Variable-delay polarization modulators for the CLASS telescopes
Variable-delay polarization modulators for the CLASS telescopes
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用于 CLASS 望远镜的可变延迟偏振调制器
DOI：
10.1117/12.2313614
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发表时间：
2018
期刊：
影响因子：
--
通讯作者：
Denes Couto, Jullianna
中科院分区：
文献类型：
--
作者：
Harrington, Kathleen;Ali, Aamir;Appel, John W.;Bennett, Charles L.;Brewer, Michael;Bustos, Ricardo;Chan, Manwei;Chuss, David T.;Cleary, Joseph;Denes Couto, Jullianna
对暴胀原始引力波的搜索和再电离光学深度的测量，都是通过它们在宇宙微波背景（CMB）极化的大角尺度相关性上的印记来实现的，这就产生了对在毫米波波段对天空中大部分区域的极化进行高灵敏度测量的需求。这些测量受到仪器和大气1=f噪声的影响，这促使偏振调制器的发展，以促进抑制这些大的系统效应。变延迟偏振调制器（VPMs）作为光学链中第一个快速调制入射偏振的元件，应用于宇宙大角尺度测量望远镜（CLASS）。VPMs由一个线偏振线网格在一个可移动的平面镜子前面组成。改变栅格和镜面之间的距离会产生平行于栅格和垂直于栅格的偏振态之间的相移变化，从而调制Stokes U（45°线偏振）和Stokes V（圆偏振）。CLASS望远镜将VPMs作为来自天空的第一个光学元件；这同时允许锁定式偏振测量和天空偏振从任何仪器偏振进一步沿着光路分离。CLASS VPM线栅采用50 μm镀铜钨丝，孔径为60 cm，间距为160μm。反射镜安装在具有1度平移自由度的柔性系统上，能够实现所需的反射镜运动，同时保持与线网格的良好平行度。线栅与反射镜的平行度大于80 μm，线栅在60 cm孔径内的均方根误差小于50 μm。q波段CLASS VPM是第一个全职观测CMB的VPM，从2016年春天开始。首个w波段CLASS VPM于2018年春季安装。
The search for inflationary primordial gravitational waves and the measurement of the optical depth to reionization, both through their imprint on the large angular scale correlations in the polarization of the cosmic microwave background (CMB), has created the need for high sensitivity measurements of polarization across large fractions of the sky at millimeter wavelengths. These measurements are subject to instrumental and atmospheric 1=f noise, which has motivated the development of polarization modulators to facilitate the rejection of these large systematic effects.Variable-delay polarization modulators (VPMs) are used in the Cosmology Large Angular Scale Surveyor (CLASS) telescopes as the first element in the optical chain to rapidly modulate the incoming polarization. VPMs consist of a linearly polarizing wire grid in front of a movable flat mirror. Varying the distance between the grid and the mirror produces a changing phase shift between polarization states parallel and perpendicular to the grid which modulates Stokes U (linear polarization at 45°) and Stokes V (circular polarization). The CLASS telescopes have VPMs as the first optical element from the sky; this simultaneously allows a lock-in style polarization measurement and the separation of sky polarization from any instrumental polarization further along in the optical path.The CLASS VPM wire grids use 50 μm copper-plated tungsten wire with a 160μm spacing across a 60 cm clear aperture. The mirror is mounted on a flexure system with one degree of translational freedom, enabling the required mirror motion while maintaining excellent parallelism with respect to the wire grid. The wire grids and mirrors are held parallel to each other to better than 80 μm, and the wire grids have RMS flatness errors below 50 μm across the 60 cm aperture. The Q-band CLASS VPM was the first VPM to begin observing the CMB full time, starting in the Spring of 2016. The first W-band CLASS VPM was installed in the Spring of 2018.
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用于低温毫米波应用的可变延迟偏振调制器。
DOI：
10.1063/1.4879499
发表时间：
2014
期刊：
The Review of scientific instruments
影响因子：
--
作者：
D. Chuss;J. Eimer;D. Fixsen;J. Hinderks;A. Kogut;J. Lazear;P. Mirel;E. Switzer;G. Voellmer;Edward J. Wollack
通讯作者：
Edward J. Wollack
DOI：
10.1117/12.2233125
发表时间：
2016-07
期刊：
--
影响因子：
--
作者：
K. Harrington;T. Marriage;Aamir Ali;J. Appel;C. Bennett;F. Boone;M. Brewer;M. Chan;D. Chuss;F. Colazo;S. Dahal;K. Denis;R. Dünner;J. Eimer;T. Essinger-Hileman;P. Fluxà;M. Halpern;G. Hilton;G. Hinshaw;J. Hubmayr;J. Iuliano;J. Karakla;J. McMahon;N. Miller;S. Moseley;G. Palma;L. Parker;M. Petroff;Basti'an Pradenas;K. Rostem;Marco Sagliocca;Deniz A. N. Valle;D. Watts;Edward J. Wollack;Zhilei Xu;L. Zeng
通讯作者：
K. Harrington;T. Marriage;Aamir Ali;J. Appel;C. Bennett;F. Boone;M. Brewer;M. Chan;D. Chuss;F. Colazo;S. Dahal;K. Denis;R. Dünner;J. Eimer;T. Essinger-Hileman;P. Fluxà;M. Halpern;G. Hilton;G. Hinshaw;J. Hubmayr;J. Iuliano;J. Karakla;J. McMahon;N. Miller;S. Moseley;G. Palma;L. Parker;M. Petroff;Basti'an Pradenas;K. Rostem;Marco Sagliocca;Deniz A. N. Valle;D. Watts;Edward J. Wollack;Zhilei Xu;L. Zeng
Hertz/VPM 旋光计：设计和首次光观察。
影响因子：
1.9
作者：
M. Krejny;D. Chuss;C. d'Aubigny;D. Golish;M. Houde;H. Hui;C. Kulesa;R. Loewenstein;S. Moseley;G. Novak;G. Voellmer;C. Walker;Edward J. Wollack
通讯作者：
Edward J. Wollack
宇宙学大角度尺度测量仪（CLASS）：40 GHz 光学设计
影响因子：
1.9
作者：
J. Eimer;C. Bennett;D. Chuss;T. Marriage;Edward J. Wollack;L. Zeng
通讯作者：
L. Zeng
使用 CLASS 实验样本方差有限 E 模式测量对再电离光学深度进行预测估计
DOI：
10.3847/1538-4357/aad283
发表时间：
2018
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Watts, Duncan J.;Wang, Bingjie;Ali, Aamir;Appel, John W.;Bennett, Charles L.;Chuss, David T.;Dahal, Sumit;Eimer, Joseph R.;Essinger-Hileman, Thomas;Harrington, Kathleen
通讯作者：
Harrington, Kathleen