Dark Energy Survey Year 3 results: Exploiting small-scale information with lensing shear ratios
Dark Energy Survey Year 3 results: Exploiting small-scale information with lensing shear ratios
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暗能量调查第三年结果：利用透镜剪切比的小规模信息
DOI：
10.1103/physrevd.105.083529
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发表时间：
2022
影响因子：
5
通讯作者：
Krause, E.
中科院分区：
文献类型：
--
作者：
Sánchez, C.;Prat, J.;Zacharegkas, G.;Pandey, S.;Baxter, E.;Bernstein, G. M.;Blazek, J.;Cawthon, R.;Chang, C.;Krause, E.
使用前三年的数据从暗能量调查（DES），我们使用的比率小规模的星系星系透镜测量周围相同的透镜样本，以约束源红移的不确定性，内在的对齐和其他系统或滋扰我们的模型参数。而不是使用一个简单的几何方法的比率已经在过去做的，我们使用完整的建模的星系-星系透镜测量，包括相应的集成功率谱和贡献的内在对齐和透镜放大。我们进行广泛的测试的小尺度剪切比（SR）建模研究不同的影响，如重子物理，非线性偏置，晕占据分布的描述和透镜放大率，除其他外，并使用真实的身体模拟的DES数据。我们使用两个独立的透镜样本具有不同的星系属性，并通过使用相应的大规模的比例，建模更简单的推导约束，我们的约束数据验证的鲁棒性。应用于DES Y3数据的结果表明，在我们的模型中，特别是在源红移校准和内在的对齐的几个讨厌的参数的约束功率的比率提供了显着的改善。对于源红移，SR提高了约束从以前的38%，在一些红移箱。这样的改进，特别是它提供的约束内在的路线，转化为更严格的宇宙学约束时，剪切比与宇宙剪切和其他2 pt功能相结合。特别是，对于DES Y3数据，SR将来自宇宙剪切的约束提高了31%，对于探测器的完全组合（）提高了10%。在这项工作中提出的剪切比被用来作为宇宙剪切的额外可能性，并fullin基准DES Y3宇宙学分析。
Using the first three years of data from the Dark Energy Survey (DES), we use ratios of small-scale galaxy-galaxy lensing measurements around the same lens sample to constrain source redshift uncertainties, intrinsic alignments and other systematics or nuisance parameters of our model. Instead of using a simple geometric approach for the ratios as has been done in the past, we use the full modeling of the galaxy-galaxy lensing measurements, including the corresponding integration over the power spectrum and the contributions from intrinsic alignments and lens magnification. We perform extensive testing of the small-scale shear-ratio (SR) modeling by studying the impact of different effects such as the inclusion of baryonic physics, nonlinear biasing, halo occupation distribution descriptions and lens magnification, among others, and using realistic-body simulations of the DES data. We validate the robustness of our constraints in the data by using two independent lens samples with different galaxy properties, and by deriving constraints using the corresponding large-scale ratios for which the modeling is simpler. The results applied to the DES Y3 data demonstrate how the ratios provide significant improvements in constraining power for several nuisance parameters in our model, especially on source redshift calibration and intrinsic alignments. For source redshifts, SR improves the constraints from the prior by up to 38% in some redshift bins. Such improvements, and especially the constraints it provides on intrinsic alignments, translate to tighter cosmological constraints when shear ratios are combined with cosmic shear and other 2pt functions. In particular, for the DES Y3 data, SR improvesconstraints from cosmic shear by up to 31%, and for the full combination of probes () by up to 10%. The shear ratios presented in this work are used as an additional likelihood for cosmic shear,and the fullin the fiducial DES Y3 cosmological analysis.
