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We introduce a galaxy cluster mass observable, $\mu_\star$, based on thestellar masses of cluster members, and we present results for the Dark EnergySurvey (DES) Year 1 observations. Stellar masses are computed using a BayesianModel Averaging method, and are validated for DES data using simulations andCOSMOS data. We show that $\mu_\star$ works as a promising mass proxy bycomparing our predictions to X-ray measurements. We measure the X-raytemperature-$\mu_\star$ relation for a total of 150 clusters matched betweenthe wide-field DES Year 1 redMaPPer catalogue, and Chandra and XMM archivalobservations, spanning the redshift range $0.1<z<0.7$. For a scaling relationwhich is linear in logarithmic space, we find a slope of $\alpha =0.488\pm0.043$ and a scatter in the X-ray temperature at fixed $\mu_\star$ of$\sigma_{{\rm ln} T_X|\mu_\star}=0.266^{+0.019}_{-0.020}$ for the joint sample.By using the halo mass scaling relations of the X-ray temperature from theWeighing the Giants program, we further derive the $\mu_\star$-conditionedscatter in mass, finding $\sigma_{{\rm ln} M|\mu_\star}=0.26^{+ 0.15}_{-0.10}$. These results are competitive with well-established cluster massproxies used for cosmological analyses, showing that $\mu_\star$ can be used asa reliable and physically motivated mass proxy to derive cosmologicalconstraints.

Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters