Evolution of UV–NIR structural properties of cluster galaxies

Barbera, F. La; Busarello, G.; Massarotti, M.; Merluzzi, P.; Mercurio, A.

doi:10.1051/0004-6361:20030780

Cited by 28 publications

(51 citation statements)

References 42 publications

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“…At these redshifts we also confirm the existence of a mild trend with luminosity (and presumably stellar mass) extending over 3-4 magnitudes, in the sense that fainter galaxies have milder colour gradients, as seen in the Coma cluster . This relationship appears to persist at least out to z ∼ 0.6 in agreement with earlier studies by La Barbera et al (2003). Linear fits (with minimum absolute deviation) to the data are shown for the 'low' and 'mid' redshift bins in Fig.…”

Section: Colour Gradients Evolutionsupporting

confidence: 89%

“…Local early-type galaxies tend to show slightly bluer colours outwards, consistent with the existence of a metal abundance gradient (e.g., Saglia et al 2000;Tamura & Ohta 2000). Based on the measured colour gradients of La Barbera et al (2003) it appears that cluster galaxies are already similar to local early-type galaxies in this respect by z = 0.6. Our sample in Paper I showed significantly larger gradients (also bluer outwards) at z = 1.3, more consistent with the existence of age gradients and more similar to the evolution seen by La Barbera et al (2003) in their sample of disks.…”

Section: Introductionsupporting

confidence: 64%

“…Based on the measured colour gradients of La Barbera et al (2003) it appears that cluster galaxies are already similar to local early-type galaxies in this respect by z = 0.6. Our sample in Paper I showed significantly larger gradients (also bluer outwards) at z = 1.3, more consistent with the existence of age gradients and more similar to the evolution seen by La Barbera et al (2003) in their sample of disks. Together with the evidence for disklike components and more flattened shapes (e.g., Papovich et al 2012; see Figure 7 in Paper I), we argued in Paper I that a population of recently quenched thin disks transforms into the local population of CRSGs (dominated by E/S0 galaxies) largely by mechanisms that do not change stellar mass (given the observed passive evolution of the luminosity function) or overall sizes (as those of our sample were broadly consistent with local values as measured in the Virgo cluster).…”

Section: Introductionmentioning

confidence: 92%

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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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Section: Colour Gradients Evolutionsupporting

confidence: 89%

Section: Introductionsupporting

confidence: 64%

Section: Introductionmentioning

confidence: 92%

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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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“…However, the scaling relations and, in particular, the zero point and the slope obtained using the whole sample of E and S0 galaxies do not differ from those obtained separately from S0 and E (Jørgensen et al 1996). This relation is the one most commonly used as reference for the local cluster galaxies (e.g., La Barbera et al 2003Barbera et al , 2010Di Serego Alighieri et al 2005;Saglia et al 2010;Raichoor et al 2012) and it is best suited to comparison with the one we derive from our galaxies at z = 1.27, given their properties.…”

Section: Comparison Data In the Local Universementioning

confidence: 57%

“…Elliptical galaxies both in field and in clusters follow this tight relation with a slope close to three out to z ∼ 1 (Hamabe & Kormendy 1987;Schade et al 1996;Ziegler et al 1999;La Barbera et al 2003Reda et al 2004;di Serego Alighieri et al 2005). On the other hand, the zero point α is found to vary with the redshift of the galaxies, reflecting their luminosity evolution and the possible evolution of R e over time.…”

