论文标题
观察地球的偏光宇宙微波背景：扫描策略和偏光仪测试LSPE/带状仪器
Observing the polarized cosmic microwave background from the Earth: scanning strategy and polarimeters test for the LSPE/STRIP instrument
论文作者
论文摘要
在CMB极化模式中检测B模式极化各向异性是现代观察性宇宙学的主要挑战之一，因为它将为我们提供一个重要的证据，有利于通货膨胀范式，并阐明了早期宇宙的物理。需要进行多频观测才能将非常弱的CMB信号与我们银河系中辐射过程的扩散极化前景相差。 “大规模极化探索器”（LSPE）是一个实验，旨在限制张量和标量模式振幅之间的比率，并研究银河系的极化发射。 LSPE由两种乐器组成：滑动，一种平流层气球，在140、210和240 GHz工作，在2021年的极性之夜将在北半球飞行两个星期，而脱衣舞则是一个基于地面的望远镜，该望远镜将于2021年初从“观察者Del Teide”（Observatoratorio del teide''Observatoratorio del Teide在Tenerife of Tenerife theerife of teerife the Skyerving Skyerving Ghz和95 Ghz和95 Ghz和95 Ghz ghz中。在我的论文中，我从2017年9月至2018年7月展示了在“ Degli Studi di Milano Bicocca”上进行的脱衣舞探测器的单位测试活动的结果，并且我介绍了我开发的代码以及我为研究扫描策略而进行的模拟。在单位级测试中，已经对68个极化器进行了800多次测试，以便在中央频率，带宽，噪声温度，白噪声水平，斜坡和膝盖频率方面选择55个具有最佳性能的55测试。剥离扫描策略基于在方位角轴周围旋转望远镜，并以恒定的高度旋转，以重叠滑动覆盖范围，其灵敏度为1.6μk（平均为1°）1°。各个来源将在校准和研究目的上定期观察。
Detecting B-mode polarization anisotropies on large angular scales in the CMB polarization pattern is one of the major challenges in modern observational cosmology since it would give us an important evidence in favor of the inflationary paradigm and would shed light on the physics of the very early Universe. Multi-frequency observations are required to disentangle the very weak CMB signal from diffuse polarized foregrounds originating by radiative processes in our galaxy. The "Large Scale Polarization Explorer" (LSPE) is an experiment that aims to constrain the ratio between the amplitudes of tensor and scalar modes and to study the polarized emission of the Milky Way. LSPE is composed of two instruments: SWIPE, a stratospheric balloon operating at 140, 210 and 240 GHz that will fly for two weeks in the Northern Hemisphere during the polar night of 2021, and STRIP, a ground-based telescope that will start to take data in early 2021 from the "Observatorio del Teide" in Tenerife observing the sky at 43 GHz and 95 GHz. In my thesis, I show the results of the unit-level tests campaign on the STRIP detectors that took place at "Università degli Studi di Milano Bicocca" from September 2017 to July 2018, and I present the code I developed and the simulations I performed to study the STRIP scanning strategy. During the unit-level tests, more than 800 tests on 68 polarimeters have been performed in order to select the 55 with the best performance in terms of central frequencies, bandwidths, noise temperatures, white noise levels, slopes and knee frequencies. The STRIP scanning strategy is based on spinning the telescope around the azimuth axis with constant elevation in order to overlap the SWIPE coverage maintaining a sensitivity of 1.6 μK (on average) per sky pixels of 1°. Individual sources will be periodically observed both for calibration and study purposes.
