Superclusters of galaxies from the 2dF redshift survey

Einasto, J.; Einasto, M.; Saar, E.; Tago, E.; Liivamägi, L. J.; Jõeveer, M.; Suhhonenko, I.; Hütsi, Gert; Jaaniste, J.; Heinämäki, P.; Müller, V.; Knebe, Alexander; Tucker, D. L.

doi:10.1051/0004-6361:20065501

Cited by 55 publications

(51 citation statements)

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“…The mean and maximum number densities of galaxies in rich superclusters are higher than in poor superclusters. Rich superclusters are more asymmetrical than poor superclusters (Einasto et al 2007a). Rich superclusters contain high-density cores (Einasto et al 2007c).…”

Section: Comparison With Other Studiesmentioning

confidence: 99%

“…The overall morphology of superclusters has been studied by several authors (Kolokotronis et al 2002;Basilakos 2003;Costa-Duarte et al 2011), we refer to Einasto et al (2007a) for a review of the properties of superclusters. The shapes and sizes of superclusters can be used to compare the observed superclusters with those obtained from cosmological simulations (Kolokotronis et al 2002;Einasto et al 2007a).…”

Section: Introductionmentioning

confidence: 99%

“…The shapes and sizes of superclusters can be used to compare the observed superclusters with those obtained from cosmological simulations (Kolokotronis et al 2002;Einasto et al 2007a). Nichol et al (2006) showed that the higher order correlation functions of the 2dFGRS do not agree with those found in numerical simulations (but this fact can be explained by non-Gaussian initial density fields, Gaztanaga & Maehoenen 1996).…”

Section: Introductionmentioning

confidence: 99%

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SDSS DR7 superclusters

Einasto

Liivamägi

Tago

et al. 2011

A&A

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Aims. We study the morphology of a set of superclusters drawn from the SDSS DR7. Methods. We calculate the luminosity density field to determine superclusters from a flux-limited sample of galaxies from SDSS DR7 and select superclusters with 300 and more galaxies for our study. We characterise the morphology of superclusters using the fourth Minkowski functional V 3 , the morphological signature (the curve in the shapefinder's K 1 -K 2 plane) and the shape parameter (the ratio of the shapefinders K 1 /K 2 ). We investigate the supercluster sample using multidimensional normal mixture modelling. We use Abell clusters to identify our superclusters with known superclusters and to study the large-scale distribution of superclusters. Results. The superclusters in our sample form three chains of superclusters; one of them is the Sloan Great Wall. Most superclusters have filament-like overall shapes. Superclusters can be divided into two sets; more elongated superclusters are more luminous, richer, have larger diameters and a more complex fine structure than less elongated superclusters. The fine structure of superclusters can be divided into four main morphological types: spiders, multispiders, filaments, and multibranching filaments. We present the 2D and 3D distribution of galaxies and rich groups, the fourth Minkowski functional, and the morphological signature for all superclusters. Conclusions. Widely different morphologies of superclusters show that their evolution has been dissimilar. A study of a larger sample of superclusters from observations and simulations is needed to understand the morphological variety of superclusters and the possible connection between the morphology of superclusters and their large-scale environment.

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Section: Comparison With Other Studiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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SDSS DR7 superclusters

Einasto

Liivamägi

Tago

et al. 2011

A&A

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“…intermediate redshifts. Deeper spectroscopic surveys will certainly change that, as can be extrapolated from Einasto et al (2007a) who identified 543 superclusters with z < 0.2.…”

Section: Introductionmentioning

confidence: 99%

Mass, light and colour of the cosmic web in the supercluster SCL2243-0935 (z = 0.447)

Schirmer

Hildebrandt

Kuijken

et al. 2011

A&A

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AstrophysicsMass, light and colour of the cosmic web in the supercluster SCL2243-0935 (z = 0.447) , ABSTRACTAims. In archival 2.2 m MPG-ESO/WFI data we discovered several mass peaks through weak gravitational lensing, forming a possible supercluster at redshift 0.45. Through wide-field imaging and spectroscopy we aim to identify the supercluster centre, confirm individual member clusters, and detect possible connecting filaments. Methods. Through multi-colour imaging with CFHT/Megaprime and INT/WFC we identify a population of early-type galaxies and use it to trace the supercluster network. EMMI/NTT multi-object spectroscopy is used to verify the initial shear-selected cluster candidates. We use weak gravitational lensing to obtain mass estimates for the supercluster centre and the filaments. Results. We identified the centre of the SCL2243-0935 supercluster, MACS J2243-0935, which was found independently by Ebeling et al. (2001Ebeling et al. ( , 2010. We found 13 more clusters or overdensities embedded in a large filamentary network. Spectroscopic confirmation for about half of them is still pending. Three Integrating the weak lensing surface mass density over the supercluster network (defined by increased i-band luminosity or g − i colours), we find (1.53 ± 1.01) × 10 15 M and M/L = 305 ± 201 for the three main filaments, consistant with theoretical predictions. The filaments' projected dimensionless surface mass density κ varies between 0.007−0.012, corresponding to ρ/ρ crit = 10−100 depending on location and de-projection. The greatly varying density of the cosmic web is also reflected in the mean colour of galaxies, e.g. g − i = 2.27 mag for the supercluster centre and 1.80 mag for the filaments. Conclusions. SCL2243 is significantly larger and much more richly structured than other known superclusters such as A901/902 or MS0302 studied with weak lensing before. It is a text-book supercluster with little contamination along the line of sight, making it a perfect sandbox for testing new techniques probing the cosmic web.

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“…These studies have revealed that in richer superclusters groups and clusters of galaxies are also richer, and they contain a larger fraction of red, non-star forming galaxies than poor superclusters (Einasto et al 2007(Einasto et al , 2007a.…”

Section: Introductionmentioning

confidence: 99%

SDSS superclusters: morphology and galaxy content

Einasto

Lietzen

Tempel

et al. 2014

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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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Superclusters of galaxies from the 2dF redshift survey

Cited by 55 publications

References 48 publications

SDSS DR7 superclusters

SDSS DR7 superclusters

Mass, light and colour of the cosmic web in the supercluster SCL2243-0935 (z = 0.447)

SDSS superclusters: morphology and galaxy content

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