Survey strategy optimization for the Atacama Cosmology Telescope
Survey strategy optimization for the Atacama Cosmology Telescope
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阿塔卡马宇宙学望远镜巡天策略优化
DOI：
10.1117/12.2232824
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
De Bernardis - For The ACT Collaboration F
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文献类型：
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作者：
De Bernardis - For The ACT Collaboration F
近年来，用于观测宇宙微波背景辐射的仪器在灵敏度和角分辨率方面都有了很大的提高。ACTPol是阿塔卡马宇宙学望远镜（ACT）的第一个偏振接收器，正在以超过2000平方英尺的arcmin分辨率观测CMB天空。°的它的升级，先进的ACTPol（AdvACT），将在五个频段和更大的天空区域观察CMB。我们描述了ACTPol和AdvACT调查的优化和实施。观测场的选择主要受科学目标的驱动，即小角度尺度CMB测量、B模式测量和互相关研究。对于ACTPol调查，我们观察到了南银河系天空的低银河前景发射，这也是为了最大限度地与几个星系调查重叠，以允许独特的互相关研究。在北方银帽的更宽的区域确保了与BOSS分光巡天有显著的额外重叠。通过观察具有不同扫描方向的场，优化场的确切形状和足迹以实现均匀覆盖并获得交联图。我们通过实施接近24小时的观测策略，在白天和夜间观测计划之间切换，并最大限度地减少望远镜空闲时间，最大限度地提高了调查的效率。我们描述了由AdvACT观测到的显著更宽区域的调查优化所代表的挑战，该区域将观测到大约一半的低前景天空。这里描述的调查策略可能会被证明是有用的未来的地面CMB调查，如西蒙斯天文台和CMB第四阶段调查的规划。
In recent years there have been significant improvements in the sensitivity and the angular resolution of the instruments dedicated to the observation of the Cosmic Microwave Background (CMB). ACTPol is the first polarization receiver for the Atacama Cosmology Telescope (ACT) and is observing the CMB sky with arcmin resolution over 2000 sq. deg. Its upgrade, Advanced ACTPol (AdvACT), will observe the CMB in five frequency bands and over a larger area of the sky. We describe the optimization and implementation of the ACTPol and AdvACT surveys. The selection of the observed fields is driven mainly by the science goals, that is, small angular scale CMB measurements, B-mode measurements and cross-correlation studies. For the ACTPol survey we have observed patches of the southern galactic sky with low galactic foreground emissions which were also chosen to maximize the overlap with several galaxy surveys to allow unique cross-correlation studies. A wider field in the northern galactic cap ensured significant additional overlap with the BOSS spectroscopic survey. The exact shapes and footprints of the fields were optimized to achieve uniform coverage and to obtain cross-linked maps by observing the fields with different scan directions. We have maximized the efficiency of the survey by implementing a close to 24 hour observing strategy, switching between daytime and nighttime observing plans and minimizing the telescope idle time. We describe the challenges represented by the survey optimization for the significantly wider area observed by AdvACT, which will observe roughly half of the low-foreground sky. The survey strategies described here may prove useful for planning future ground-based CMB surveys, such as the Simons Observatory and CMB Stage IV surveys.
