The asymmetry of received intensity pattern within the bandwidth is derived from the analogy of the intensity distribution of two-slit interference. This suggests that the length of 1 2 λ delay line should be adjusted to the slightly upper frequency than the central frequency of the radio telescope with a wide bandwith. Some strange communication signals and man-made noises prevented us from obtaining the discernible information from the observed data for the sun. To overcome this difficulties, it is necessary to alter the operating frequency and site. It will be fo1lowed to measure the angular dimensions of the superposed radio sources by changing the distance between two antennas.

ABSTRACT
Ⅰ. 序論
Ⅱ. 位相切換電波干涉計의 製作 및 實驗結果
Ⅲ. 位相切換電波干涉計의 帶域幅
Ⅳ. 結論 및 앞으로의 硏究
參考文獻

• 朴弘緖(Department of Astronomy and Meteorology, College of Liberal Arts and Sciendes, Seoul National University) | Hong Suh Park