Features of the Spatial Distribution of Galaxy Clusters

TL;DR

This study identifies anisotropic, quasi-periodic features in the spatial distribution of galaxy clusters across both hemispheres, using spectroscopic and photometric redshift data, revealing consistent preferred directions and significant spectral features.

Contribution

It demonstrates the detection of anisotropic, quasi-periodic spatial features in galaxy cluster distributions using photometric redshifts, extending previous findings to the southern hemisphere.

Findings

Detection of a preferred direction in the northern hemisphere with high significance.

Identification of a corresponding preferred direction in the southern hemisphere.

Presence of significant spectral features in the power spectra at specific wave numbers.

Abstract

A statistical analysis of anisotropic quasiperiodic features of the spatial distribution of galaxy clusters obtained on the basis of spectroscopic and photometric redshifts in the interval $0.1 \leq z \leq 0.47$ has been carried out. Based on data from the SDSS~III catalog, we show that the preferential direction previously detected in the northern hemisphere (a narrow cone of directions: $\alpha_0=170^\circ \pm 5^\circ, \ \delta_0= 29^\circ \pm 5^\circ$), along which the one-dimensional distribution of projections of the Cartesian coordinates of clusters contains a significant ($\gtrsim (4 - 5) \sigma$) quasi-periodic component, can also be found using photometric redshifts, achieving a certain accuracy ($\Delta z \lesssim 0.013$). Based on data from the photometric DES$\times$unWISE catalog, we have analyzed the spatial distribution of clusters in the southern hemisphere, where a cone of close directions was also detected ($\alpha_0=346^\circ \pm 5^\circ,\ \delta_0= - 29^\circ \pm 5^\circ $), which are approximately an extention of the directions revealed in the northern hemisphere. The power spectra of one-dimensional distributions along these directions contain significant ($\gtrsim (4 - 5) \sigma$) features in the same interval of wave numbers $0.04 \lesssim k \lesssim 0.06~h$~Mpc$^{-1}$.