论文标题
田莱盘阵列低Z调查预测
The Tianlai dish array low-z surveys forecasts
论文作者
论文摘要
我们介绍了调查的科学案例，该案例用Tianlai Dish Dish阵列干涉仪调谐到$ \左[1300，1400 \右] \ Mathrm {MHz} $频率范围。从根据调查策略的逼真的模拟可见性数据开始，我们重建了天空的地图并进行前景减法。 We show that a survey of the North Celestial Polar cap during a year of observing time and covering an area of $150 \, \mathrm{deg^2}$ would reach a sensitivity of $ 1.5-2 \, \mathrm{mK} $ per $1 \, \mathrm{MHz} \times 0.25^2 \, \mathrm{deg^2 }$ voxel and通过混合模式略微影响。田莱将能够检测到附近的少数$（\ sim 10）$（\ sim 10），以及与北天体帽调查光学星系的21 \ 21 \，CM强度图的非常强的互相关信号。我们还研究了中纬度调查的性能，涵盖了$ \ sim 1500 \，\ mathrm {deg^2} $，以$δ= 55^\ circ $的偏好为中心，这与Sloan Digital Sky Survey Footprint重叠。尽管中纬度调查的噪声水平较高，并且由于模式混合而引起的显着扭曲，但天莱仍能够检测到21 \，CM信号与斯隆语光学银河系样品之间的高度显着的互相关。使用来自这两个调查的任何一个或两种调查的外乳外信号，都可以评估校准不确定性，天线模式不确定性，噪声源和模式混合的影响，以进行未来的调查，需要更高的灵敏度。
We present the science case for surveys with the Tianlai dish array interferometer tuned to the $\left[ 1300, 1400 \right] \mathrm{MHz}$ frequency range. Starting from a realistic generation of mock visibility data according to the survey strategy, we reconstruct a map of the sky and perform a foreground subtraction. We show that a survey of the North Celestial Polar cap during a year of observing time and covering an area of $150 \, \mathrm{deg^2}$ would reach a sensitivity of $ 1.5-2 \, \mathrm{mK} $ per $1 \, \mathrm{MHz} \times 0.25^2 \, \mathrm{deg^2 }$ voxel and be marginally impacted by mode-mixing. Tianlai would be able to detect a handful $(\sim 10)$ of nearby massive \HI clumps as well as a very strong cross-correlation signal of 21\,cm intensity maps with the North Celestial Cap Survey optical galaxies. We have also studied the performance of a mid-latitude survey, covering $\sim 1500 \, \mathrm{deg^2}$ centered on a declination of $δ=55^\circ$, which overlaps the Sloan Digital Sky Survey footprint. Despite a higher noise level for the mid-latitude survey, as well as significant distortions due to mode mixing, Tianlai would be able to detect a highly significant cross-correlation between the 21\,cm signal and the Sloan spectroscopic galaxy sample. Using the extragalactic signals from either or both of these surveys, it will be possible to assess the impact of calibration uncertainties, antenna pattern uncertainties, sources of noise, and mode mixing for future surveys requiring higher sensitivity.
