SDSS DR7 superclusters

Einasto, M.; Liivamägi, L. J.; Saar, E.; Einasto, J.; Tempel, Elmo; Tago, E.; Martı́nez, Vicent J.

doi:10.1051/0004-6361/201117529

Cited by 47 publications

(81 citation statements)

References 98 publications

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“…Poor spider-type superclusters are similar to our Local supercluster with one rich cluster and filaments of galaxies and poor groups of galaxies around it (Einasto et al 2007b). Einasto et al (2012a) analysed the structure of rich galaxy clusters in superclusters of different morphologies and showed that clusters in superclusters of spider morphology have higher probabilities of having substructure and their main galaxies have higher peculiar velocities than clusters in superclusters of filament morphology.…”

Section: Introductionmentioning

confidence: 62%

“…As a result, the maximum sizes in the sky projection and the velocity dispersions of our groups are similar at all distances. Our initial sample is chosen in the distance interval 120 h −1 Mpc ≤ d ≤ 340 h −1 Mpc (the redshift range 0.04 < z < 0.09) where the selection effects are the smallest (we discuss the selection effects in detail in Tago et al 2010;Einasto et al 2012a). The details of data reduction and the description of the group catalogue can be found in Tempel et al (2012).…”

Section: Galaxy Group and Supercluster Datamentioning

confidence: 99%

“…The morphology of all superclusters used in this study was determined in Einasto et al (2012a) applying Minkowski functionals. For a given surface the four Minkowski functionals are proportional to the enclosed volume V, the area of the surface S , the integrated mean curvature C, and the integrated Gaussian curvature χ (see Appendix B andEinasto et al 2007b, 2011a, for details and references).…”

Section: Galaxy Group and Supercluster Datamentioning

confidence: 99%

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SDSS superclusters: morphology and galaxy content

Einasto

Lietzen

Tempel

et al. 2014

A&A

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Context. Understanding the formation, evolution and present-day properties of the cosmic web and objects forming it is an important task in cosmology. Aims. We compare the galaxy populations in superclusters of different morphology in the nearby Universe (180 h −1 Mpc ≤ d ≤ 270 h −1 Mpc) to see whether the inner structure and overall morphology of superclusters are important in shaping galaxy properties in superclusters. Methods. We find supercluster morphology with Minkowski functionals and analyse the probability density distributions of colours, morphological types, stellar masses, star formation rate (SFR) of galaxies, and the peculiar velocities of the main galaxies in groups in superclusters of filament and spider types, and in the field. We test the statistical significance of the results with the KS test. Results. The fraction of red, early-type, low SFR galaxies in filament-type superclusters is higher than in spider-type superclusters; in low-density global environments their fraction is lower than in superclusters. In all environments the fraction of red, high stellar mass, and low SFR galaxies in rich groups is higher than in poor groups. In superclusters of spider morphology red, high SFR galaxies have higher stellar masses than in filament-type superclusters. Groups of equal richness host galaxies with larger stellar masses, a larger fraction of early-type and red galaxies, and a higher fraction of low SFR galaxies, if they are located in superclusters of filament morphology. The peculiar velocities of the main galaxies in groups from superclusters of filament morphology are higher than in those of spider morphology. Groups with higher peculiar velocities of their main galaxies in filament-type superclusters are located in higher density environment than those with low peculiar velocities. There are significant differences between galaxy populations of the individual richest superclusters. Conclusions. Both local (group) and global (supercluster) environments and even supercluster morphology play an important role in the formation and evolution of galaxies. Differences in the inner structure of superclusters of filament and spider morphology and the dynamical state of galaxy groups in them may lead to the differences found in our study.

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Section: Introductionmentioning

confidence: 62%

Section: Galaxy Group and Supercluster Datamentioning

confidence: 99%

Section: Galaxy Group and Supercluster Datamentioning

confidence: 99%

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SDSS superclusters: morphology and galaxy content

Einasto

Lietzen

Tempel

et al. 2014

A&A

Self Cite

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“…The morphology of superclusters up to a distance of 340 h −1 Mpc was determined in Einasto et al (2012a) who classified superclusters as filaments and spiders on the basis of their morphological information and visual appearance. The details about supercluster morphology are given in Einasto et al (2007cEinasto et al ( , 2011c.…”

Section: Luminosity Density Field and Superclustersmentioning

confidence: 99%

Unusual A2142 supercluster with a collapsing core: distribution of light and mass

Einasto

Gramann

Saar

et al. 2015

A&A

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Context. Superclusters of galaxies can be used to test cosmological models of the formation and evolution of the largest structures in the cosmic web, and of galaxy and cluster evolution in superclusters. Aims. We study the distribution, masses, and dynamical properties of galaxy groups in the A2142 supercluster. Methods. We analyse the global luminosity density distribution in the supercluster and divide the supercluster into the high-density core and the low-density outskirts regions. We find galaxy groups and filaments in these regions, calculate their masses and mass-tolight ratios and analyse their dynamical state with 1D and 3D statistics. We use the spherical collapse model to study the dynamical state of the supercluster. Results. In the A2142 supercluster rich groups and clusters lie along an almost straight line forming the 50 h −1 Mpc long main body of the supercluster. The A2142 supercluster has a very high density core surrounded by lower-density outskirts. The total estimated mass of the supercluster is M est = 6.2 × 10 15 M . More than a half of groups with at least ten member galaxies in the supercluster lie in the high-density core of the supercluster, centred at the X-ray cluster A2142. Most of the groups in the core region are multimodal. In the outskirts of the supercluster, the number of groups is larger than in the core, and groups are poorer. The orientation of the axis of the cluster A2142 follows the orientations of its X-ray substructures and radio halo, and is aligned along the supercluster axis. The high-density core of the supercluster with the global density D8 ≥ 17 and perhaps with D8 ≥ 13 may have started to collapse. Conclusions. A2142 supercluster with collapsing core and straight body, is an unusual object among superclusters. In the course of the future evolution, the supercluster may split into several systems.

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“…Furthermore, the properties of groups in superclusters, and galaxies in them, can be studied (Einasto et al 2003(Einasto et al , 2011(Einasto et al , 2012Lietzen et al 2012;Krause et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Tempel

Tamm

Gramann

et al. 2014

A&A

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230

488

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We provide flux-and volume-limited galaxy group and cluster catalogues based on the spectroscopic sample of the galaxies of SDSS data release 10. We used a modified friends-of-friends method with a variable linking length in the transverse and radial directions to identify as many realistic groups as possible. The flux-limited catalogue incorporates galaxies down to m r = 17.77 mag. It includes 588 193 galaxies and 82 458 groups. The volume-limited catalogues are complete for absolute magnitudes down to M r,lim = −18.0, −18.5, −19.0, −19.5, −20.0, −20.5, and −21.0; the completeness is achieved within different spatial volumes. Our analysis shows that flux-and volume-limited group samples are well compatible, especially for the larger groups/clusters. Dynamical mass estimates based on radial velocity dispersions and group extent in the sky were added to the extracted groups.

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SDSS DR7 superclusters

Cited by 47 publications

References 98 publications

SDSS superclusters: morphology and galaxy content

SDSS superclusters: morphology and galaxy content

Unusual A2142 supercluster with a collapsing core: distribution of light and mass

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

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