Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters-猫眼课题宝

DOI：

10.1093/mnras/staa526

发表时间：

2019-03

期刊：

Monthly Notices of the Royal Astronomical Society

影响因子：

4.8

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

A. Palmese;A. Palmese;J. Annis;J. Burgad;A. Farahi;M. Soares-Santos;B. Welch;M. Pereira;Huan Lin;S. Bhargava;D. Hollowood;R. Wilkinson;P. Giles;T. Jeltema;A. Romer;A. Evrard;M. Hilton;C. Cervantes;A. Bermeo;J. Mayers;J. DeRose;D. Gruen;D. Gruen;W. Hartley;W. Hartley;O. Lahav;B. Leistedt;T. McClintock;E. Rozo;E. Rykoff;E. Rykoff;T. Varga;T. Varga;Risa Wechsler;Risa Wechsler;Yuanyuan Zhang;S. Ávila;D. Brooks;E. Buckley-Geer;D. Burke;D. Burke;A. Rosell;M. Kind;M. Kind;J. Carretero;F. Castander;C. Collins;L. Costa;S. Desai;J. Vicente;H. Diehl;J. Dietrich;P. Doel;B. Flaugher;P. Fosalba;J. Frieman;J. Frieman;J. García-Bellido;D. Gerdes;R. Gruendl;R. Gruendl;J. Gschwend;G. Gutiérrez;K. Honscheid;D. James;E. Krause;K. Kuehn;N. Kuropatkin;A. Liddle;M. Lima;M. Maia;R. Mann;J. Marshall;F. Menanteau;F. Menanteau;R. Miquel;R. Ogando;A. Plazas;A. Roodman;A. Roodman;P. Rooney;M. Sahlén;E. Sánchez;Scarpine;M. Schubnell;S. Serrano;I. Sevilla-Noarbe;F. Sobreira;J. Stott;J. Stott;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;D. Tucker;P. T. P. Viana-P.-T.-P.-Viana-2178222408;Vikram;A. Walker

我们引入了一个星系团质量可观测的星系团，μ⋆，基于星系团成员的恒星质量，并给出了暗能量调查(DES)1年(Y1)观测的结果。恒星质量使用贝叶斯模型平均方法计算，并使用模拟和COSMOS数据对DES数据进行了验证。我们通过将我们的预测与X射线测量进行比较，表明μ⋆是一个很有前途的质量替代物。我们测量了宽视场DES Y1redMaPPer星表与Chandra和XMM档案观测之间匹配的总共129个星系团的X射线温度-μ⋆关系，横跨红移范围0.1&lt；$z$&lt；0.7。对于对数空间中线性的标度关系，我们发现联合样品的斜率α=0.488±0.043，在固定的μ⋆为$sigma_{{rm ln}T_\mathm{X}|\MU_\STAR}=0.266^{+0.019}_(-0.020)}$时的X射线温度散射值。利用加权巨星程序得到的X-射线温度的晕质量标度关系，进一步推导出μ⋆条件下的质量散射量，得到M=0.26^+0.15}-0.10}。这些结果与用于宇宙学分析的成熟的星系团质量代理具有竞争性，表明μ⋆可以作为一个可靠的和物理激励的质量代理来推导宇宙约束。

We introduce a galaxy cluster mass observable, μ⋆, 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 μ⋆ works as a promising mass proxy by comparing our predictions to X-ray measurements. We measure the X-ray temperature–μ⋆ 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 α = 0.488 ± 0.043 and a scatter in the X-ray temperature at fixed μ⋆ of $\sigma _{{\rm ln} T_\mathrm{ X}|\mu _\star }= 0.266^{+0.019}_{-0.020}$ for the joint sample. By using the halo mass scaling relations of the X-ray temperature from the Weighing the Giants program, we further derive the μ⋆-conditioned scatter in mass, finding $\sigma _{{\rm ln} M|\mu _\star }= 0.26^{+ 0.15}_{- 0.10}$. These results are competitive with well-established cluster mass proxies used for cosmological analyses, showing that μ⋆ can be used as a reliable and physically motivated mass proxy to derive cosmological constraints.

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

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