The Dark Energy Survey Year 3 high redshift sample: Selection, characterization and analysis of galaxy clustering

TL;DR

This paper presents the selection, characterization, and analysis of high-redshift galaxy samples from DES Year 3 data, extending the redshift range and providing robust cosmological constraints through galaxy clustering measurements.

Contribution

It introduces a novel high-redshift galaxy sample selection using Bayesian redshift estimation and machine learning corrections, significantly extending DES Year 3 analysis capabilities.

Findings

Galaxy clustering yields $ m \Omega_m h$ constraint of 0.195^{+0.023}_{-0.018}

Achieved 2-3% measurements of galaxy clustering amplitude

Sample contains about 9 million galaxies with over twice the density of previous analyses

Abstract

The fiducial cosmological analyses of imaging galaxy surveys like the Dark Energy Survey (DES) typically probe the Universe at redshifts $z < 1$. This is mainly because of the limited depth of these surveys, and also because such analyses rely heavily on galaxy lensing, which is more efficient at low redshifts. In this work we present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around $z \sim 0.9$, $1.2$ and $1.5$, which significantly extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions. The analysis of galaxy clustering measurements, with a total signal-to-noise $S/N \sim 70$ after scale cuts, yields robust cosmological constraints on a combination of the fraction of matter in the Universe $\Omega_m$ and the Hubble parameter $h$, $\Omega_m h = 0.195^{+0.023}_{-0.018}$, and 2-3% measurements of the amplitude of the galaxy clustering signals, probing galaxy bias and the amplitude of matter fluctuations, $b \sigma_8$. A companion paper $\textit{(in preparation)}$ will present the cross-correlations of these high-$z$ samples with CMB lensing from Planck and SPT, and the cosmological analysis of those measurements in combination with the galaxy clustering presented in this work.