@article{oai:jaxa.repo.nii.ac.jp:00033097,
 author = {山岡, 典子 and 釜江, 常好 and 高橋, 忠幸 and 郡司, 修一 and 田村, 忠久 and 宮崎, 聡 and 関本, 裕太郎 and 田中, 光明 and 山上, 隆正 and 西村, 純 and 矢島, 信之 and 能町, 正治 and 村上, 浩之 and 中川, 道夫 and Yamaoka, Noriko and Kamae, Tuneyoshi and Takahashi, Tadayuki and Gunji, Shuichi and Tamura, Tadahisa and Miyazaki, Satoshi and Sekimoto, Yutaro and Tanaka, Mitsuaki and Yamagami, Takamasa and Nishimura, Jun and Yajima, Nobuyuki and Nomachi, Masaharu and Murakami, Hiroyuki and Nakagawa, Michio},
 journal = {宇宙科学研究所報告. 特集: 大気球研究報告},
 month = {Dec},
 note = {マイクロチャネルプレート(MCP)とCCDカメラとを組み合わせたナイトビュアー, VMEバス上の搭載用計算機とビデオモジュールを用いて画像処理を行う気球搭載用スターセンサーシステムを開発した。本システムは画角9.1×6.3度を持ち, 光度8.1等までの星を観測できた。本システムで絶対方位を知り, 更に検出器をその方位に指向させる「より戻し制御方式」で方向規正することで±0.5度の精度で追尾観測を可能にした。, We developed a new kind of star sensor system for a balloon borne experiment. A MCP (micro channel plate) coupled to a CCD camera images the sky. Its field of view is 9.1×6.3 degrees and identifies stars of magnitude ∿8.1. The star image on the CCD camera is digitalized (512×512 pixels) by the image processing board on VME bus. The microprocessor selects the bright points and then transmits brightness and position of each point to the ground through PCM telemetry (max 2kB/s). On the ground station, the star image is reconstructed every three seconds by using a 32bit workstation. In 1989 we used this star sensor system for the experiment Welcome, to observe hard X/γ rays from astronomical objects. From the reconstructed star image the direction of payload was determined within ±0.02 degree. The attitude of the payload was controlled by yorimodoshi method. And the combination with the new star sensor system enabled us to track the astronomical source with a stability better than ±0.5 degree., 資料番号: SA0166966000},
 pages = {73--84},
 title = {MCP を用いた気球用高感度スターセンサーシステムの開発},
 volume = {27},
 year = {1990}
}