Dark Energy Survey Year 3 Results: A 2.7% measurement of Baryon Acoustic Oscillation distance scale at redshift 0.835
Dark Energy Survey Year 3 Results: A 2.7% measurement of Baryon Acoustic Oscillation distance scale at redshift 0.835
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DOI：
10.1103/physrevd.105.043512
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发表时间：
2021-07
期刊：
影响因子：
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通讯作者：
D. C. T. Abbott;M. Aguena;S. Allam;F. Andrade-Oliveira;J. Asorey;S. Ávila;G. Bernstein;E. Bertin;A. Brandao-Souza;D. Brooks;D. Burke;J. Calcino;H. Camacho;A. Rosell;D. Carollo;M. Kind;J. Carretero;F. Castander;R. Cawthon;K. Chan;A. Choi;C. Conselice;M. Costanzi;M. Crocce;L. Costa;M. Pereira;T. Davis;J. Vicente;S. Desai;H. Diehl;P. Doel;K. Eckert;J. Elvin-Poole;S. Everett;A. Evrard;X. Fang;I. Ferrero;A. Fert'e;B. Flaugher;P. Fosalba;J. Garc'ia-Bellido;E. Gaztañaga;D. Gerdes;T. Giannantonio;K. Glazebrook;D. Gomes;D. Gruen;R. Gruendl;J. Gschwend;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;D. Huterer;B. Jain;D. James;T. Jeltema;N. Kokron;E. Krause;K. Kuehn;O. Lahav;G. Lewis;C. Lidman;M. Lima;H. Lin;M. Maia;U. Malik;P. Martini;Peter Melchior;J. Mena-Fern'andez;F. Menanteau;R. Miquel;J. Mohr;R. Morgan;J. Muir;J. Myles;A. Moller;A. Palmese;F. Paz-Chinch'on;W. Percival;A. Pieres;A. P. Malag'on;A. Porredon;J. Prat;M. Rodríguez-Monroy;A. Romer;A. Roodman;R. Rosenfeld;A. Ross;E. Sanchez;D. S. Cid;V. Scarpine;S. Serrano;I. Sevilla-Noarbe;E. Sheldon;M. Smith;M. Soares-Santos;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;C. To;M. Troxel;B. Tucker;D. Tucker;I. Tutusaus;S. Uddin;T. Varga;J. Weller;R. Wilkinson
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作者：
D. C. T. Abbott;M. Aguena;S. Allam;F. Andrade-Oliveira;J. Asorey;S. Ávila;G. Bernstein;E. Bertin;A. Brandao-Souza;D. Brooks;D. Burke;J. Calcino;H. Camacho;A. Rosell;D. Carollo;M. Kind;J. Carretero;F. Castander;R. Cawthon;K. Chan;A. Choi;C. Conselice;M. Costanzi;M. Crocce;L. Costa;M. Pereira;T. Davis;J. Vicente;S. Desai;H. Diehl;P. Doel;K. Eckert;J. Elvin-Poole;S. Everett;A. Evrard;X. Fang;I. Ferrero;A. Fert'e;B. Flaugher;P. Fosalba;J. Garc'ia-Bellido;E. Gaztañaga;D. Gerdes;T. Giannantonio;K. Glazebrook;D. Gomes;D. Gruen;R. Gruendl;J. Gschwend;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;D. Huterer;B. Jain;D. James;T. Jeltema;N. Kokron;E. Krause;K. Kuehn;O. Lahav;G. Lewis;C. Lidman;M. Lima;H. Lin;M. Maia;U. Malik;P. Martini;Peter Melchior;J. Mena-Fern'andez;F. Menanteau;R. Miquel;J. Mohr;R. Morgan;J. Muir;J. Myles;A. Moller;A. Palmese;F. Paz-Chinch'on;W. Percival;A. Pieres;A. P. Malag'on;A. Porredon;J. Prat;M. Rodríguez-Monroy;A. Romer;A. Roodman;R. Rosenfeld;A. Ross;E. Sanchez;D. S. Cid;V. Scarpine;S. Serrano;I. Sevilla-Noarbe;E. Sheldon;M. Smith;M. Soares-Santos;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;C. To;M. Troxel;B. Tucker;D. Tucker;I. Tutusaus;S. Uddin;T. Varga;J. Weller;R. Wilkinson
我们目前的角直径测量获得的测量位置的重子声振荡（BAO）在一个优化的样本中的星系从第一个三年的暗能量调查数据（DES Y3）。该样本由700万个星系组成，分布在4100 deg$^2$的足迹上，$为0.60.75 $。当与DES 3x 2 pt + SNIa相结合时，它们导致$H_0 $和$\Omega_m$约束的$\sim 20\%$改进
We present angular diameter measurements obtained by measuring the position of Baryon Acoustic Oscillations (BAO) in an optimised sample of galaxies from the first three years of Dark Energy Survey data (DES Y3). The sample consists of 7 million galaxies distributed over a footprint of 4100 deg$^2$ with $0.60.75$. When combined with DES 3x2pt + SNIa, they lead to improvements in $H_0$ and $\Omega_m$ constraints by $\sim 20\%$