On the Level of Cluster Assembly Bias in SDSS

TL;DR

This study investigates the apparent discrepancy in clustering biases of SDSS galaxy clusters, revealing that projection effects significantly influence measurements and that the true halo assembly bias aligns with LCDM predictions.

Contribution

The paper introduces a new robust estimator for cluster membership distance, reducing projection bias and reconciling observed clustering biases with theoretical LCDM expectations.

Findings

Projection effects account for most of the observed bias discrepancy.

The revised bias ratio aligns with LCDM predictions within uncertainties.

Future surveys will improve detection of halo assembly bias.

Abstract

Recently, several studies have discovered a strong discrepancy between the large-scale clustering biases of two subsamples of galaxy clusters at the same halo mass, split by their average projected membership distances $R_{\mathrm{mem}}$. The level of this discrepancy significantly exceeds the maximum halo assembly bias signal predicted by LCDM. In this study, we explore whether some of the clustering bias differences could be caused by biases in $R_{\mathrm{mem}}$ due to projection effects from other systems along the line-of-sight. We thoroughly investigate the halo assembly bias of the photometrically-detected redMaPPer clusters in SDSS, by defining a new variant of the average membership distance estimator $\tilde{R}_{\mathrm{mem}}$ that is more robust against projection effects in the cluster membership identification. Using the angular mark correlation functions of clusters, we show that the large-scale bias differences when splitting by $R_{\mathrm{mem}}$ can be largely attributed to such projection effects. After splitting by $\tilde{R}_{\mathrm{mem}}$, the anomalously large signal is reduced, giving a ratio of $1.02\pm0.14$ between the two clustering biases as measured from weak lensing. Using a realistic mock cluster catalog, we predict that the bias ratio between two $\tilde{R}_{\mathrm{mem}}$-split subsamples should be $<1.10$, which is at least 60% weaker than the maximum halo assembly bias signal (1.24) when split by halo concentration. Therefore, our results demonstrate that the level of halo assembly bias exhibited by redMaPPer clusters in SDSS is consistent with the LCDM prediction. With a ten-fold increase in cluster numbers, deeper ongoing surveys will enable a more robust detection of halo assembly bias. Our findings also have important implications for how projection effects and their impact on cluster cosmology can be quantified in photometric cluster catalogs.