment. The analysis of the extinction distributions of the optically red and blue SF galaxies supports the assumption of the red SF galaxies as a dusty population.

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Cluster and cluster galaxy evolution history from IR to X-ray observations of the young cluster RX J1257.2+4738 at z = 0.866

Cited by 8 publications

References 37 publications

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

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

Multi-wavelength landscape of the young galaxy cluster RXJ 1257.2+4738 atz= 0.866

Multi-wavelength landscape of the young galaxy cluster RX J1257.2+4738 atz= 0.866

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