Probing galaxy evolution through the internal colour gradients, the Kormendy relations and the Photometric Plane of cluster galaxies at z ~ 0.2

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

doi:10.1051/0004-6361:20047157

Cited by 33 publications

(36 citation statements)

References 62 publications

(76 reference statements)

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“…We collect redshifts available from targeted studies on particular clusters in our samples (Lemonon et al 1997;Pierre et al 1997;Boschin et al 2004;La Barbera et al 2004;Barrena et al 2007a,b;Frye et al 2007;Maurogordato et al 2008;Girardi et al 2011;Owers et al 2011;Coe et al 2012; Figure 2. Normalised profiles of the NB filters used to survey Hα emitters at the redshift of our clusters.…”

Section: Ancillary Datamentioning

confidence: 99%

A large Hα survey of star formation in relaxed and merging galaxy cluster environments atz∼ 0.15–0.3

Stroe

Sobral

Afonso

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the first results from the largest Hα survey of star formation and AGN activity in galaxy clusters. Using 9 different narrow band filters, we select > 3000 Hα emitters within 19 clusters and their larger scale environment over a total volume of 1.3 × 10 5 Mpc 3 . The sample includes both relaxed and merging clusters, covering the 0.15 − 0.31 redshift range and spanning from 5 × 10 14 M to 30 × 10 14 M . We find that the Hα luminosity function (LF) for merging clusters has a higher characteristic density φ * compared to relaxed clusters. φ * drops from cluster core to cluster outskirts for both merging and relaxed clusters, with the merging cluster values ∼ 0.3 dex higher at each projected radius. The characteristic luminosity L * drops over the 0.5 − 2.0 Mpc distance from the cluster centre for merging clusters and increases for relaxed objects. Among disturbed objects, clusters hosting large-scale shock waves (traced by radio relics) are overdense in Hα emitters compared to those with turbulence in their intra-cluster medium (traced by radio haloes). We speculate that the increase in star formation activity in disturbed, young, massive galaxy clusters can be triggered by interactions between gas-rich galaxies, shocks and/or the intra-cluster medium, as well as accretion of filaments and galaxy groups. Our results indicate that disturbed clusters represent vastly different environments for galaxy evolution compared to relaxed clusters or average field environments.

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Section: Ancillary Datamentioning

confidence: 99%

A large Hα survey of star formation in relaxed and merging galaxy cluster environments atz∼ 0.15–0.3

Stroe

Sobral

Afonso

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The average age is a crude but robust way to represent the SFH of galaxies, and rest-frame optical colors are used extensively to obtain ages. Radial gradients of colors have been detected in bulges (Peletier et al 1990;Silva & Bothun 1998;La Barbera et al 2004;Menanteau et al 2004;Wu et al 2005;Moorthy & Holtzman, 2006;Roche et al 2010) and disks (Peletier & Balcells 1996;de Jong 1996;Peletier & de Grijs 1998;Bell & de Jong 2000;MacArthur et al 2004;Muñoz-Mateos et al 2007;Tortora et al 2010;Bakos et al 2008). Usually, a color gradient is interpreted as due to radial variations in age or metallicity, but because of the agemetallicity-extinction degeneracy, color gradients can also be related to metallicity and/or extinction gradients that are certainly present in the disks and central regions of massive galaxies.…”

