The spatial distribution of galaxies within the CMB cold spot in the Corona Borealis supercluster

TL;DR

This study investigates the distribution and colors of galaxies within a CMB cold spot in the Corona Borealis supercluster, revealing inhomogeneous galaxy densities, a filament structure, and potential background cluster signatures.

Contribution

It provides the first detailed analysis of galaxy spatial distribution and color properties within this specific CMB cold spot, identifying possible new structures.

Findings

Inhomogeneous galaxy distribution with a prominent filament

Excess of faint, red galaxies indicating possible background cluster

Radial dependence of galaxy overdensity extending up to 15 arcmin

Abstract

We study the spatial distribution and colours of galaxies within the region covered by the cold spot in the cosmic microwave background (CMB) recently detected by the Very Small Array (VSA; Genova-Santos et al. 2005, 2008) towards the Corona Borealis supercluster (CrB-SC). The spot is in the northern part of a region with a radius ~1 degree (~5 Mpc at the redshift of CrB-SC) enclosing the clusters Abell 2056, 2065, 2059 and 2073, and where the density of galaxies, excluding the contribution from those clusters, is ~2 times higher than the mean value in typical intercluster regions of the CrB-SC. Two of such clusters (Abell 2056 and 2065) are members of the CrB-SC, while the other two are in the background. This high density intercluster region is quite inhomogeneous, being the most remarkable feature a large concentration of galaxies in a narrow filament running from Abell 2065 with a length of ~35 arcmin (~3 Mpc at the redshift of CrB-SC) in the SW-NE direction. This intercluster population of galaxies probably results from the interaction of clusters Abell 2065 and 2056. The area subtended by the VSA cold spot shows an excess of faint (21<r<22) and red (1.1<r-i<1.3) galaxies as compared with typical values within the CrB-SC intercluster regions. This overdensity of galaxies shows a radial dependence and extends out to ~15 arcmin. This could be signature of a previously unnoticed cluster in the background.