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Table · dataset · 2023

Stellar mass as a galaxy cluster mass proxy

Listed in IVOA Registry (Virtual Observatory)

We introduce a galaxy cluster mass observable, {mu}_*_, based on the stellar masses of cluster members, and we present results for the Dark Energy Survey (DES) Year 1 (Y1) observations.

Description

Stellar masses are computed using a Bayesian model averaging method, and are validated for DES data using simulations and COSMOS data. We show that {mu}_*_ works as a promising mass proxy by comparing our predictions to X-ray measurements.

We measure the X-ray temperature-{mu}_*_ relation for a total of 129 clusters matched between the wide-field DES Y1 redMaPPer catalogue and Chandra and XMM archival observations, spanning the redshift range 0.1<z<0.7. For a scaling relation that is linear in logarithmic space, we find a slope of {alpha}=0.488+/-0.043 and a scatter in the X-ray temperature at fixed {mu}_*_ of {sigma}_lnTX|{mu}*_= 0.266^+0.019^_-0.020_ for the joint sample.

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By using the halo mass scaling relations of the X-ray temperature from the Weighing the Giants program, we further derive the {mu}_*_-conditioned scatter in mass, finding {sigma}_lnM|{mu}*_=0.26^+0.15^_-0.10_. These results are competitive with well-established cluster mass proxies used for cosmological analyses, showing that {mu}_*_ can be used as a reliable and physically motivated mass proxy to derive cosmological constraints.

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