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T. Hasekawa：“蛇夫座超星系团大规模结构的发现”《天体物理学杂志》。
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暗能量勘测相机（DECam）项目的现状
DOI：
10.1117/12.926216
发表时间：
2012
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作者：
Flaugher B
通讯作者：
Flaugher B
DOI：
10.1117/12.927286
发表时间：
2012-09
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作者：
J. Austermann;K. Aird;J. Beall;D. Becker;A. Bender;B. Benson;L. Bleem;J. Britton;J. Carlstrom;J. Carlstrom;C. Chang;C. Chang;H. Chiang;H. Cho;T. Crawford;A. Crites;A. Datesman;T. Haan;M. Dobbs;E. George;N. Halverson;N. Harrington;J. Henning;G. Hilton;G. Holder;W. Holzapfel;S. Hoover;Norden E. Huang;J. Hubmayr;K. Irwin;R. Keisler;J. Kennedy;L. Knox;Adrian T. Lee;E. Leitch;Dale Li;M. Lueker;D. Marrone;J. McMahon;J. Mehl;S. Meyer;T. Montroy;T. Natoli;J. Nibarger;M. Niemack;V. Novosad;S. Padin;C. Pryke;C. Reichardt;J. Ruhl;B. Saliwanchik;J. Sayre;K. Schaffer;E. Shirokoff;A. Stark;K. Story;K. Vanderlinde;J. Vieira;Gensheng Wang;R. Williamson;V. Yefremenko;K. W. Yoon;O. Zahn
通讯作者：
J. Austermann;K. Aird;J. Beall;D. Becker;A. Bender;B. Benson;L. Bleem;J. Britton;J. Carlstrom;J. Carlstrom;C. Chang;C. Chang;H. Chiang;H. Cho;T. Crawford;A. Crites;A. Datesman;T. Haan;M. Dobbs;E. George;N. Halverson;N. Harrington;J. Henning;G. Hilton;G. Holder;W. Holzapfel;S. Hoover;Norden E. Huang;J. Hubmayr;K. Irwin;R. Keisler;J. Kennedy;L. Knox;Adrian T. Lee;E. Leitch;Dale Li;M. Lueker;D. Marrone;J. McMahon;J. Mehl;S. Meyer;T. Montroy;T. Natoli;J. Nibarger;M. Niemack;V. Novosad;S. Padin;C. Pryke;C. Reichardt;J. Ruhl;B. Saliwanchik;J. Sayre;K. Schaffer;E. Shirokoff;A. Stark;K. Story;K. Vanderlinde;J. Vieira;Gensheng Wang;R. Williamson;V. Yefremenko;K. W. Yoon;O. Zahn
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发表时间：
2010-11
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影响因子：
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作者：
The Polarbear Collaboration J. Errard;P. Ade;A. Anthony;K. Arnold;F. Aubin;D. Boettger;J. Borrill;C. Cantalupo;M. Dobbs;D. Flanigan;A. Ghribi;N. Halverson;M. Hazumi;W. Holzapfel;J. Howard;P. Hyland;A. Jaffe;B. Keating;T. Kisner;Z. Kermish;A. Lee;E. Linder;M. Lungu;T. Matsumura;N. Miller;X. Meng;M. Myers;H. Nishino;R. O’Brient;D. O'Dea;C. Reichardt;I. Schanning;A. Shimizu;C. Shimmin;M. Shimon;H. Spieler;B. Steinbach;R. Stompor;A. Suzuki;T. Tomaru;H. Tran;C. Tucker;E. Quealy;P. Richards;O. Z. L. AstroparticuleCosmologie;7. Universit'eParis;France.;D. Physics;U. California;Berkeley U.S.;S. O. Physics;Astronomy;U. Cardiff;U.K.;Department of Astrophysical;P. Sciences;U. Colorado;U.S.;Center for Computational Astrophysics;S. Sciences;San Diego;Computational Cosmology Center;L. B. N. Laboratory;Space Sciences Laboratory;Berkeley;P. Department;Mcgill University;Canada.;High Energy Accelerator Research Organization;Tsukuba;Ibaraki;Japan.;I. College;P. Division
通讯作者：
The Polarbear Collaboration J. Errard;P. Ade;A. Anthony;K. Arnold;F. Aubin;D. Boettger;J. Borrill;C. Cantalupo;M. Dobbs;D. Flanigan;A. Ghribi;N. Halverson;M. Hazumi;W. Holzapfel;J. Howard;P. Hyland;A. Jaffe;B. Keating;T. Kisner;Z. Kermish;A. Lee;E. Linder;M. Lungu;T. Matsumura;N. Miller;X. Meng;M. Myers;H. Nishino;R. O’Brient;D. O'Dea;C. Reichardt;I. Schanning;A. Shimizu;C. Shimmin;M. Shimon;H. Spieler;B. Steinbach;R. Stompor;A. Suzuki;T. Tomaru;H. Tran;C. Tucker;E. Quealy;P. Richards;O. Z. L. AstroparticuleCosmologie;7. Universit'eParis;France.;D. Physics;U. California;Berkeley U.S.;S. O. Physics;Astronomy;U. Cardiff;U.K.;Department of Astrophysical;P. Sciences;U. Colorado;U.S.;Center for Computational Astrophysics;S. Sciences;San Diego;Computational Cosmology Center;L. B. N. Laboratory;Space Sciences Laboratory;Berkeley;P. Department;Mcgill University;Canada.;High Energy Accelerator Research Organization;Tsukuba;Ibaraki;Japan.;I. College;P. Division
小场调制 CMB 偏振实验中的制图：近似最大似然法
DOI：
10.1111/j.1365-2966.2008.14195.x
发表时间：
2008
影响因子：
4.8
作者：
D. Sutton;B. Johnson;M. Brown;P. Cabella;P. Ferreira;K. Smith
通讯作者：
K. Smith