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

Coenda, Valeria; Muriel, H.

doi:10.1051/0004-6361/200811504

Cited by 15 publications

(19 citation statements)

References 89 publications

(116 reference statements)

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“…As expected, brighter galaxies are larger, as previously found in several environments independently of the morphological types (e.g. Coenda et al 2005;Bernardi et al 2007; von der Linden et al 2007;Coenda & Muriel 2009;Nair et al 2010).…”

Section: Colour-magnitude Diagram: Red Sequencesupporting

confidence: 87%

“…12. The curvature in the luminositysize relation was previously reported by Bernardi et al (2007) and Coenda & Muriel (2009). Taking into account the error-bars, the differences among the different sequences in Fig.…”

Section: Luminosity-size Relationsupporting

confidence: 75%

“…On the other hand, several authors have found that the size-luminosity relationship for early-type galaxies varies depending on whether the galaxies are central, satellite, or inhabit the field (e.g. Coenda & Muriel 2009;Bernardi 2009). …”

Section: Introductionmentioning

confidence: 99%

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Comparing galaxy populations in compact and loose groups of galaxies

Coenda

Muriel

Martínez

2012

A&A

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Aims. We compare the properties of galaxies in compact groups, loose groups, and the field to deepen our understanding of the physical mechanisms acting upon galaxy evolution in different environments. Methods. We select samples of galaxies in compact groups, loose groups, and field galaxies from the Sloan Digital Sky Survey. We compare the properties of the galaxy populations in these different environments: absolute magnitude, colour, size, surface brightness, stellar mass, and concentration. We also study the fraction of red and early-type galaxies, the luminosity function, the colourluminosity, and luminosity-size relations.Results. The population of galaxies in compact groups differ from that of loose groups and the field. The fraction of red and early-type galaxies is larger in compact groups. Galaxies in compact groups are, on average, systematically smaller in size, more concentrated, and have higher surface brightnesses than galaxies in the field and in loose groups. At a fixed absolute magnitude, or fixed surface brightness, galaxies in compact groups are smaller in size. Conclusions. The physical mechanisms that transform galaxies into earlier types could be more effective within compact groups, owing to the typically high densities and small velocity dispersions of these environments, which could explain the large fraction of red and early-type galaxies we found in compact groups. Galaxies inhabiting compact groups have undergone a major transformation compared to galaxies that inhabit loose groups.

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Section: Colour-magnitude Diagram: Red Sequencesupporting

confidence: 87%

Section: Luminosity-size Relationsupporting

confidence: 75%

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Comparing galaxy populations in compact and loose groups of galaxies

Coenda

Muriel

Martínez

2012

A&A

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“…For this purpose, we use the sample of galaxies in clusters selected by Coenda & Muriel (2009;hereafter Paper I) plus a new subsample of X-ray clusters obtained by crosscorrelating the Northern ROSAT All-Sky Galaxy Cluster Survey (NORAS; Bohringer et al 2000, hereafter B00) with the Sloan Digital Sky Survey (SDSS; York et al 2000). We have analysed a wide range of properties of high-and low-velocity subsamples of cluster members with clustocentric distances 1 < r/r vir < 2 in the redshift range 0.05 < z < 0.10.…”

Section: Introductionmentioning

confidence: 99%

Galaxy properties in clusters

Muriel

Coenda

2014

A&A

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Aims. We explore the properties of galaxies on the outskirts of clusters and their dependence on recent dynamical history in order to understand the real impact that the cluster core has on the evolution of galaxies. Methods. We analyse the properties of more than 1000 galaxies brighter than M0.1 r = −19.6 on the outskirts of 90 clusters (1 < r/r vir < 2) in the redshift range 0.05 < z < 0.10. Using the line of sight velocity of galaxies relative to the cluster's mean, we selected low and high velocity subsamples. Theoretical predictions indicate that a significant fraction of the first subsample should be backsplash galaxies, that is, objects that have already orbited near the cluster centre. A significant proportion of the sample of high relative velocity (HV) galaxies seems to be composed of infalling objects. Results. Our results suggest that, at fixed stellar mass, late-type galaxies in the low-velocity (LV) sample are systematically older, redder, and have formed fewer stars during the last 3 Gyrs than galaxies in the HV sample. This result is consistent with models that assume that the central regions of clusters are effective in quenching the star formation by means of processes such as ram pressure stripping or strangulation. At fixed stellar mass, LV galaxies show some evidence of having higher surface brightness and smaller size than HV galaxies. These results are consistent with the scenario where galaxies that have orbited the central regions of clusters are more likely to suffer tidal effects, producing loss of mass as well as a re-distribution of matter towards more compact configurations. Finally, we found a higher fraction of ET galaxies in the LV sample, supporting the idea that the central region of clusters of galaxies may contribute to the transformation of morphological types towards earlier types.

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“…These results can be related to the different processes that affect the evolution of galaxies in various environments. References: Coenda and Muriel (2009).…”

Section: Galaxy Properties In Clusters: Dependence On the Environmentmentioning

confidence: 99%

JD2 - Diffuse Light in Galaxy Clusters

Arnaboldi

Gerhard

2009

Proc. IAU

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Abstract. Diffuse intracluster light (ICL) has now been observed in nearby and in intermediate redshift clusters. Individual intracluster stars have been detected in the Virgo and Coma clusters and the first color-magnitude diagram and velocity measurements have been obtained. Recent studies show that the ICL contains of the order of 10% and perhaps up to 30% of the stellar mass in the cluster, but in the cores of some dense and rich clusters like Coma, the local ICL fraction can be high as 40%-50%. What can we learn from the ICL about the formation of galaxy clusters and the evolution of cluster galaxies? How and when did the ICL form? What is the connection to the central brightest cluster galaxy? Cosmological N-body and hydrodynamical simulations are beginning to make predictions for the kinematics and origin of the ICL. The ICL traces the evolution of baryonic substructures in dense environments and can thus be used to constrain some aspects of cosmological simulations that are most uncertain, such as the modeling of star formation and the mass distribution of the baryonic component in galaxies.

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

Cited by 15 publications

References 89 publications

Comparing galaxy populations in compact and loose groups of galaxies

Comparing galaxy populations in compact and loose groups of galaxies

Galaxy properties in clusters

JD2 - Diffuse Light in Galaxy Clusters

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