Dark Energy Survey Year 1 results: weak lensing mass calibration of redMaPPer galaxy clusters
Dark Energy Survey Year 1 results: weak lensing mass calibration of redMaPPer galaxy clusters
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DOI：
10.1093/mnras/sty2711
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发表时间：
2018-04
影响因子：
4.8
通讯作者：
T. McClintock;T. Varga;D. Gruen;E. Rozo;E. Rykoff;T. Shin;Peter Melchior;J. DeRose;S. Seitz;J. Dietrich;E. Sheldon;Y. Zhang;A. V. D. Linden;T. Jeltema;A. Mantz;A. Romer;S. Allen;M. Becker;A. Bermeo;S. Bhargava;M. Costanzi;S. Everett;A. Farahi;N. Hamaus;W. Hartley;D. Hollowood;B. Hoyle;H. Israel;P. Li;N. MacCrann;G. Morris;A. Palmese;A. Plazas;G. Pollina;M. Rau;M. Simet;M. Soares-Santos;M. Troxel;C. Cervantes;Risa Wechsler;J. Zuntz;T. Abbott;F. Abdalla;S. Allam;J. Annis;S. Ávila;S. Bridle;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;F. Castander;M. Crocce;C. Cunha;C. D'Andrea;L. Costa;C. Davis;J. Vicente;H. Diehl;P. Doel;A. Drlica-Wagner;A. Evrard;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;D. Gerdes;T. Giannantonio;R. Gruendl;G. Gutiérrez;K. Honscheid;D. James;D. Kirk;E. Krause;K. Kuehn;O. Lahav;T. Li;M. Lima;M. March;J. Marshall;F. Menanteau;R. Miquel;J. Mohr;B. Nord;R. Ogando;A. Roodman;E. Sánchez;V. Scarpine;R. Schindler;I. Sevilla-Noarbe;M. Smith;R. C. Smith;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;D. Tucker;V. Vikram;A. Walker;J. Weller
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文献类型：
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作者：
T. McClintock;T. Varga;D. Gruen;E. Rozo;E. Rykoff;T. Shin;Peter Melchior;J. DeRose;S. Seitz;J. Dietrich;E. Sheldon;Y. Zhang;A. V. D. Linden;T. Jeltema;A. Mantz;A. Romer;S. Allen;M. Becker;A. Bermeo;S. Bhargava;M. Costanzi;S. Everett;A. Farahi;N. Hamaus;W. Hartley;D. Hollowood;B. Hoyle;H. Israel;P. Li;N. MacCrann;G. Morris;A. Palmese;A. Plazas;G. Pollina;M. Rau;M. Simet;M. Soares-Santos;M. Troxel;C. Cervantes;Risa Wechsler;J. Zuntz;T. Abbott;F. Abdalla;S. Allam;J. Annis;S. Ávila;S. Bridle;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;F. Castander;M. Crocce;C. Cunha;C. D'Andrea;L. Costa;C. Davis;J. Vicente;H. Diehl;P. Doel;A. Drlica-Wagner;A. Evrard;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;D. Gerdes;T. Giannantonio;R. Gruendl;G. Gutiérrez;K. Honscheid;D. James;D. Kirk;E. Krause;K. Kuehn;O. Lahav;T. Li;M. Lima;M. March;J. Marshall;F. Menanteau;R. Miquel;J. Mohr;B. Nord;R. Ogando;A. Roodman;E. Sánchez;V. Scarpine;R. Schindler;I. Sevilla-Noarbe;M. Smith;R. C. Smith;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;D. Tucker;V. Vikram;A. Walker;J. Weller
我们使用弱引力透镜约束了暗能量调查第一年数据中确定的redMaPPer星系团的质量-丰度标度关系。我们将星团分成4×3个富集度λ和红移z的λ≥20和0.2≤z≤0.65，并利用它们堆叠的弱透镜信号测量这些丰富度和红移z的平均质量。通过将标度关系建模为⟨M 200M|λ，z⟩=M0(λ/40)F((1+z)/1.35)G，我们将标度关系的归一化限制在5.0%的水平，M0=[3.081±0.075(STAT)±0.133(Sys)]⋅10 14 M⊙在λ=40和z=0.35时。丰富度标度指数F=1.356±0.051(STAT)±0.008(Sys)，红移标度指数G=−0.30±0.30(STAT)±0.008(Sys)。这是迄今为止对归一化和丰富度指数进行的最严格的测量。我们使用半解析协方差矩阵来表征恢复的弱透镜轮廓中的统计误差。我们的分析解释了以下系统误差的来源：剪切和光度红移误差、星团偏心、源样品的星团成员稀释、晕质量关联函数建模中的系统不确定性、晕三轴性和投影效应。我们讨论了减少这种系统误差预算的前景，它支配着M0上的不确定性。我们的结果与文献中以前的测量结果非常一致，但不确定度明显小于文献中的测量结果，并且预示着DES星系团调查作为精密宇宙学和即将到来的星系调查(如LSST、Euclid和WFIRST)的工具的能力是好的。
We constrain the mass--richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing. We split clusters into 4×3 bins of richness λ and redshift z for λ≥20 and 0.2≤z≤0.65 and measure the mean masses of these bins using their stacked weak lensing signal. By modeling the scaling relation as ⟨M 200m |λ,z⟩=M 0 (λ/40) F ((1+z)/1.35) G , we constrain the normalization of the scaling relation at the 5.0 per cent level as M 0 =[3.081±0.075(stat)±0.133(sys)]⋅10 14 M ⊙ at λ=40 and z=0.35 . The richness scaling index is constrained to be F=1.356±0.051 (stat)±0.008 (sys) and the redshift scaling index G=−0.30±0.30 (stat)±0.06 (sys) . These are the tightest measurements of the normalization and richness scaling index made to date. We use a semi-analytic covariance matrix to characterize the statistical errors in the recovered weak lensing profiles. Our analysis accounts for the following sources of systematic error: shear and photometric redshift errors, cluster miscentering, cluster member dilution of the source sample, systematic uncertainties in the modeling of the halo--mass correlation function, halo triaxiality, and projection effects. We discuss prospects for reducing this systematic error budget, which dominates the uncertainty on M 0. Our result is in excellent agreement with, but has significantly smaller uncertainties than, previous measurements in the literature, and augurs well for the power of the DES cluster survey as a tool for precision cosmology and upcoming galaxy surveys such as LSST, Euclid and WFIRST.