Evolution of the Color‐Magnitude Relation in High‐Redshift Clusters: Early‐Type Galaxies in the Lynx Supercluster at<i>z</i>∼ 1.26

Mei, S.; Holden, B. P.; Blakeslee, John P.; Rosati, P.; Postman, Marc; Jee, M. James; Rettura, Alessandro; Sirianni, M.; Demarco, R.; Ford, H. C.; Franx, Marijn; Homeier, N.; Illingworth, G. D.

doi:10.1086/503826

Cited by 102 publications

(128 citation statements)

References 56 publications

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“…In Figs 2-4 we show observational estimates for the CGLF from Strazzullo et al (2006Strazzullo et al ( , 2010 and Fassbender et al (2014), as well as our estimates based upon the data sets of Mei et al (2006b), Hilton et al (2009) andSnyder et al (2012). Strazzullo et al (2006Strazzullo et al ( , 2010 estimate the CGLF for their galaxy cluster sample by using a reference field, down to an equivalent photometric depth or deeper, to statistically remove the contribution from background galaxies, which is known to bias CGLF estimates (Andreon, Punzi & Grado 2005), particularly at bright magnitudes where the statistics are typically quite poor.…”

Section: Observational Estimatesmentioning

confidence: 80%

“…(i) Mei et al (2006b) : Mei et al,present i 775 (F775W) and z 850 (F850LP) observations of the clusters RX J0849+4452 and RX J0848+4453, which together make up the Lynx Supercluster, located at z ∼ 1.2. Applying the colour selection 0.8 < (i 775 − z 850 ) < 1.1, the flux selection 21 < z 850 < 24 and an aperture selection of 120 arcsec, left 40 galaxies, of which 14 are confirmed cluster members and 26 are cluster member candidates.…”

Section: O B S E Rvat I O Na L Data S E T Smentioning

confidence: 99%

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The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Merson¹,

Baugh²,

González-Pérez³

et al. 2015

Mon. Not. R. Astron. Soc.

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High redshift galaxy clusters allow us to examine galaxy formation in extreme environments.Here we compile data for 15 z > 1 galaxy clusters to test the predictions from a state-of-theart semi-analytical model of galaxy formation. The model gives a good match to the slope and zero-point of the cluster red sequence. The model is able to match the cluster galaxy luminosity function at faint and bright magnitudes, but under-estimates the number of galaxies around the break in the cluster luminosity function. We find that simply assuming a weaker dust attenuation improves the model predictions for the cluster galaxy luminosity function, but worsens the predictions for the red sequence at bright magnitudes. Examination of the properties of the bright cluster galaxies suggests that the default dust attenuation is large due to these galaxies having large reservoirs of cold gas as well as small radii. We find that matching the luminosity function and colours of high redshift cluster galaxies, whilst remaining consistent with local observations, poses a challenge for galaxy formation models.

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Section: Observational Estimatesmentioning

confidence: 80%

Section: O B S E Rvat I O Na L Data S E T Smentioning

confidence: 99%

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Merson¹,

Baugh²,

González-Pérez³

et al. 2015

Mon. Not. R. Astron. Soc.

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“…(e.g., Mei et al 2006) and is attributed to the long-wavelength halo of the ACS/WFC (Sirianni et al 2005). This effect, although small, has implications for the galaxy colour measurement and must be accounted for.…”

