Deep luminosity functions and colour–magnitude relations for cluster galaxies at 0.2 &lt; z &lt; 0.6

Propris, Roberto De; Phillipps, S.; Bremer, M. N.

doi:10.1093/mnras/stt1262

Cited by 52 publications

(75 citation statements)

References 83 publications

(112 reference statements)

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“…Andreon 2006;De Propris et al 2007. De Propris et al (2013) wrote that surface brightness selection effects could account for claims of evolution at the faint end. Observations with various surface brightness limits are required to confirm this hypothesis.…”

Section: The Faint End Of the Glfmentioning

confidence: 99%

“…De Propris et al 1999Propris et al , 2007Propris et al , 2013De Lucia et al 2004Andreon 2006;Muzzin et al 2008;Mancone et al 2010Mancone et al , 2012). This scenario is strongly supported by the lack of evolution in the colour−magnitude relation for the bright galaxies in clusters from z = 1 to z = 0 (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Smail et al 1998;De Lucia et al 2004Tanaka et al 2005;Stott et al 2007;Gilbank et al 2008;Rudnick et al 2009;Vulcani et al 2011) or remain constant with redshift (e.g. De Propris et al 2003Propris et al , 2007Propris et al , 2013Andreon 2006). The first type of behaviour is the most commonly observed, but the cold dark matter scenario predicts a larger number of low mass galaxies Rudnick et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: The Faint End Of the Glfmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…stellar synthesis models generated by EZGal 16 . These models were normalized to a lower redshift (z ∼ 0.6) L * cluster galaxy in the observed-frame F814W band (De Propris et al 2013) and generated for a variety of different formation epochs and at a variety of different metallicities. As a rough check, we note that the galaxy properties generated by these models show broad agreement in the observed-frame K band with L * galaxies at similar redshifts (z ∼ 3−4) observed in photometric surveys and in simulations (e.g., Cirasuolo et al 2010;Henriques et al 2012;Muzzin et al 2013).…”

Section: The Density Of Massive Galaxies In CL J0227-0421mentioning

confidence: 99%

VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

Lemaux

Cucciati

Tasca

et al. 2014

A&A

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Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we performed a systematic search for overdense environments in the early universe (z > 2) and report here on the discovery of Cl J0227-0421, a massive protocluster at z = 3.29. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, δ gal = 10.5 ± 2.8, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated by a variety of methods to be ∼3 × 10 14 M at z ∼ 3.3, which, evolved to z = 0 results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy, which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics that are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates among and differences in the stacked spectra of member galaxies with respect to the field, we defer any conclusions about these trends to future work with the ensemble of protostructures that are found in the full VUDS sample.

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“…These galaxies then evolve passively in the subsequent time (e.g. Andreon 2008; De Propris, Phillipps & Bremer 2013). Nonetheless, the details of how these massive passive cluster galaxies formed and evolved, in particular the physical processes involved, remains a matter of debate.…”

Section: Introductionmentioning

confidence: 99%

Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

Chan

Beifiori

Mendel

et al. 2016

Mon. Not. R. Astron. Soc.

137

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(2016) 'Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 at z = 1.39.', Monthly notices of the Royal Astronomical Society., 458 (3). pp. 3181-3209. Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe analyse the sizes, colour gradients, and resolved stellar mass distributions for 36 massive and passive galaxies in the cluster XMMUJ2235-2557 at z = 1.39 using optical and nearinfrared Hubble Space Telescope imaging. We derive light-weighted Sérsic fits in five HST bands (i 775 , z 850 ,Y 105 , J 125 , H 160 ), and find that the size decreases by ∼ 20% going from i 775 to H 160 band, consistent with recent studies. We then generate spatially resolved stellar mass maps using an empirical relationship between M * /L H 160 and (z 850 − H 160 ) and use these to derive mass-weighted Sérsic fits: the mass-weighted sizes are ∼ 41% smaller than their restframe r-band counterparts compared with an average of ∼ 12% at z ∼ 0. We attribute this evolution to the evolution in the M * /L H 160 and colour gradient. Indeed, as expected, the ratio of mass-weighted to light-weighted size is correlated with the M * /L gradient, but is also mildly correlated with the mass surface density and mass-weighted size. The colour gradients (∇ z−H ) are mostly negative, with a median value of ∼ 0.45 mag dex −1 , twice the local value. The evolution is caused by an evolution in age gradients along the semi-major axis (a), with ∇ age = d log(age)/d log(a) ∼ −0.33, while the survival of weaker colour gradients in old, local galaxies implies that metallicity gradients are also required, with ∇ Z = d log(Z)/d log(a) ∼ −0.2. This is consistent with recent observational evidence for the inside-out growth of passive galaxies at high redshift, and favours a gradual mass growth mechanism, such as minor mergers.

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Deep luminosity functions and colour–magnitude relations for cluster galaxies at 0.2 < z < 0.6

Cited by 52 publications

References 83 publications

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

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

VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

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