利用transit卫星：PAON-4和天籁碟形阵列进行天空重建
Sky reconstruction from transit visibilities: PAON-4 and Tianlai Dish Array
摘要：
球谐$m$ -模式分解是一种适用于工作在凌日模式的射电干涉仪的强有力的天图重建方法。它可以应用于各种配置，包括碟形阵列和圆柱体。文中给出了仪器响应函数、点扩散函数、传递函数、噪声协方差矩阵和噪声功率谱的计算方法。在本文中的分析集中在碟形阵列工作在过境模式。我们发现，具有规则间距的阵列具有更明显的旁瓣，以及在其噪声功率谱的结构，相比，具有不规则间距的阵列，特别是在南北方向。噪声功率谱$C^{\mathrm{noise}}(\ell)$的良好知识对于强度映射实验是必不可少的，因为非均匀$C^{\mathrm{noise}}(\ell)$是HI功率谱测量的潜在问题。不同的配置进行了研究，以优化PAON-4和天籁碟阵列布局。我们提出了他们的预期性能和他们的灵敏度21厘米发射的银河系和当地河外HI团块
英文摘要：
The spherical harmonics $m$-mode decomposition is a powerful sky map reconstruction method suitable for radio interferometers operating in transit mode. It can be applied to various configurations, including dish arrays and cylinders. We describe the computation of the instrument response function, the point spread function (PSF), transfer function, the noise covariance matrix and noise power spectrum. The analysis in this paper is focused on dish arrays operating in transit mode. We show that arrays with regular spacing have more pronounced side lobes as well as structures in their noise power spectrum, compared to arrays with irregular spacing, specially in the north-south direction. A good knowledge of the noise power spectrum $C^{\mathrm{noise}}(\ell)$ is essential for intensity mapping experiments as non uniform $C^{\mathrm{noise}}(\ell)$ is a potential problem for the measurement of the HI power spectrum. Different configurations have been studied to optimise the PAON-4 and Tianlai dish array layouts. We present their expected performance and their sensitivities to the 21-cm emission of the Milky Way and local extragalactic HI clumps
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