Section: The Kormendy Relation At Z = 13mentioning

confidence: 92%

Scaling relations of cluster elliptical galaxies atz~ 1.3

Saracco

Casati

Gargiulo

et al. 2014

A&A

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Context. We studied the size-surface brightness and the size-mass relations of a sample of 16 cluster elliptical galaxies in the mass range ∼1010 −2 × 10 11 M , which were morphologically selected in the cluster RDCS J0848+4453 at z = 1.27. Aims. Our aim is to assess whether they have completed their mass growth at their redshift or significant mass, and/or size growth can or must still take place until z = 0. This will enable us to know whether the elliptical galaxies of clusters follow or not the observed size evolution of passive galaxies. Methods. To compare our data with the local universe we considered the Kormendy relation derived from the early-type galaxies of a local Coma Cluster reference sample and the WINGS survey sample. The comparison with the local Kormendy relation shows that the luminosity evolution due to the aging of the stellar content already assembled at z = 1.27 brings them on the local relation. Moreover, this stellar content places them on the size-mass relation of the local cluster ellipticals. These results imply that for a given mass, the stellar mass at z ∼ 1.3 is distributed within these ellipticals according to the same stellar mass profile of local ellipticals. We find that a pure size evolution, even mild, is ruled out for our galaxies since it would lead them away from both the Kormendy and the size-mass relation. If an evolution of the effective radius takes place, this must be compensated by an increase in the luminosity, hence of the stellar mass of the galaxies, to keep them on the local relations. We show that to follow the Kormendy relation, the stellar mass must increase as the effective radius. However, this mass growth is not sufficient to keep the galaxies on the size-mass relation for the same variation in effective radius. Thus, if we want to preserve the Kormendy relation, we fail to satisfy the size-mass relation and vice versa. Results. The combined analysis of the size-surface brightness relation with the size-mass relation leads to the result that these galaxies cannot increase solely in size and cannot significantly grow in mass. Conclusions. We conclude that these 16 cluster ellipticals at z = 1.27 have, for the most part, completed their stellar mass growth at the redshift they are and that consequently, their evolution at z < 1.27 will be dominated by the aging of their stellar content. If this result is generalizable, then it shows that elliptical galaxies in the above mass range do not contribute to the observed size evolution of passive galaxies, as also found by other authors. This evolution would be instead mainly driven by disk galaxies. We do not find hints of differences between the properties of these cluster ellipticals and those of field ellipticals at comparable redshift, even if this last comparison is still based on a low number statistics.

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Color gradients reflect an inside-out growth in early-type galaxies of the cluster MACS J1206.2-0847

Marian

Ziegler

Kuchner

et al. 2018

A&A

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Aims. Color gradients of galaxies are a powerful tool for resolving the variations of stellar populations within galaxies. We use this approach to explore the evolution of early-type galaxies in the core of the massive galaxy cluster MACS J1206.2-0847 at z = 0.44. Methods. We used imaging data in 12 filters (covering a wavelength range from 400 − 1600nm) from the Hubble Space Telescope provided by the CLASH survey, as well as additional spectral information from its follow-up program, CLASH-VLT. We performed multiwavelength optimized model fitting using Galapagos-2 from the MegaMorph project to measure their photometric parameters (total integrated magnitudes, effective radii r e , and Sérsic indices n). We used them to derive color gradients for the colors g 475 − I 814 , r 625 − Y 105 , I 814 − H 160 , and Y 105 − H 160 at radii ranging between 0.1 -2 r e for 79 early-type cluster galaxies. From synthetic spectral models that use simple star formation recipes, we inferred ages and metallicities of the stellar population at different locations within each galaxy and characterized their influence on the radial color trends. Results. Early-type galaxies show a substantial decrease in effective radii r e with wavelength. We measure that galaxy sizes are ∼25 % smaller in the red H 160 filter than in the blue r 625 filter but maintain a constant (within 3σ) Sérsic index n with wavelength. We find negative color gradients in all colors with slopes ranging between -0.07 and -0.17 mag dex −1 and with no obvious dependence on total magnitude, stellar mass, or location inside the cluster core. We explain the observed radial trends of color gradients as a result of the ages and metallicities of the respective stellar populations. Red galaxy cores are typically ∼3 Gyr older and more enriched in metals than the galaxy outskirts, which are of solar metallicity. Conclusions. Our results support the predictions from hydrodynamical cosmological simulations, which describe a passive evolution combined with an inside-out-growth of early-type galaxies. In this scenario, galaxies assemble their stellar mass primarily in the outskirts through the accretion of mass-poor satellites and thus manifest the observed trends of color-, metallicity-and age gradients.

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Evolution of UV–NIR structural properties of cluster galaxies

Cited by 28 publications

References 42 publications

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

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

Scaling relations of cluster elliptical galaxies atz~ 1.3

Color gradients reflect an inside-out growth in early-type galaxies of the cluster MACS J1206.2-0847

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