The LSPE collaboration, S. Aiola, G. Amico, P. Battaglia, E. Battistelli, A. Baù, P. de Bernardis, M. Bersanelli, A. Boscaleri, F. Cavaliere, A. Coppolecchia, A… 展开作者
The LSPE collaboration, S. Aiola, G. Amico, P. Battaglia, E. Battistelli, A. Baù, P. de Bernardis, M. Bersanelli, A. Boscaleri, F. Cavaliere, A. Coppolecchia, A. Cruciani, F. Cuttaia, A. D' Addabbo, G. D'Alessandro, S. De Gregori, F. Del Torto, M. De Petris, L. Fiorineschi, C. Franceschet, E. Franceschi, M. Gervasi, D. Goldie, A. Gregorio, V. Haynes, N. Krachmalnicoff, L. Lamagna, B. Maffei, D. Maino, S. Masi, A. Mennella, Ng Ming Wah, G. Morgante, F. Nati, L. Pagano, A. Passerini, O. Peverini, F. Piacentini, L. Piccirillo, G. Pisano, S. Ricciardi, P. Rissone, G. Romeo, M. Salatino, M. Sandri, A. Schillaci, L. Stringhetti, A. Tartari, R. Tascone, L. Terenzi, M. Tomasi, E. Tommasi, F. Villa, G. Virone, S. Withington, A. Zacchei, M. Zannoni
备注：
In press. Copyright 2012 Society of Photo-Optical Instrumentation Engineers. One print or electronic copy may be made for personal use only. Systematic reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited
发表信息：
SPIE proceedings of the Astronomical Telescopes + Instrumentation 2012 Conference - Ground-based and Airborne Instrumentation for Astronomy IV, Amsterdam 1-6 July 2012, paper #8446-277
The LSPE is a balloon-borne mission aimed at measuring the polarization of the Cosmic Microwave Background (CMB) at large angular scales, and in particular to constrain the curl component of CMB polarization (B-modes) produced by tensor perturbations generated during cosmic inflation, in the very early universe. Its primary target is to improve the limit on the ratio of tensor to scalar perturbations amplitudes down to r = 0.03, at 99.7% confidence. A second target is to produce wide maps of foreground polarization generated in our Galaxy by synchrotron emission and interstellar dust emission. These will be important to map Galactic magnetic fields and to study the properties of ionized gas and of diffuse interstellar dust in our Galaxy. The mission is optimized for large angular scales, with coarse angular resolution (around 1.5 degrees FWHM), and wide sky coverage (25% of the sky). The payload will fly in a circumpolar long duration balloon mission during the polar night. Using the Earth as a giant solar shield, the instrument will spin in azimuth, observing a large fraction of the northern sky. The payload will host two instruments. An array of coherent polarimeters using cryogenic HEMT amplifiers will survey the sky at 43 and 90 GHz. An array of bolometric polarimeters, using large throughput multi-mode bolometers and rotating Half Wave Plates (HWP), will survey the same sky region in three bands at 95, 145 and 245 GHz. The wide frequency coverage will allow optimal control of the polarized foregrounds, with comparable angular resolution at all frequencies.
The STRIP instrument of the Large Scale Polarization Explorer: microwave eyes to map the Galactic polarized foregrounds
本文讨论了“大尺度偏振探测器”（LSPE）实验中STRIP仪器的最新进展。LSPE是一个新颖的项目，它结合了地基（STRIP）和球载（SWIPE）的大角度尺度上的微波天空的偏振测量，试图探测宇宙微波背景偏振的“B模式”。STRIP将从特内里费岛的“Observatorio del Teide”观测大约25%的北方天空，使用43 GHz的49个相干偏振仪阵列，与1.5米全旋转交叉Dragone望远镜耦合。第二个频道有六个单元，频率为95千兆赫，将用作大气监测器。目前，STRIP仪器的大部分硬件已经在子系统级开发和测试。从2018年7月开始的系统级表征将使STRIP在年底内在观测站进行运输和安装。整个仪器的现场检定和校准将为STRIP进行为期2年的CMB偏振观测做好准备。
A Pipeline for the AI-Assisted Analysis of Imaging X-ray Polarimetry Explorer Observations of Black Hole X-ray Binaries and Limits on Their Polarization Variability
Washington University in St. Louis（华盛顿大学圣路易斯分校）；Washington University in St. Louis McDonnell Center for the Space Sciences and Center for Quantum Leaps（华盛顿大学圣路易斯分校麦克唐纳空间科学中心与量子跃迁中心）
