Characterization and performance of the second-year SPT-3G focal plane-猫眼课题宝

第二年SPT-3G焦平面的特性和性能

DOI：

发表时间：

2018

期刊：

Astronomical Telescopes + Instrumentation

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作者：

D. Dutcher;P. Ade;Z. Ahmed;A. Anderson;J. Avva;R. Thakur;A. Bender;A. Bender;B. Benson;J. Carlstrom;J. Carlstrom;F. Carter;F. Carter;T. Cecil;C. Chang;C. Chang;J. Cliche;A. Cukierman;T. Haan;J. Ding;M. Dobbs;M. Dobbs;W. Everett;A. Foster;J. Gallicchio;J. Gallicchio;A. Gilbert;J. Groh;A. Harke;A. Harke;S. Guns;N. Halverson;N. Harrington;J. Henning;J. Henning;W. Holzapfel;N. Huang;K. Irwin;O. Jeong;M. Jonas;T. Khaire;A. Kofman;M. Korman;D. Kubik;S. Kuhlmann;Chaohua Kuo;A. Lowitz;Adrian T. Lee;Adrian T. Lee;S. Meyer;D. Michalik;J. Montgomery;A. Nadolski;T. Natoli;H. Nguyen;G. Noble;V. Novosad;S. Padin;Z. Pan;J. Pearson;C. Posada;W. Quan;A. Rahlin;J. Ruhl;J. Sayre;E. Shirokoff;G. Smecher;J. Sobrin;A. Stark;K. Story;A. Suzuki;K. Thompson;C. Tucker;K. Vanderlinde;J. Vieira;J. Vieira;Gensheng Wang;N. Whitehorn;N. Whitehorn;V. Yefremenko;K. Yoon;M. Young

10米南极望远镜的第三代仪器SPT-3G于2017年1月首次安装。除了全新的低温恒温器、二次望远镜光学系统和读出电子设备外，焦平面上的探测器数量比以前的仪器增加了一个数量级，达到了16000个。SPT-3G焦平面由十个探测器模块组成，每个模块在一块6英寸的硅片上有269个三色偏振敏感像素阵列。每个像素内是一个宽带双极化正弦天线；每个正交线偏振的信号被直列集总元件滤波器分为以95、150和220 GHz为中心的三个频段，并通过超导微带传输到Ti/Au过渡边缘传感器（TES）辐射热计。TES薄膜、微带滤波器和辐射热计岛的性能必须严格控制，以达到最佳性能。在SPT-3G运行的第二年，我们用新的探测器阵列替换了焦平面上的所有10个晶圆，以提高映射速度并提高整体性能。在这里，我们讨论了2018焦平面的TES超导转变温度和正常电阻，探测器饱和功率，带通，光效率和全阵列良率。

The third-generation instrument for the 10-meter South Pole Telescope, SPT-3G, was first installed in January 2017. In addition to completely new cryostats, secondary telescope optics, and readout electronics, the number of detectors in the focal plane has increased by an order of magnitude from previous instruments to ~16,000. The SPT-3G focal plane consists of ten detector modules, each with an array of 269 trichroic, polarization-sensitive pixels on a six-inch silicon wafer. Within each pixel is a broadband, dual-polarization sinuous antenna; the signal from each orthogonal linear polarization is divided into three frequency bands centered at 95, 150, and 220 GHz by in-line lumped element filters and transmitted via superconducting microstrip to Ti/Au transition-edge sensor (TES) bolometers. Properties of the TES film, microstrip filters, and bolometer island must be tightly controlled to achieve optimal performance. For the second year of SPT-3G operation, we have replaced all ten wafers in the focal plane with new detector arrays tuned to increase mapping speed and improve overall performance. Here we discuss the TES superconducting transition temperature and normal resistance, detector saturation power, bandpasses, optical efficiency, and full array yield for the 2018 focal plane.

QUaD: A HIGH-RESOLUTION COSMIC MICROWAVE BACKGROUND POLARIMETER

DOI： 10.1088/0004-637x/692/2/1221

发表时间： 2008-05

期刊：

The Astrophysical Journal

影响因子： --

作者：

QUaD collaboration J. R. Hinderks;P. Ade;J. Bock;M. Bowden;M. L. Brown;G. Cahill;J. Carlstrom;P. G. Castro;S. Church;T. Culverhouse;R. Friedman;K. Ganga;W. Gear;S. Gupta;J. Harris;V. Haynes;B. Keating;J. Kovac;E. Kirby;A. E. Lange;E. Leitch;O. Mallie;S. Melhuish;Y. Memari;J. A. Murphy;A. Orlando;R. Schwarz;C. O'Sullivan;L. Piccirillo;C. Pryke;N. Rajguru;B. Rusholme;A. Taylor;K. Thompson;C. Tucker;A. H. Turner;E. Y. S. Wu;M. University;Nasa Goddard Cardiff University;Jpl Caltech University of Edinburgh;U. Cambridge;National University of Ireland Maynooth;U. Chicago;Universidade T'ecnica de Lisboa;Laboratoire Apccnrs;U. Manchester;University of California San Diego University College London-University-of-California-San-Diego-University-2303464988

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Characterization and performance of the second-year SPT-3G focal plane

第二年SPT-3G焦平面的特性和性能

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