Astronomy and Astrophysics, volume 587A, 116-116 (2016/3-1)
Shell-like structures in our cosmic neighbourhood.
EINASTO M., HEINAEMAEKI P., LIIVAMAEGI L.J., MARTINEZ V.J., HURTADO-GIL L., ARNALTE-MUR P., NURMI P., EINASTO J. and SAAR E.
Abstract (from CDS):
Signatures of the processes in the early Universe are imprinted in the cosmic web. Some of them may define shell-like structures characterised by typical scales. Examples of such structures are shell-like systems of galaxies, which are interpreted as a signatures of the baryon acoustic oscillations. We search for shell-like structures in the distribution of nearby rich clusters of galaxies drawn from the SDSS DR8. We calculated the distance distributions between rich clusters of galaxies and groups and clusters of various richness, searched for the maxima in the distance distributions and selected candidates of shell-like structures. We analysed the space distribution of groups and clusters that form shell walls. We find six possible candidates of shell-like structures, in which galaxy clusters have the maximum in their distance distribution to other galaxy groups and clusters at a distance of about 120-130h–1Mpc. Another, less probable maximum is found at a distance of about 240h–1Mpc. The rich galaxy cluster A1795, which is the central cluster of the Bootes supercluster, has the highest maximum in the distance distribution of all other surrounding groups and clusters in our rich cluster sample. It lies at a distance of about 120h–1Mpc. The structures of galaxy systems that cause this maximum form an almost complete shell of galaxy groups, clusters, and superclusters. The richest systems in the nearby universe, the Sloan Great Wall, the Corona Borealis supercluster, and the Ursa Major supercluster, are among them. The probability that we obtain maxima like this from random distributions is lower than 0.001. Our results confirm that shell-like structures can be found in the distribution of nearby galaxies and their systems. The radii of the possible shells are larger than expected for a baryonic acoustic oscillations (BAO) shell (≃109h–1Mpc versus ≃120-130h–1Mpc), and they are determined by very rich galaxy clusters and superclusters. In contrast, BAO shells are barely seen in the galaxy distribution. We discuss possible consequences of these differences.
large-scale structure of Universe - galaxies: clusters: general
Table 1 objects not identified.
View the reference in ADS
To bookmark this query, right click on this link: simbad:2016A&A...587A.116E and select 'bookmark this link' or equivalent in the popup menu