Section: Introductionmentioning

confidence: 99%

The star formation history of CALIFA galaxies: Radial structures

Delgado

Pérez

Fernandes

et al. 2014

A&A

148

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We have studied the radial structure of the stellar mass surface density (µ * ) and stellar population age as a function of the total stellar mass and morphology for a sample of 107 galaxies from the CALIFA survey. We applied the fossil record method based on spectral synthesis techniques to recover the star formation history (SFH), resolved in space and time, in spheroidal and disk dominated galaxies with masses from 10 9 to 10 12 M . We derived the half-mass radius, and we found that galaxies are on average 15% more compact in mass than in light. The ratio of half-mass radius to half-light radius (HLR) shows a dual dependence with galaxy stellar mass; it decreases with increasing mass for disk galaxies, but is almost constant in spheroidal galaxies. In terms of integrated versus spatially resolved properties, we find that the galaxy-averaged stellar population age, stellar extinction, and µ * are well represented by their values at 1 HLR. Negative radial gradients of the stellar population ages are present in most of the galaxies, supporting an inside-out formation. The larger inner (≤1 HLR) age gradients occur in the most massive (10 11 M ) disk galaxies that have the most prominent bulges; shallower age gradients are obtained in spheroids of similar mass. Disk and spheroidal galaxies show negative µ * gradients that steepen with stellar mass. In spheroidal galaxies, µ * saturates at a critical value (∼7 × 10 2 M /pc 2 at 1 HLR) that is independent of the galaxy mass. Thus, all the massive spheroidal galaxies have similar local µ * at the same distance (in HLR units) from the nucleus. The SFH of the regions beyond 1 HLR are well correlated with their local µ * , and follow the same relation as the galaxy-averaged age and µ * ; this suggests that local stellar mass surface density preserves the SFH of disks. The SFH of bulges are, however, more fundamentally related to the total stellar mass, since the radial structure of the stellar age changes with galaxy mass even though all the spheroid dominated galaxies have similar radial structure in µ * . Thus, galaxy mass is a more fundamental property in spheroidal systems, while the local stellar mass surface density is more important in disks.

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“…Several authors have investigated the scaling relations of galaxies in clusters. Ziegler et al (1999), La Barbera et al (2004), Bernardi et al (2007), von der Linden et al (2007), Liu et al (2007) and Bildfell et al (2008). von der Linden et al (2007) found that brightest cluster galaxies (BCG) have a higher fraction of dark matter and consequently larger radii and higher velocity dispersions that non-BCG galaxies.…”

Section: Introductionmentioning

confidence: 99%

Galaxy properties in clusters: dependence on the environment and the cluster identification techniques

Coenda

Muriel

2009

A&A

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Aims. We investigate the dependence of several galaxy properties on the environment and cluster identification techniques. Methods. We select clusters of galaxies from two catalogues based on the SDSS: the ROSAT-SDSS galaxy cluster survey, which is an X-ray selected cluster sample and the MaxBCG catalogue, in which clusters are optically selected. Based on a volume limited sample of galaxies drawn from the spectroscopic DR5 SDSS, we constructed sub-samples of clusters of galaxies with more than ten members. Scaling relations as well as segregation of galaxy properties as a function of the normalized clustocentric radii are analyzed. The properties of galaxies in clusters are compared with those of field galaxies. Results. Galaxies in X-ray and MaxBCG selected clusters show similar size-luminosity relations. At equal luminosity, late type galaxies in the field have sizes smaller than cluster galaxies of the same morphological type. The Faber-Jackson relation for early-type galaxies in clusters is also the same for X-ray selected and MaxBCG clusters. We found clear differences between the dynamical properties of galaxies in clusters, the brightest cluster galaxies (BCG s ) and field galaxies. Using several criteria to classify galaxies into morphological types, we reproduce the well know morphological segregation. The correlation is up to r/r 200 ∼ 1. For the whole range of clustocentric distances, X-ray selected clusters present a higher fraction of early type galaxies than MaxBCG clusters. We also found that bright galaxies preferentially inhabit the cluster centers. Median sizes of galaxies, such as the radius that encloses 50% of Petrosian flux r 50 , present a behaviour that also depends on the cluster selection criteria. For galaxies in X-ray selected clusters, median values of r 50 decrease as r/r 200 goes to zero, whereas the opposite is observed for galaxies in the MaxBCG clusters. These different behaviours are mainly due to early type galaxies. The results are discussed in terms of the different processes that affect the evolution of galaxies in different environments.

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Probing galaxy evolution through the internal colour gradients, the Kormendy relations and the Photometric Plane of cluster galaxies at z ~ 0.2

Cited by 33 publications

References 62 publications

A large Hα survey of star formation in relaxed and merging galaxy cluster environments atz∼ 0.15–0.3

A large Hα survey of star formation in relaxed and merging galaxy cluster environments atz∼ 0.15–0.3

The star formation history of CALIFA galaxies: Radial structures

Galaxy properties in clusters: dependence on the environment and the cluster identification techniques

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