LSPE-STRIP利用明亮天体源的在线定标策略
LSPE-STRIP on-sky calibration strategy using bright celestial sources
AI总结：
本文提出LSPE-STRIP微波望远镜的在线定标策略，通过模拟明亮天体源观测，确定增益、偏振、波束和指向等关键仪器参数，以支持B模式偏振探测。
摘要：
本文描述了LSPE-Strip仪器的全局在线定标策略。Strip是一台微波望远镜，工作在Q和W波段（中心频率分别为43和95 GHz），安装于特内里费岛的泰德天文台，其目标是观测并表征偏振银河系前景辐射，并补充由LSPE-SWIPE仪器及其他在更高频率运行的类似实验所进行的宇宙微波背景偏振观测，以探测宇宙暴胀时期的B模式信号。从仪器部分参数（NET、1/f噪声拐点频率、波束特性、观测效率）的基本假设出发，我们进行了真实模拟，研究通过观测Strip覆盖区域内（天空覆盖率为30%）明亮天体定标源所能达到的精度水平，用于确定和表征主要仪器参数：全局和相对增益因子（强度和偏振）、偏振方向、偏振效率、强度到偏振的泄漏、波束、窗口函数和指向模型。
英文摘要：
In this paper we describe the global on-sky calibration strategy of the LSPE-Strip instrument. Strip is a microwave telescope operating in the Q- and W-bands (central frequencies of 43 and 95 GHz respectively) from the Observatorio del Teide in Tenerife, with the goal to observe and characterise the polarised Galactic foreground emission, and complement the observations of the polarisation of the cosmic microwave background to be performed by the LSPE-SWIPE instrument and other similar experiments operating at higher frequencies to target the detection of the B-mode signal from the inflationary epoch of the Universe. Starting from basic assumptions on some of the instrument parameters (NET, 1/f noise knee frequency, beam properties, observing efficiency) we perform realistic simulations to study the level of accuracy that can be achieved through observations of bright celestial calibrators in the Strip footprint (sky fraction of 30 %) on the determination and characterisation of the main instrument parameters: global and relative gain factors (in intensity and in polarisation), polarisation direction, polarisation efficiency, leakage from intensity to polarisation, beams, window functions and pointing model.
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