Method of analysis of the spatial galaxy distribution at gigaparsec scales. I. Initial principles

TL;DR

This paper proposes a new method for analyzing the large-scale spatial distribution of luminous matter in the universe using photometric redshift data from deep multiband surveys, aiming to identify super large structures at gigaparsec scales.

Contribution

It introduces an analysis framework based on deep field surveys and photometric redshift distributions to study super large structures at gigaparsec scales, including considerations of systematic errors.

Findings

Method based on N(z) distribution in large sky regions.

Use of deep multiband surveys with 10°x10° coverage.

Analysis of distortion effects in photo-z determination.

Abstract

Initial principles of a method of analysis of the luminous matter spatial distribution with sizes about thousands Mpc are presented. The method is based on an analysis of the photometric redshift distribution N(z) in the deep fields with large redshift bins \Deltaz=0.1{\div}0.3. Number density fluctuations in the bins are conditioned by the Poisson's noise, the correlated structures and the systematic errors of the photo-z determination. The method includes covering of a sufficiently large region on the sky by a net of the deep multiband surveys with the sell size about 10^{\circ}x10^{\circ} where individual deep fields have angular size about 10'x10' and may be observed at telescopes having diameters 3-10 meters. The distributions of photo-z within each deep field will give information about the radial extension of the super large structures while a comparison of the individual radial distributions of the net of the deep fields will give information on the tangential extension of the super large structures. A necessary element of the method is an analysis of possible distortion effects related to the methodic of the photo-z determination.