An Overview of the SPTpol Experiment
An Overview of the SPTpol Experiment
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SPTpol 实验概述
DOI：
10.1007/s10909-012-0505-y
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发表时间：
2012
影响因子：
2
通讯作者：
E. Young
中科院分区：
文献类型：
--
作者：
L. Bleem;P. Ade;K. Aird;J. Austermann;J. Beall;Dan Becker;B. Benson;J. Britton;J. Carlstrom;J. Carlstrom;C. L. Chang;C. L. Chang;Hsiao;T. Haan;T. Crawford;A. Crites;A. Datesman;M. Dobbs;W. Everett;A. Ewall;E. George;N. Halverson;N. Harrington;J. Henning;G. Hilton;W. Holzapfel;S. Hoover;J. Hubmayr;K. Irwin;R. Keisler;J. Kennedy;Adrian T. Lee;E. Leitch;Dale Li;M. Lueker;D. Marrone;J. McMahon;J. Mehl;S. Meyer;J. Montgomery;T. Montroy;T. Natoli;J. Nibarger;M. Niemack;V. Novosad;S. Padin;C. Pryke;C. Reichardt;J. Ruhl;B. Saliwanchik;J. Sayre;K. Schafer;E. Shirokoff;K. Story;K. Vanderlinde;J. Vieira;Gensheng Wang;R. Williamson;V. Yefremenko;K. W. Yoon;E. Young
2012年，南极望远镜(SPT)将开始一次625°2的测量，以测量宇宙微波背景(CMB)的偏振各向异性。CMB B模角功率谱的观测将用于寻找由膨胀引力波引起的大角度尺度信号。此外，B模光谱将通过CMB的引力透镜来测量中微子的质量。新的780像素偏振敏感相机由两种不同的探测器架构组成，将以两种频率绘制天空地图。在150 GHz下，该相机由由美国国家标准与技术研究所(NIST)制造的波纹馈电喇叭耦合TES偏振器阵列组成。在90 GHz，我们使用了阿贡国家实验室开发的独立封装的双偏振吸收耦合偏振测量仪。每个90 GHz像素通过机械加工的轮廓馈电喇叭连接到望远镜。整个焦平面使用数字频域多路复用器系统读出。我们讨论了这个实验的设计和目标，并对探测器进行了描述。
In 2012 the South Pole Telescope (SPT) will begin a 625 deg2 survey to measure the polarization anisotropy of the cosmic microwave background (CMB). Observations of the CMB B-mode angular power spectrum will be used to search for the large angular scale signal induced by inflationary gravitational waves. Additionally, the B-mode spectrum will enable a measurement of the neutrino mass through the gravitational lensing of the CMB. The new 780 pixel polarization-sensitive camera is composed of two different detector architectures and will map the sky at two frequencies. At 150 GHz, the camera consists of arrays of corrugated feedhorn-coupled TES polarimeters fabricated at the National Institute of Standards and Technology (NIST). At 90 GHz, we use individually packaged dual-polarization absorber-coupled polarimeters developed at Argonne National Laboratory. Each 90 GHz pixel couples to the telescope through machined contoured feedhorns. The entire focal plane is read out using a digital frequency-domain multiplexer system. We discuss the design and goals of this experiment and provide a description of the detectors.
DOI：
10.1088/0004-637x/722/2/1180
发表时间：
2010-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
F. W. High;B. Stalder;J. Song;P. Ade;K. Aird;S. Allam;R. Armstrong;W. Barkhouse;B. Benson;B. Benson;E. Bertin;Suman Bhattacharya;L. Bleem;M. Brodwin;E. Buckley-Geer;J. Carlstrom;P. Challis;C. Chang;T. Crawford;A. Crites;T. Haan;S. Desai;M. Dobbs;J. Dudley;R. Foley;E. George;M. Gladders;N. Halverson;M. Hamuy;S. Hansen;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;Adrian T. Lee;Adrian T. Lee;E. Leitch;Huan Lin;Yen-Ting Lin;A. Loehr;M. Lueker;D. Marrone;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. J. Mohr-J.;T. Montroy;N. Morell;C. Ngeow;S. Padin;T. Plagge;T. Plagge;C. Pryke;C. Reichardt;A. Rest;J. Ruel;J. Ruhl;K. Schaffer;L. Shaw;L. Shaw;E. Shirokoff;R. C. Smith;H. Spieler;Z. Staniszewski;A. Stark;C. Stubbs;D. Tucker;K. Vanderlinde;J. Vieira;R. Williamson;W. M. Wood-Vasey;Y. Yang;O. Zahn;A. Zenteno
通讯作者：
F. W. High;B. Stalder;J. Song;P. Ade;K. Aird;S. Allam;R. Armstrong;W. Barkhouse;B. Benson;B. Benson;E. Bertin;Suman Bhattacharya;L. Bleem;M. Brodwin;E. Buckley-Geer;J. Carlstrom;P. Challis;C. Chang;T. Crawford;A. Crites;T. Haan;S. Desai;M. Dobbs;J. Dudley;R. Foley;E. George;M. Gladders;N. Halverson;M. Hamuy;S. Hansen;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;Adrian T. Lee;Adrian T. Lee;E. Leitch;Huan Lin;Yen-Ting Lin;A. Loehr;M. Lueker;D. Marrone;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. J. Mohr-J.;T. Montroy;N. Morell;C. Ngeow;S. Padin;T. Plagge;T. Plagge;C. Pryke;C. Reichardt;A. Rest;J. Ruel;J. Ruhl;K. Schaffer;L. Shaw;L. Shaw;E. Shirokoff;R. C. Smith;H. Spieler;Z. Staniszewski;A. Stark;C. Stubbs;D. Tucker;K. Vanderlinde;J. Vieira;R. Williamson;W. M. Wood-Vasey;Y. Yang;O. Zahn;A. Zenteno