The [ITAL]K[/ITAL]-Band Luminosity Function in Galaxy Clusters to [CLC][ITAL]z[/ITAL][/CLC] [FORMULA][F]∼1[/F][/FORMULA]

Propris, Roberto De; Stanford, S. A.; Eisenhardt, Peter; Dickinson, Mark; Elston, R.

doi:10.1086/300978

Cited by 130 publications

(196 citation statements)

References 63 publications

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“…Purely passive evolution of early-type galaxies is consistent with several other studies including the evolution of the K band luminosity function (De Propris et al 1999, Toft et al 2003, evolution of the fundamental plane in terms of mass-to-light ratios (van Dokkum et al 1998), and studies of the scatter of the colour-magnitude relation (see e.g. Ellis et al 1997.…”

Section: Resultssupporting

confidence: 89%

“…The models (described in the previous section) are normalised at low redshift to K * of the Coma cluster (De Propris et al 1998). The evolution is seen to be consistent with passive evolution models, with z f ≈ 1.5 if the models are normalised to Coma, or a higher redshift of formation if the models are normalised to the low redshift points from De Propris et al (1999).…”

Section: Resultsmentioning

confidence: 53%

“…Schechter (1976) functions were fit to the LFs of each cluster individually, with the faint end slope fixed at α = −0.9 (the local value for the Coma cluster, De Propris et al 1998, and the field, Gardner et al 1997), since the data were not deep enough to constrain both α and K * precisely. The evolution of K * with redshift is shown in the lower right panel of figure 1, along with lower redshift points from De Propris et al (1999). The models (described in the previous section) are normalised at low redshift to K * of the Coma cluster (De Propris et al 1998).…”

Section: Resultsmentioning

confidence: 99%

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The $K$-band luminosity functions of galaxies in high-redshift clusters

Ellis

Jones

2004

IAU

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Section: Resultssupporting

confidence: 89%

Section: Resultsmentioning

confidence: 53%

Section: Resultsmentioning

confidence: 99%

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The $K$-band luminosity functions of galaxies in high-redshift clusters

Ellis

Jones

2004

IAU

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“…They form such a distinctive population that their colours can be used to search for high redshift clusters in wide-field images (e.g., Gladders & Yee 2000;Eisenhardt et al 2008). These predominantly early type galaxies have little or no ongoing star formation subsequent to forming the bulk of their stellar populations and assembling their stellar masses at high redshift (e.g., Kodama & Arimoto 1997;Stanford et al 1998;De Propris et al 1999;Mancone et al 2010;Mei et al 2012 and references herein). However, while their stellar populations and luminosities evolve passively, their morphologies may not, and may also evolve differently from those of similarly passive field galaxies.…”

Section: Introductionmentioning

confidence: 99%

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Propris¹,

Bremer²,

Phillipps³

2016

Mon. Not. R. Astron. Soc.

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Galaxies arrive on the red sequences of clusters at high redshift (z > 1) once their star formation is quenched and evolve passively thereafter. However, we have previously found that cluster red sequence galaxies (CRSGs) undergo significant morphological evolution subsequent to the cessation of star formation, at some point in the past 9-10 Gyr. Through a detailed study of a large sample of cluster red sequence galaxies spanning 0.2 < z < 1.4 we elucidate the details of this evolution. Below z ∼ 0.5 − 0.6 (in the last 5-6 Gyr) there is little or no morphological evolution in the population as a whole, unlike in the previous 4-5 Gyrs. Over this earlier time (i) disklike systems with Sérsic n < 2 progressively disappear, as (ii) the range of their axial ratios similarly decreases, removing the most elongated systems (those consistent with thin disks seen at an appreciable inclination angle), and (iii) radial colour gradients (bluer outwards) decrease in an absolute sense from significant age-related gradients to a residual level consistent with the metallicity-induced gradients seen in low redshift cluster members. The distribution of their effective radii shows some evidence of evolution, consistent with growth of at most a factor < 1.5 between z ∼ 1.4 and z ∼ 0.5, significantly less than for comparable field galaxies, while the distribution of their central (< 1kpc) bulge surface densities shows no evolution at least at z < 1. A simple model involving the fading and thickening of a disk component after comparatively recent quenching (after z ∼ 1.5) around an otherwise passively evolving older spheroid component is consistent with all of these findings.

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“…z ! 1 and colors of these early-type galaxies evolve slowly with time and have very small scatter (e.g., Schade et al 1996;Stanford, Eisenhardt, & Dickinson 1998;van Dokkum et al 1998;De Propris et al 1999), indicating that the stars in early-type galaxies were formed at . z 1 2 On the other hand, there is growing evidence for morphological evolution among cluster galaxies.…”

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confidence: 99%

The Galaxy Population of Cluster RX J0848+4453 at [CLC][ITAL]z[/ITAL][/CLC] = 1.27

Dokkum

Stanford

Holden

et al. 2001

The Astrophysical Journal

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We present a study of the galaxy population in the IR-selected cluster RX J0848ϩ4453 at , using z p 1.27 deep Hubble Space Telescope (HST) NICMOS H F160W and WFPC2 I F814W images of the cluster core. We morphologically classify all galaxies to that are covered by the HST imaging and determine photometric K p 20.6 s redshifts using deep ground-based BRIzJK s photometry. Of 22 likely cluster members with morphological classifications, 11 (50%) are classified as early-type galaxies, nine (41%) as spiral galaxies, and two (9%) as "merger/ peculiar." At HST resolution, the second brightest cluster galaxy is resolved into a spectacular merger between three red galaxies of similar luminosity, separated from each other by ≈6 kpc, with an integrated magnitude Ϫ1 h 50 (∼3 at ). The two most luminous early-type galaxies also show evidence for recent or K p 17.6 L zp 1.27 * ongoing interactions. Mergers and interactions between galaxies are possible because RX J0848ϩ4453 is not yet relaxed. The fraction of early-type galaxies in our sample is similar to that in clusters at and consistent 0.5 ! z ! 1 with a gradual decrease of the number of early-type galaxies in clusters from to . We find evidence z p 0 z ≈ 1.3 that the color-magnitude relation of the early-type galaxies is less steep than in the nearby Coma Cluster. This may indicate that the brightest early-type galaxies have young stellar populations at but is also consistent z p 1.27 with predictions of single-age "monolithic" models with a galactic wind. The scatter in the color-magnitude relation is ≈0.04 in rest-frame UϪV, similar to that in clusters at . Taken together, these results show 0 ! z ! 1 that luminous early-type galaxies exist in clusters at but that their number density may be smaller than z ≈ 1.3 in the local universe. Additional observations are needed to determine whether the brightest early-type galaxies harbor young stellar populations.

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The [ITAL]K[/ITAL]-Band Luminosity Function in Galaxy Clusters to [CLC][ITAL]z[/ITAL][/CLC] [FORMULA][F]∼1[/F][/FORMULA]

Cited by 130 publications

References 63 publications

The $K$-band luminosity functions of galaxies in high-redshift clusters

The $K$-band luminosity functions of galaxies in high-redshift clusters

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

The Galaxy Population of Cluster RX J0848+4453 at [CLC][ITAL]z[/ITAL][/CLC] = 1.27

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