The red-sequence of 72 WINGS local galaxy clusters

Valentinuzzi, T.; Poggianti, Bianca M.; Fasano, G.; D’Onofrio, M.; Moretti, Alessia; Ramella, M.; Biviano, A.; Fritz, J.; Varela, J.; Bettoni, D.; Vulcani, Benedetta; Moles, M.; Couch, Warrick J.; Dressler, Alan; Kjærgaard, P.; Omizzolo, A.; Cava, A.

doi:10.1051/0004-6361/201117522

Cited by 47 publications

(49 citation statements)

References 84 publications

(126 reference statements)

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“…Our results indicate that pre-processing in groups leads to a strong evolution in galaxy properties, before they are accreted by large clusters. In agreement to Valentinuzzi et al (2011), we find that local density is the main driver for galaxy evolution and not the parent halo mass. The evolution is such that star formation is quenched in the group scale, but morphological transformation is a separate process, occurring in larger galaxy systems.…”

Section: Transitional Galaxy Populations: Blue Bulges and Red Discssupporting

confidence: 87%

NoSOCS in SDSS – V. Red disc and blue bulge galaxies across different environments

Lopes

Rembold

Ribeiro

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigated the typical environment and physical properties of "red discs" and "blue bulges", comparing those to the "normal" objects in the blue cloud and red sequence. Our sample is composed of cluster members and field galaxies at z ≤ 0.1, so that we can assess the impact of the local and global environment. We find that disc galaxies display a strong dependence on environment, becoming redder for higher densities. This effect is more pronounced for objects within the virial radius, being also strong related to the stellar mass. We find that local and global environment affect galaxy properties, but the most effective parameter is stellar mass. We find evidence for a scenario where "blue discs" are transformed into "red discs" as they grow in mass and move to the inner parts of clusters. From the metallicity differences of red and blue discs, and the analysis of their star formation histories, we suggest the quenching process is slow. We estimate a quenching time scale of ∼ 2−3 Gyr. We also find from the sSFR−M * plane that "red discs" gradually change as they move into clusters. The "blue bulges" have many similar properties than "blue discs", but some of the former show strong signs of asymmetry. The high asymmetry "blue bulges" display enhanced recent star formation compared to their regular counterparts. That indicates some of these systems may have increased their star formation due to mergers. Nonetheless, there may not be a single evolutionary path for these blue early-type objects.

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Section: Transitional Galaxy Populations: Blue Bulges and Red Discssupporting

confidence: 87%

NoSOCS in SDSS – V. Red disc and blue bulge galaxies across different environments

Lopes

Rembold

Ribeiro

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Popesso et al found significant suppression in the late type luminosity function (corresponding to our blue population) for small cluster-centric distances; we find that there is substantial change in the red luminosity function close to the cluster core as well. The colour-magnitude relation parameters drawn from the WINGS clusters (Valentinuzzi et al 2011) are quite similar to the values we see here, although the gradient scatter from our sample is twice as large as that from WINGS. That sample is also X-ray selected, but from clusters with lower Table 1.…”

Section: Discussionsupporting

confidence: 81%

“…Bower, Lucey & Ellis 1992;Valentinuzzi et al 2011). The origin of the red sequence and its relation to the massmetallicity relation was explored in a seminal paper by Arimoto & Yoshii (1987).…”

Section: Red Sequence Selectionmentioning

confidence: 99%

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Optical and X-ray profiles in the REXCESS sample of galaxy clusters*

Holland

Böhringer

Chon

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Galaxy clusters' structure, dominated by dark matter, is traced by member galaxies in the optical and hot intra-cluster medium (ICM) in X-rays. We compare the radial distribution of these components and determine the mass-to-light ratio vs. system mass relation.We use 14 clusters from the REXCESS sample which is representative of clusters detected in X-ray surveys. Photometric observations with the Wide Field Imager on the 2.2m MPG/ESO telescope are used to determine the number density profiles of the galaxy distribution out to r 200 . These are compared to electron density profiles of the ICM obtained using XMM-Newton, and dark matter profiles inferred from scaling relations and an NFW model.While red sequence galaxies trace the total matter profile, the blue galaxy distribution is much shallower. We see a deficit of faint galaxies in the central regions of massive and regular clusters, and strong suppression of bright and faint blue galaxies in the centres of cool-core clusters, attributable to ram pressure stripping of gas from blue galaxies in high density regions of ICM and disruption of faint galaxies due to galaxy interactions. We find a mass-to-light ratio vs. mass relation within r 200 of (3.0 ± 0.4) × 10 2 h M L −1 at 10 15 M with slope 0.16 ± 0.14, consistent with most previous results.

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“…We started by comparing the color-magnitude (CM) relation (B − V)(≤ r) − M V of clusters with the average red sequence slope found by Valentinuzzi et al (2011) for the WINGS galaxies in the CM diagrams of the single clusters. In Figure 10 …”

Section: Color-magnitude Diagram Of Galaxy Clustersmentioning

confidence: 99%

Characterization of Omega-WINGS galaxy clusters

Cariddi

D’Onofrio

Fasano

et al. 2018

A&A

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Context. Galaxy clusters are the largest virialized structures in the observable Universe. Knowledge of their properties provides many useful astrophysical and cosmological information. Aims. Our aim is to derive the luminosity and stellar mass profiles of the nearby galaxy clusters of the Omega-WINGS survey and to study the main scaling relations valid for such systems. Methods. We merged data from the WINGS and Omega-WINGS databases, sorted the sources according to the distance from the brightest cluster galaxy (BCG), and calculated the integrated luminosity profiles in the B and V bands, taking into account extinction, photometric and spatial completeness, K correction, and background contribution. Then, by exploiting the spectroscopic sample we derived the stellar mass profiles of the clusters. Results. We obtained the luminosity profiles of 46 galaxy clusters, reaching r 200 in 30 cases, and the stellar mass profiles of 42 of our objects. We successfully fitted all the integrated luminosity growth profiles with one or two embedded Sérsic components, deriving the main clusters parameters. Finally, we checked the main scaling relation among the clusters parameters in comparison with those obtained for a selected sample of early-type galaxies (ETGs) of the same clusters. Conclusions. We found that the nearby galaxy clusters are non-homologous structures such as ETGs and exhibit a color-magnitude (CM) red-sequence relation very similar to that observed for galaxies in clusters. These properties are not expected in the current cluster formation scenarios. In particular the existence of a CM relation for clusters, shown here for the first time, suggests that the baryonic structures grow and evolve in a similar way at all scales.

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The red-sequence of 72 WINGS local galaxy clusters

Cited by 47 publications

References 84 publications

NoSOCS in SDSS – V. Red disc and blue bulge galaxies across different environments

NoSOCS in SDSS – V. Red disc and blue bulge galaxies across different environments

Optical and X-ray profiles in the REXCESS sample of galaxy clusters*

Characterization of Omega-WINGS galaxy clusters

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