North Celestial Region Observed with 21 CentiMeter Array  

作　　者：Bi-Xuan Zhao Qian Zheng Huan-Yuan Shan Quan Guo Kuan-Jun Li 

机构地区：[1]Shanghai Astronomical Observatory,Chinese Academy of Sciences,80 Nandan Road,Shanghai 200030,China [2]National Astronomical Observatory,Chinese Academy of Sciences,20 Datun Road,Beijing 100101,China

出　　处：《Research in Astronomy and Astrophysics》2022年第1期126-136,共11页天文和天体物理学研究（英文版）

基　　金：supported by the National SKA Program of China No.2020SKA0110100;the Key Projects of Frontier Science of Chinese Academy of Sciences under grant No.QYZDYSSW-SLH022;the Strategic Priority Research Program of Chinese Academy of Sciences under grant No.XDB23000000;sponsorship from Shanghai Pujiang Program 19PJ1410800and NSFC of China under grant 11973069;sponsorship from Shanghai Pujiang Program 19PJ1410700;support from NSFC under grant 11973070;the Shanghai Committee of Science and Technology grant No.19ZR1466600;Key Research Program of Frontier Sciences,CAS,grant No.ZDBS-LY-7013。

摘　　要：The 21 CentiMeter Array(21 CMA) is a radio interferometer in western China. The key science objective of21 CMA is statistically measuring the redshifted H I 21 cm signal of the Epoch of Reionization(EoR). In order to achieve this, a catalog of radio sources is necessary for both calibration and foreground removal. In this work, we present a catalog of 832 radio sources within a radius of 5° around the North Celestial Pole region observed with21 CMA. Three days of data taken in 2013 are used in the analysis, with a frequency coverage from 75 to 200 MHz and an angular resolution of about two arcminutes at 200 MHz. Flux densities and estimated spectral indices of the radio sources are provided in the source catalog. For simplicity, only the east–west baseline is used for the observations to avoid the so-called w-term in the data analysis. The longest baseline along the east–west direction is 2780 m. Comparing our source counts with other radio observations, we find a good agreement with the observations made with the Giant Metrewave Radio Telescope and Murchison Widefield Array. Our data reduction is still limited by grating lobes of very bright sources in the field due to the redundant configuration of21 CMA. We note that understanding the properties of radio sources, and modeling and removing the radio sources are challenges for the EoR experiments.

关 键 词：radio continuum:general instrumentation:interferometers radio continuum:galaxies methods:observational 

分 类 号：P16[天文地球—天文学]