EDP Sciences
Free Access
Volume 476, Number 2, December III 2007
Page(s) 697 - 711
Section Cosmology (including clusters of galaxies)
DOI https://doi.org/10.1051/0004-6361:20078037
Published online 23 October 2007

A&A 476, 697-711 (2007)
DOI: 10.1051/0004-6361:20078037

The richest superclusters

I. Morphology
M. Einasto1, E. Saar1, L. J. Liivamägi1, J. Einasto1, E. Tago1, V. J. Martínez2, J.-L. Starck3, V. Müller4, P. Heinämäki5, P. Nurmi5, M. Gramann1, and G. Hütsi1

1  Tartu Observatory, 61602 Tõravere, Estonia
    e-mail: maret@aai.ee
2  Observatori Astronòmic, Universitat de València, Apartat de Correus 22085, 46071 València, Spain
3  CEA-Saclay, DAPNIA/SEDI-SAP, Service d'Astrophysique, 91191 Gif-sur-Yvette, France
4  Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
5  Turku University, Tuorla Observatory, Väisäläntie 20, Piikkiö, Finland

(Received 8 June 2007 / Accepted 2 October 2007)

Context.Superclusters are the largest systems in the Universe to give us information about the formation and evolution of structures in the very early Universe. Our present series of papers is devoted to the study of the morphology and internal structure of superclusters of galaxies.
Aims. We study the morphology of the richest superclusters from the catalogs of superclusters of galaxies in the 2dF Galaxy Redshift Survey and compare the morphology of real superclusters with model superclusters in the Millennium Simulation.
Methods.We use Minkowski functionals and shapefinders to quantify the morphology of superclusters: their sizes, shapes, and clumpiness. We generate empirical models of simple geometry to understand which morphologies correspond to the supercluster shapefinders (Appendix A).
Results. Rich superclusters have elongated, filamentary shapes with high-density clumps in their core regions. The clumpiness of superclusters is determined using the fourth Minkowski functional V3. In the K1-K2 shapefinder plane the morphology of superclusters is described by a curve which is characteristic of multi-branching filaments as shown by our empirical models.

We found several differences between observed and model superclusters. The curves of the fourth Minkowski functional V3 for observed and model superclusters have different shapes indicating that their structure is different. The values of V3 for the supercluster SCL126 (the Sloan Great Wall) show that this supercluster has a very high density core which is absent in other superclusters. The values of the shapefinders H1-H3 and K1 and K2 for observed superclusters have much larger scatter than for model superclusters. The differences between the fourth Minkowski functional V3 for the bright and faint galaxies in observed superclusters are larger than in simulated superclusters.
Conclusions.Our results show how the Minkowski functionals and shapefinders can be used to describe the morphology of superclusters: their shapes, sizes and clumpiness.

The shapes of observed superclusters are more diverse than the shapes of simulated superclusters. The larger scatter of the fourth Minkowski functional V3 for the bright and faint galaxies for observed superclusters compared to simulated superclusters is an indication that the clumpiness of bright and faint galaxies in models does not reflect well the clumpiness of different galaxies in observed superclusters.

Our results suggest also that the volume covered by the Millennium Simulations may be too small to properly describe the large morphological variety of superclusters.

Key words: cosmology: large-scale structure of Universe -- galaxies: clusters

© ESO 2007

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.