Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies
Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies
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DOI：
10.1093/mnras/sty957
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发表时间：
2017-08
影响因子：
4.8
通讯作者：
B. Hoyle;D. Gruen;G. Bernstein;M. Rau;J. Vicente;W. Hartley;E. Gaztañaga;J. DeRose;M. Troxel;C. Davis;A. Alarcon;N. MacCrann;J. Prat;C. S'anchez;E. Sheldon;Risa Wechsler;J. Asorey;M. Becker;C. Bonnett;A. Rosell;D. Carollo;M. Kind;F. Castander;R. Cawthon;C. Chang;M. Childress;T. Davis;A. Drlica-Wagner;M. Gatti;K. Glazebrook;J. Gschwend;S. Hinton;J. Hoormann;A. Kim;A. King;K. Kuehn;G. Lewis;C. Lidman;H. Lin;E. MacAulay;M. Maia;P. Martini;D. Mudd;A. Moller;R. Nichol;R. Ogando;R. Rollins;A. Roodman;A. Ross;E. Rozo;E. Rykoff;S. Samuroff;I. Sevilla-Noarbe;R. Sharp;N. E. Sommer;B. Tucker;S. Uddin;T. Varga;P. Vielzeuf;F. Yuan;B. Zhang;T. Abbott;F. Abdalla;S. Allam;J. Annis;K. Bechtol;A. Benoit-Lévy;E. Bertin;D. Brooks;E. Buckley-Geer;D. Burke;M. Busha;D. Capozzi;J. Carretero;M. Crocce;C. D'Andrea;L. Costa;D. Depoy;S. Desai;H. Diehl;P. Doel;T. Eifler;J. Estrada;A. Evrard;E. Fernandez;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;D. Gerdes;T. Giannantonio;D. Goldstein;R. Gruendl;G. Gutiérrez;K. Honscheid;D. James;M. Jarvis;T. Jeltema;M. Johnson;M. Johnson;D. Kirk;E. Krause;S. Kuhlmann;N. Kuropatkin;O. Lahav;T. Li;M. Lima;M. March;J. Marshall;Peter Melchior;F. Menanteau;R. Miquel;B. Nord;C. O’Neill;A. Plazas;A. Romer;M. Sako;E. Sánchez;B. Santiago;V. Scarpine;R. Schindler;M. Schubnell;M. Smith;R. C. Smith;M. Soares-Santos;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;D. Tucker;V. Vikram;A. Walker;J. Weller;W. Wester;R. Wolf;B. Yanny;J. Zuntz
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文献类型：
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作者：
B. Hoyle;D. Gruen;G. Bernstein;M. Rau;J. Vicente;W. Hartley;E. Gaztañaga;J. DeRose;M. Troxel;C. Davis;A. Alarcon;N. MacCrann;J. Prat;C. S'anchez;E. Sheldon;Risa Wechsler;J. Asorey;M. Becker;C. Bonnett;A. Rosell;D. Carollo;M. Kind;F. Castander;R. Cawthon;C. Chang;M. Childress;T. Davis;A. Drlica-Wagner;M. Gatti;K. Glazebrook;J. Gschwend;S. Hinton;J. Hoormann;A. Kim;A. King;K. Kuehn;G. Lewis;C. Lidman;H. Lin;E. MacAulay;M. Maia;P. Martini;D. Mudd;A. Moller;R. Nichol;R. Ogando;R. Rollins;A. Roodman;A. Ross;E. Rozo;E. Rykoff;S. Samuroff;I. Sevilla-Noarbe;R. Sharp;N. E. Sommer;B. Tucker;S. Uddin;T. Varga;P. Vielzeuf;F. Yuan;B. Zhang;T. Abbott;F. Abdalla;S. Allam;J. Annis;K. Bechtol;A. Benoit-Lévy;E. Bertin;D. Brooks;E. Buckley-Geer;D. Burke;M. Busha;D. Capozzi;J. Carretero;M. Crocce;C. D'Andrea;L. Costa;D. Depoy;S. Desai;H. Diehl;P. Doel;T. Eifler;J. Estrada;A. Evrard;E. Fernandez;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;D. Gerdes;T. Giannantonio;D. Goldstein;R. Gruendl;G. Gutiérrez;K. Honscheid;D. James;M. Jarvis;T. Jeltema;M. Johnson;M. Johnson;D. Kirk;E. Krause;S. Kuhlmann;N. Kuropatkin;O. Lahav;T. Li;M. Lima;M. March;J. Marshall;Peter