Spectroscopic Characterization of redMaPPer Galaxy Clusters with DESI

TL;DR

This study uses DESI spectroscopy to quantify projection effects in redMaPPer galaxy clusters, revealing their dependence on richness, redshift, and luminosity, and establishing a link between spectroscopic richness and halo mass.

Contribution

It provides the first spectroscopic evidence of how projection effects vary with redshift and luminosity, and relates spectroscopic richness to halo mass.

Findings

Projection effects are more than twice as large at low richness.

Projection effects increase by up to 25% from z~0.1 to z~0.2.

Fainter galaxies are more often misassociated behind clusters.

Abstract

Optical galaxy cluster identification algorithms such as redMaPPer promise to enable an array of astrophysical and cosmological studies, but suffer from biases whereby galaxies in front of and behind a galaxy cluster are mistakenly associated with the primary cluster halo. These projection effects caused by irreducible photometric redshift uncertainty must be quantified to facilitate the use of optical cluster catalogues. We present measurements of galaxy cluster projection effects and velocity dispersion using spectroscopy from the Dark Energy Spectroscopic Instrument (DESI). Our findings are as follows: we confirm that the fraction of redMaPPer putative member galaxies mistakenly associated with cluster haloes is richness dependent, being more than twice as large at low richness than high richness; we present the first spectroscopic evidence of an increase in projection effects with increasing redshift, by as much as 25 per cent from $z\sim0.1$ to $z\sim0.2$; moreover, we find qualitative evidence for luminosity dependence in projection effects, with fainter galaxies being more commonly far behind clusters than their bright counterparts; finally we fit the scaling relation between measured mean spectroscopic richness and velocity dispersion, finding an implied linear scaling between spectroscopic richness and halo mass. We discuss further directions for the application of spectroscopic datasets to improve use of optically selected clusters to test cosmological models.