Quasi-spherical superclusters

Abstract

Context. Superclusters are systems with varied properties and varied fractional overdensities. Their dynamical state evolves under the influence of two components: dark energy and gravitational force. The dominant component at any spatial location and cosmic epoch is determined by the total mass and the local overdensity of the system. However, generally the dynamical state of superclusters is poorly known. Aims. We study properties of superclusters and select a sample of quasi-spherical superclusters, the dynamics of which can be studied using the Λ significance diagram. Methods. We extracted our supercluster sample with an adaptive local threshold density method from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) data and estimated their masses using the dynamical masses for member galaxies and groups. We used topological analysis based on Minkowski functionals and the positions of galaxies and galaxy groups in superclusters. Finally, we highlight the dynamical state of a few exceptional types of superclusters found in this study using the Λ significance diagram. Results. Our final sample contains 65 superclusters in the distance range of 130 to 450 Mpc. Supercluster masses range between 1.1 × 10 15 M and 1.4 × 10 16 M and sizes between 25 Mpc and 87 Mpc. We find that pancake-type superclusters form the lowluminosity, small, poor and low-mass end of superclusters. We find four superclusters of unusual types, exhibiting exceptionally spherical shapes. These so-called quasi-spherical systems contain a high-density core surrounded by a relatively spherical density and galaxy distribution. The mass-to-light ratio of these quasi-sphericals is higher than those of the other superclusters, suggesting a relatively high dark matter content. Using the Λ significance diagram for oblate and prolate spheroids, we find that three quasispherical superclusters are gravitationally bound at the present epoch. Conclusions. Quasi-spherical superclusters are among the largest gravitationally bound systems found to date, and form a special class of giant systems that, dynamically, are in between large gravitationally unbound superclusters and clusters of galaxies in an equilibrium configuration.

Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog

“…The topological analysis of the shape of superclusters may explain this phenomenon more clearly. Recently, Bag et al (2023) found that large superclusters with volumes 10 4 Mpc 3 tend to be more filamentary, and Heinämäki et al (2022) found that the low-luminosity, small, poor, and lowmass end of superclusters has pancake-type shapes, while only a handful exhibit exceptionally spherical shapes. The supercluster environment weakly affects the evolution of clusters.…”