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

Palmese, A. and Annis, J. and Burgad, J. and Farahi, A. and Soares-Santos, M. and Welch, B. and Pereira, M. da Silva and Lin, H. and Bhargava, S. and Hollowood, D. L. and Wilkinson, R. and Giles, P. and Jeltema, T. and Romer, A. K. and Evrard, A. E. and Hilton, M. and Cervantes, C. Vergara and Bermeo, A. and Mayers, J. and DeRose, J. and Gruen, D. and Hartley, W. G. and Lahav, O. and Leistedt, B. and McClintock, T. and Rozo, E. and Rykoff, E. S. and Varga, T. N. and Wechsler, R. H. and Zhang, Y. and Avila, S. and Brooks, D. and Buckley-Geer, E. and Burke, D. L. and Rosell, A. Carnero and Kind, M. Carrasco and Carretero, J. and Castander, F. J. and Collins, C. and da Costa, L. N. and Desai, S. and De Vicente, J. and Diehl, H. T. and Dietrich, J. P. and Doel, P. and Flaugher, B. and Fosalba, P. and Frieman, J. and Garcia-Bellido, J. and Stott, J. (2020) Stellar mass as a galaxy cluster mass proxy:application to the Dark Energy Survey redMaPPer clusters. Monthly Notices of the Royal Astronomical Society, 493 (4). pp. 4591-4606. ISSN 0035-8711

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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. 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)vertical bar mu(*) = 0.266(-0.020)(+0.019) for the joint sample. By using the halo mass scaling relations of the X-ray temperature from the Weighing the Giants program, we further derive the mu(star)- conditioned scatter inmass, finding sigma(lnM)vertical bar mu(*) = 0.26(-0.10)(+0.15). 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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Journal Article
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Monthly Notices of the Royal Astronomical Society
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24 Aug 2020 10:25
Last Modified:
19 Sep 2020 06:27