Melchior;F. Menanteau;R. Miquel;B. Nord;C. O’Neill;A. Plazas;A. Romer;M. Sako;E. Sánchez;B. Santiago;V. Scarpine;R. Schindler;M. Schubnell;M. Smith;R. C. Smith;M. Soares-Santos;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;D. Tucker;V. Vikram;A. Walker;J. Weller;W. Wester;R. Wolf;B. Yanny;J. Zuntz
我们描述的推导和验证的红移分布估计和它们的不确定性的人口的星系作为弱透镜源的暗能量调查（DES）的第1年宇宙学分析。贝叶斯测光红移（Bayesian Photometric Redshift，BPZ）代码用于将星系分配到z = 0.2到z = 1.3之间的四个红移仓，并为仓i的成员产生透镜加权红移分布ni PZ（z）dni/dz的初始估计。宇宙学参数的精确测定关键取决于对ni的了解，但对单个星系的bin分配或红移误差不敏感。宇宙学分析允许位移ni（z）= niPZ（z-zi）来校正ni（z）的平均红移。在宇宙演化巡天（COSMOS）领域的BPZ估计从DES griz通量的独立估计的星系的30波段光度红移的比较约束的zi，为样本匹配的通量，预见的大小，和透镜重量DES弱透镜源。在相关论文中，三个最低红移区间的zi进一步受到红色星系周围源星系的角聚集的限制，其光度红移为0.15 < z < 0.9。本文详细介绍了BPZ和COSMOS程序，并证明了宇宙学推断是不敏感的细节的ni（z）以外的选择zi。聚类和COSMOS验证方法在两种方法都可以应用的情况下，在四个箱中产生一致的zi估计值，四个箱中的组合不确定度分别为σzi = 0.015、0.013、0.011和0.022。重复photo-z程序，而不是使用方向邻域拟合算法，或使用从COSMOS中匹配样本估计的ni（z），在宇宙学推论中没有明显的差异。
We describe the derivation and validation of redshift distribution estimates and their uncertainties for the populations of galaxies used as weak-lensing sources in the Dark Energy Survey (DES) Year 1 cosmological analyses. The Bayesian Photometric Redshift (BPZ) code is used to assign galaxies to four redshift bins between z ≈ 0.2 and ≈1.3, and to produce initial estimates of the lensing-weighted redshift distributions ni PZ(z) ∝ dni/dz for members of bin i. Accurate determination of cosmological parameters depends critically on knowledge of ni , but is insensitive to bin assignments or redshift errors for individual galaxies. The cosmological analyses allow for shifts ni(z) = niPZ(z − zi) to correct the mean redshift of ni(z) for biases in niPZ. The zi are constrained by comparison of independently estimated 30-band photometric redshifts of galaxies in the Cosmic Evolution Survey (COSMOS) field to BPZ estimates made from the DES griz fluxes, for a sample matched in fluxes, pre-seeing size, and lensing weight to the DES weak-lensing sources. In companion papers, the zi of the three lowest redshift bins are further constrained by the angular clustering of the source galaxies around red galaxies with secure photometric redshifts at 0.15 < z < 0.9. This paper details the BPZ and COSMOS procedures, and demonstrates that the cosmological inference is insensitive to details of the ni(z) beyond the choice of zi . The clustering and COSMOS validation methods produce consistent estimates of zi in the bins where both can be applied, with combined uncertainties of σzi = 0.015, 0.013, 0.011, and 0.022 in the four bins. Repeating the photo-z procedure instead using the Directional Neighbourhood Fitting algorithm, or using the ni(z) estimated from the matched sample in COSMOS, yields no discernible difference in cosmological inferences.