Clusters at Half Hubble Time: Galaxy Structure and Colors in RX J0152.7−1357 and MS 1054−03

Blakeslee, John P.; Holden, B.; Franx, Marijn; Rosati, P.; Bouwens, Rychard; Demarco, R.; Ford, H. C.; Homeier, N.; Illingworth, G. D.; Jee, M. James; Mei, S.; Menanteau, F.; Meurer, G. R.; Postman, Marc; Tran, Kim‐Vy H.

doi:10.1086/503539

Cited by 122 publications

(190 citation statements)

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“…5) with a simplistic approach. The restframe U − B scatter calculated from synthetic colors for the red-sequence galaxies is ∼0.06, in good agreement with previous estimates at similar redshifts (Blakeslee et al 2006;Gobat et al 2008;Mei et al 2009). Assuming that the star formation histories of the bright red sequence galaxies may be described by a simple exponentially declining star formation rate with time-scale τ, we evolved the z ∼ 1.39 red-sequence galaxies to earlier epochs (see also a more detailed analysis in Gobat et al 2008).…”

Section: Color−magnitude Diagramssupporting

confidence: 91%

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Strazzullo

Rosati

Pannella

et al. 2010

A&A

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130

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We present a multi-wavelength study of galaxy populations in the core of the massive, X-ray luminous cluster XMMU J2235 at z = 1.39, based on high quality VLT and HST photometry at optical and near-infrared wavelengths. We derive luminosity functions in the z, H, and K s bands, approximately corresponding to restframe U, R and z band. These show a faint-end slope consistent with being flat, and a characteristic magnitude M * close to passive evolution predictions of M * of local massive clusters, with a formation redshift z > 2. The color−magnitude and color-mass diagrams show evidence of a tight red sequence (intrinsic scatter < ∼ 0.08) of massive galaxies already in place, with overall old stellar populations and generally early-type morphology. Beside the red colors, these massive (>6 × 10 10 M ) galaxies typically show early-type spectral features, and rest-frame far-UV emission consistent with very low star formation rates (SFR < 0.2 M yr −1 ). Star forming spectroscopic members, with SFR of up to ∼100 M /yr, are all located at clustercentric distances > ∼ 250 kpc, with the central cluster region already appearing effectively quenched. Most part of the cluster galaxies more massive than 6 × 10 10 M within the studied area do not appear to host significant levels of star formation. The high-mass end of the galaxy populations in the core of this cluster appears to be in a very advanced evolutionary stage, not only in terms of formation of the stellar populations, but also of the assembly of the stellar mass. The high-mass end of the galaxy stellar mass function is essentially already in place. The stellar mass fraction estimated within r 500 (∼1%, Kroupa IMF) is already similar to that of local massive clusters. On the other hand, surface brightness distribution modeling of the massive red sequence galaxies may suggest that their size is often smaller than expected based on the local stellar mass vs. size relation. An evolution of the stellar mass vs. size relation might imply that, in spite of the overall early assembly of these sources, their evolution is not complete, and processes like minor (and likely dry) merging might still shape the structural properties of these objects to resemble those of their local counterparts, without substantially affecting their stellar mass or host stellar populations. Nonetheless, a definite conclusion on the actual relevance of size evolution for the studied early-type sample is precluded by possible systematics and biases.

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Section: Color−magnitude Diagramssupporting

confidence: 91%

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Strazzullo

Rosati

Pannella

et al. 2010

A&A

Self Cite

130

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“…5 and following). We used the recent intermediate redshift sample , the classic high redshift sample of Damjanov et al (2009), the new high redshift sample of Belli et al (2014), and the catalogue of van de , which contains a composition of various high redshift samples, such as Bezanson et al (2013), van Dokkum et al (2009), Onodera et al (2012, Cappellari et al (2009), Newman et al (2010, van der Wel et al (2008), Blakeslee et al (2006), Toft et al (2012), and their own work. We cannot perform a comparison with these datasets in every figure, because sometimes some samples do not contain the required parameters.…”

Section: Resultsmentioning

confidence: 99%

Dozens of compact and high velocity-dispersion, early-type galaxies in Sloan Digital Sky Survey

Saulder

Bosch

Mieske

2015

A&A

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Context. Passive galaxies at high redshift are much smaller than equally massive early types today. If this size evolution is caused by stochastic merging processes, then a small fraction of the compact galaxies should persist until today. Up to now it has not been possible to systematically identify the existence of such objects in Sloan Digital Sky Survey (SDSS). Aims. We aim at finding potential survivors of these compact galaxies in SDSS, as targets for more detailed follow-up observations. Methods. From the virial theorem, it is expected that for a given mass, compact galaxies have stellar velocity dispersion higher than the mean owing to their smaller sizes. Therefore velocity dispersion, coupled with size (or mass), is an appropriate method of selecting relics, independent of the stellar population properties. Based on these considerations, we designed a set of criteria the use the distribution of early-type galaxies from SDSS on the log 10 (R 0 )−log 10 (σ 0 ) plane to find the most extreme objects on it. We thus selected compact massive galaxy candidates by restricting them to high velocity dispersions σ 0 > 323.2 km s −1 and small sizes R 0 < 2.18 kpc. Results. We find 76 galaxies at 0.05 < z < 0.2, which have properties that are similar to the typical quiescent galaxies at high redshift. We discuss how these galaxies relate to average present-day early-type galaxies. We study how well these galaxies fit on well-known local universe relations of early-type galaxies, such as the fundamental plane, the red sequence, or mass-size relations. As expected from the selection criteria, the candidates are located in an extreme corner of the mass-size plane. However, they do not extend as deeply into the so-called zone of exclusion as some of the red nuggets found at high redshift, since they are a factor 2−3 less massive on a given intrinsic scale size. Several of our candidates are close to the size resolution limit of SDSS, but are not so small that they are classified as point sources. We find that our candidates are systematically offset on a scaling relation compared to the average early-type galaxies, but still within the general range of other early-type galaxies. Furthermore, our candidates are similar to the mass-size range expected for passive evolution of the red nuggets from their high redshift to the present. Conclusions. The 76 selected candidates form an appropriate set of objects for further follow-up observations. They do not constitute a separate population of peculiar galaxies, but form the extreme tail of a continuous distribution of early-type galaxies. We argue that selecting a high-velocity dispersion is the best way to find analogues of compact high redshift galaxies in the local universe.

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“…Later this cluster was observed with the ACS/HST using F606W, F775W, and F850LP bands, and Postman et al (2005) performed a new visual morphological classification based on these images. There is a publicly available catalogue from Blakeslee et al (2006) that includes the morphological type and spectroscopic redshift of 142 members of this cluster. Regarding the available imaging data we explored two options: (i) the F606W WFPC2/HST available science mosaic (Förster Schreiber et al 2006); and (ii) the Rc SuprimeCam/Subaru raw images available on request from the SMOKA Science Archive.…”

Section: Unreliable Morphological Classificationmentioning

confidence: 99%

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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Clusters at Half Hubble Time: Galaxy Structure and Colors in RX J0152.7−1357 and MS 1054−03

Cited by 122 publications

References 84 publications

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Dozens of compact and high velocity-dispersion, early-type galaxies in Sloan Digital Sky Survey

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

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