Dark Energy Survey Year 3 results: redshift calibration of the weak lensing source galaxies

Dark Energy Survey Year 3 results: redshift calibration of the weak lensing source galaxies
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DOI：
10.1093/mnras/stab1515
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发表时间：
2020-12
期刊：
Monthly Notices of the Royal Astronomical Society
影响因子：
4.8
通讯作者：
J. Myles;A. Alarcon;A. Amon;C. S'anchez;S. Everett;J. DeRose;J. McCullough;D. Gruen;G. Bernstein;M. Troxel;S. Dodelson;A. Campos;N. MacCrann;Biao Yin;M. Raveri;A. Amara;M. Becker;A. Choi;J. Cordero;K. Eckert;M. Gatti;G. Giannini;J. Gschwend;R. Gruendl;I. Harrison;W. Hartley;E. Huff;N. Kuropatkin;H. Lin;D. Masters;R. Miquel;J. Prat;A. Roodman;E. Rykoff;I. Sevilla-Noarbe;E. Sheldon;Risa Wechsler;B. Yanny;T. Abbott;M. Aguena;S. Allam;J. Annis;D. Bacon;E. Bertin;S. Bhargava;S. Bridle;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;F. Castander;C. Conselice;M. Costanzi;M. Crocce;L. Costa;M. Pereira;S. Desai;H. Diehl;T. Eifler;J. Elvin-Poole;A. Evrard;I. Ferrero;A. Fert'e;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;T. Giannantonio;S. Hinton;D. Hollowood;K. Honscheid;B. Hoyle;D. Huterer;D. James;E. Krause;K. Kuehn;O. Lahav;M. Lima;M. Maia;J. Marshall;P. Martini;Peter Melchior;F. Menanteau;J. Mohr;R. Morgan;J. Muir;R. Ogando;A. Palmese;F. Paz-Chinch'on;A. Plazas;M. Rodríguez-Monroy;S. Samuroff;E. Sánchez;V. Scarpine;L. Secco;S. Serrano;M. Smith;M. Soares-Santos;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;C. To;T. Varga;J. Weller;W. Wester
J. Myles;A. Alarcon;A. Amon;C. S'anchez;S. Everett;J. DeRose;J. McCullough;D. Gruen;G. Bernstein;M. Troxel;S. Dodelson;A. Campos;N. MacCrann;Biao Yin;M. Raveri;A. Amara;M. Becker;A. Choi;J. Cordero;K. Eckert;M. Gatti;G. Giannini;J. Gschwend;R. Gruendl;I. Harrison;W. Hartley;E. Huff;N. Kuropatkin;H. Lin;D. Masters;R. Miquel;J. Prat;A. Roodman;E. Rykoff;I. Sevilla-Noarbe;E. Sheldon;Risa Wechsler;B. Yanny;T. Abbott;M. Aguena;S. Allam;J. Annis;D. Bacon;E. Bertin;S. Bhargava;S. Bridle;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;F. Castander;C. Conselice;M. Costanzi;M. Crocce;L. Costa;M. Pereira;S. Desai;H. Diehl;T. Eifler;J. Elvin-Poole;A. Evrard;I. Ferrero;A. Fert'e;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;T. Giannantonio;S. Hinton;D. Hollowood;K. Honscheid;B. Hoyle;D. Huterer;D. James;E. Krause;K. Kuehn;O. Lahav;M. Lima;M. Maia;J. Marshall;P. Martini;Peter Melchior;F. Menanteau;J. Mohr;R. Morgan;J. Muir;R. Ogando;A. Palmese;F. Paz-Chinch'on;A. Plazas;M. Rodríguez-Monroy;S. Samuroff;E. Sánchez;V. Scarpine;L. Secco;S. Serrano;M. Smith;M. Soares-Santos;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;C. To;T. Varga;J. Weller;W. Wester
中科院分区：
物理与天体物理2区
文献类型：
--
作者：
J. Myles;A. Alarcon;A. Amon;C. S'anchez;S. Everett;J. DeRose;J. McCullough;D. Gruen;G. Bernstein;M. Troxel;S. Dodelson;A. Campos;N. MacCrann;Biao Yin;M. Raveri;A. Amara;M. Becker;A. Choi;J. Cordero;K. Eckert;M. Gatti;G. Giannini;J. Gschwend;R. Gruendl;I. Harrison;W. Hartley;E. Huff;N. Kuropatkin;H. Lin;D. Masters;R. Miquel;J. Prat;A. Roodman;E. Rykoff;I. Sevilla-Noarbe;E. Sheldon;Risa Wechsler;B. Yanny;T. Abbott;M. Aguena;S. Allam;J. Annis;D. Bacon;E. Bertin;S. Bhargava;S. Bridle;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;F. Castander;C. Conselice;M. Costanzi;M. Crocce;L. Costa;M. Pereira;S. Desai;H. Diehl;T. Eifler;J. Elvin-Poole;A. Evrard;I. Ferrero;A. Fert'e;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;T. Giannantonio;S. Hinton;D. Hollowood;K. Honscheid;B. Hoyle;D. Huterer;D. James;E. Krause;K. Kuehn;O. Lahav;M. Lima;M. Maia;J. Marshall;P. Martini;Peter Melchior;F. Menanteau;J. Mohr;R. Morgan;J. Muir;R. Ogando;A. Palmese;F. Paz-Chinch'on;A. Plazas;M. Rodríguez-Monroy;S. Samuroff;E. Sánchez;V. Scarpine;L. Secco;S. Serrano;M. Smith;M. Soares-Santos;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;C. To;T. Varga;J. Weller;W. Wester

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通过像暗能量巡天（DES）这样的宽视场测光实验来确定星系的红移分布是用引力透镜映射物质密度场的重要组成部分。在这项工作中，我们描述的方法来分配个人弱透镜源星系从DES第3年弱透镜源目录到四个层析箱，并估计在这些箱子的红移分布。作为第一次应用这些方法的数据，我们验证了假设适用于DES Y3弱透镜源星系，并制定了全面的治疗系统的不确定性。我们的方法包括从三个独立的似然函数相结合的信息：自组织映射p（z）（sompz），一种方法，用于约束红移星系测光;集群红移（WZ），约束红移星系密度函数的互相关;和剪切比（SR），它提供了约束红移的星系剪切相关函数的比例在小尺度上。最后，我们描述了如何将这些独立的探测器相结合，以产生一个合奏的红移分布封装我们的全部不确定性。我们在每个层析箱中的平均红移上用组合的有效不确定度σ 0.01校准红移。
Determining the distribution of redshifts of galaxies observed by wide-field photometric experiments like the Dark Energy Survey (DES) is an essential component to mapping the matter density field with gravitational lensing. In this work we describe the methods used to assign individual weak lensing source galaxies from the DES Year 3 Weak Lensing Source Catalogue to four tomographic bins and to estimate the redshift distributions in these bins. As the first application of these methods to data, we validate that the assumptions made apply to the DES Y3 weak lensing source galaxies and develop a full treatment of systematic uncertainties. Our method consists of combining information from three independent likelihood functions: self-organizing map p(z) (sompz), a method for constraining redshifts from galaxy photometry; clustering redshifts (WZ), constraints on redshifts from cross-correlations of galaxy density functions; and shear ratios (SRs), which provide constraints on redshifts from the ratios of the galaxy-shear correlation functions at small scales. Finally, we describe how these independent probes are combined to yield an ensemble of redshift distributions encapsulating our full uncertainty. We calibrate redshifts with combined effective uncertainties of σ〈z〉 ∼ 0.01 on the mean redshift in each tomographic bin.