Section: Galaxy Photometrymentioning

confidence: 99%

Multiwavelength observations of a rich galaxy cluster at z $\thicksim$ 1

Santos

Rosati

Gobat

et al. 2009

A&A

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Context. XMMU J1229+0151 is a rich galaxy cluster with redshift z = 0.975 that was serendipitously detected in X-rays within the scope of the XMM-Newton Distant Cluster Project. Both HST/ACS observations in the i 775 and z 850 passbands and VLT/FORS2 spectroscopy were obtained, in addition to follow-up Near-Infrared (NIR) imaging in the J-and Ks-bands with NTT/SOFI. Aims. We investigate the photometric, structural, and spectral properties of the early-type galaxies in the high-redshift cluster XMMU J1229+0151. Methods. Source detection and aperture photometry are performed in the optical and NIR imaging. Galaxy morphology is inspected visually and by means of Sersic profile fitting to the 21 spectroscopically confirmed cluster members in the ACS field of view. The i 775 − z 850 colour−magnitude relation (CMR) is derived with a method based on galaxy magnitudes obtained by fitting the surface brightness of the galaxies with Sersic models. Stellar masses and formation ages of the cluster galaxies are derived by fitting the observed spectral energy distributions (SED) with models developed by Bruzual & Charlot. Star-formation histories of the early-type galaxies are constrained by analysing the stacked spectrophotometric data. Results. The structural Sersic index n obtained by model fitting agrees with the visual morphological classification of the confirmed members, indicating a clear predominance of elliptical galaxies (15/21). The i 775 − z 850 colour−magnitude relation of the spectroscopic members shows a very tight red-sequence with a zero point of 0.86 ± 0.04 mag, and intrinsic scatter equal to 0.039 mag. The CMR obtained with the galaxy models has similar parameters. By fitting both the spectra and SED of the early-type population, we obtain a star-formation-weighted age of 4.3 Gyr for a median galaxy stellar-mass of 7.4 × 10 10 M . Instead of identifying a brightest cluster galaxy (BCG) unambiguously, we find three bright galaxies with a similar z 850 magnitude, which are, in addition, the most massive cluster members, with ∼2 × 10 11 M . Our results strengthen the current evidence of a lack of significant evolution in both the scatter and slope of the red-sequence out to z ∼ 1.

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“…The effects of the environment on galaxy evolution have been studied at progressively higher redshifts through analysis of single clusters (e.g. Treu et al 2003;Nakata et al 2005;Tran et al 2005;Mei et al 2006;Menci et al 2008;Rettura et al 2008), as well as studying the variation of galaxy colours, morphologies, and other physical parameters as a function of projected or 3-dimensional density (e.g. Dressler et al 1997;Blanton et al 2005;Cucciati et al 2006;Cooper et al 2007;Elbaz et al 2007).…”

Section: Introductionmentioning

confidence: 99%

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Salimbeni

Castellano

Pentericci

et al. 2009

A&A

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Aims. The aim of the present paper is to identify and study the properties and galactic content of groups and clusters in the GOODSSouth field up to z ∼ 2.5, and to analyse the physical properties of galaxies as a continuous function of environmental density up to high redshift. Methods. We used the deep (z 850 ∼ 26), multi-wavelength GOODS-MUSIC catalogue, which has a 15% of spectroscopic redshifts and accurate photometric redshifts for the remaining fraction. On these data, we applied a (2+1)D algorithm, previously developed by our group, that provides an adaptive estimate of the 3D density field. We supported our analysis with simulations to evaluate the purity and the completeness of the cluster catalogue produced by our algorithm. Results. We find several high-density peaks embedded in larger structures in the redshift range 0.4-2.5. From the analysis of their physical properties (mass profile, M 200 , σ v , L X , U − B vs. B diagram), we find that most of them are groups of galaxies, while two are poor clusters with masses a few times 10 14 M . For these two clusters we find from the Chandra 2Ms data an X-ray emission significantly lower than expected from their optical properties, suggesting that the two clusters are either not virialised or are gas poor. We find that the slope of the colour magnitude relation, for these groups and clusters, is constant at least up to z ∼ 1. We also analyse the dependence on environment of galaxy colours, luminosities, stellar masses, ages, and star formations. We find that galaxies in high-density regions are, on average, more luminous and massive than field galaxies up to z ∼ 2. The fraction of red galaxies increases with luminosity and with density up to z ∼ 1.2. At higher z this dependence on density disappears. The variation of galaxy properties as a function of redshift and density suggests that a significant change occurs at z ∼ 1.5-2.

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Evolution of the Color‐Magnitude Relation in High‐Redshift Clusters: Early‐Type Galaxies in the Lynx Supercluster atz∼ 1.26

Cited by 102 publications

References 56 publications

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Multiwavelength observations of a rich galaxy cluster at z $\thicksim$ 1

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

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