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影响因子：
4.8
作者：
P. Lemos;M. Raveri;A. Campos;Y. Park;C. Chang;N. Weaverdyck;D. Huterer;A. Liddle;J. Blazek;R. Cawthon;A. Choi;J. DeRose;S. Dodelson;C. Doux;M. Gatti;D. Gruen;I. Harrison;E. Krause;O. Lahav;N. MacCrann;J. Muir;J. Prat;M. Rau;R. Rollins;S. Samuroff;J. Zuntz;W. Hartley;B. Hoyle;I. Sevilla-Noarbe;M. Troxel;M. Aguena;S. Allam;J. Annis;S. Ávila;D. Bacon;G. Bernstein;E. Bertin;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;C. Conselice;M. Costanzi;M. Crocce;M. Pereira;J. Vicente;S. Desai;H. Diehl;P. Doel;K. Eckert;T. Eifler;J. Elvin-Poole;S. Everett;A. Evrard;I. Ferrero;A. Fert'e;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;D. Gerdes;T. Giannantonio;R. Gruendl;J. Gschwend;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;E. Huff;D. James;M. Jarvis;M. Lima;M. Maia;M. March;J. Marshall;P. Martini;Peter Melchior;F. Menanteau;R. Miquel;J. Mohr;R. Morgan;J. Myles;R. Ogando;A. Palmese;S. Pandey;F. Paz-Chinch'on;A. Plazas;M. Rodríguez-Monroy;A. Roodman;E. Sánchez;V. Scarpine;M. Schubnell;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
通讯作者：
P. Lemos;M. Raveri;A. Campos;Y. Park;C. Chang;N. Weaverdyck;D. Huterer;A. Liddle;J. Blazek;R. Cawthon;A. Choi;J. DeRose;S. Dodelson;C. Doux;M. Gatti;D. Gruen;I. Harrison;E. Krause;O. Lahav;N. MacCrann;J. Muir;J. Prat;M. Rau;R. Rollins;S. Samuroff;J. Zuntz;W. Hartley;B. Hoyle;I. Sevilla-Noarbe;M. Troxel;M. Aguena;S. Allam;J. Annis;S. Ávila;D. Bacon;G. Bernstein;E. Bertin;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;C. Conselice;M. Costanzi;M. Crocce;M. Pereira;J. Vicente;S. Desai;H. Diehl;P. Doel;K. Eckert;T. Eifler;J. Elvin-Poole;S. Everett;A. Evrard;I. Ferrero;A. Fert'e;B. Flaugher;P. Fosalba;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;D. Gerdes;T. Giannantonio;R. Gruendl;J. Gschwend;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;E. Huff;D. James;M. Jarvis;M. Lima;M. Maia;M. March;J. Marshall;P. Martini;Peter Melchior;F. Menanteau;R. Miquel;J. Mohr;R. Morgan;J. Myles;R. Ogando;A. Palmese;S. Pandey;F. Paz-Chinch'on;A. Plazas;M. Rodríguez-Monroy;A. Roodman;E. Sánchez;V. Scarpine;M. Schubnell;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
影响因子：
6.5
作者：
S. Unruh;P. Schneider;S. Hilbert
通讯作者：
S. Unruh;P. Schneider;S. Hilbert
影响因子：
4.8
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
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
暗能量调查第三年结果：弱透镜形状目录
影响因子：
4.8
作者：
M. Gatti;E. Sheldon;A. Amon;M. Becker;M. Troxel;A. Choi;C. Doux;N. MacCrann;A. Navarro;I. Harrison;D. Gruen;G. Bernstein;M. Jarvis;L. Secco;A. Ferté;T. Shin;J. McCullough;R. Rollins;R. Chen;C. Chang;S. Pandey;I. Tutusaus;J. Prat;J. Elvin;C. Sánchez;A. Plazas;A. Roodman;J. Zuntz;T. Abbott;M. Aguena;S. Allam;J. Annis;S. Ávila;D. Bacon;E. Bertin;S. Bhargava;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;F. Castander;C. Conselice;M. Costanzi;M. Crocce;L. Costa;T. Davis;J. Vicente;S. Desai;H. Diehl;J. Dietrich;P. Doel;A. Drlica;K. Eckert;S. Everett;I. Ferrero;J. Frieman;J. García;D. Gerdes;T. Giannantonio;R. Gruendl;J. Gschwend;G. Gutiérrez;W. Hartley;S. Hinton;D. Hollowood;K. Honscheid;B. Hoyle;E. Huff;D. Huterer;B. Jain;D. James;T. Jeltema;E. Krause;R. Kron;N. Kuropatkin;M. Lima;M. Maia;J. Marshall;R. Miquel;R. Morgan;J. Myles;A. Palmese;F. Paz;E. Rykoff;S. Samuroff;E. Sánchez;V. Scarpine;M. Schubnell;S. Serrano;I. Sevilla;M. Smith;M. Soares;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;C. To;D. Tucker;T. Varga;Risa Wechsler;J. Weller;W. Wester;R. Wilkinson
通讯作者：
R. Wilkinson
DOI：
10.3847/1538-4365/abeb66
发表时间：
2020-11
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
I. Sevilla-Noarbe;K. Bechtol;M. Carrasco Kind;A. Carnero Rosell;M. Becker;A. Drlica-Wagner;R. Gruendl-R.-Grue
通讯作者：
I. Sevilla-Noarbe;K. Bechtol;M. Carrasco Kind;A. Carnero Rosell;M. Becker;A. Drlica-Wagner;R. Gruendl-R.-Grue