This post is also available in: English (英語)
基本的な撮像手段が今と同じですが、撮像デバイスは1-２世代前ですね。当時は高かった冷却CCDカメラ（Teleris2,KAF-400e),特注メタンバンドフィルター（日本真空光学,半値幅6.5nm)では32㎝反射（F/32 3×3のビニング撮像で2０秒と現在の100倍露光、相当大変だった。貧弱な画像ではあったが、CH4 画像がアマチュアでも可能となり、うれしかった。木星面では明らかに大きいGRSと永続白斑BE（前方）とFA（後方）がCH4では捉え、その後2000年の3月後半に2つの永続白斑が合体し今のBAを形成。
The image of Jupiter from 1999
The basic imaging method is the same as it is now, but the imaging device is 1-2 generations ago. The cooled CCD camera (Teleris2, KAF-400e), which was expensive at that time, and the custom-made methane band filter (Nippon Vacuum Optics, half-value width 6.5 nm) 32 cm newtonian (F / 32 3×3 binning imaging in 20 seconds, which is now 100 times more exposed. It was quite difficult. It was a poor image, but I was happy that the CH4 image was possible even for amateurs. On the Jupiter feature, the clearly large GRS and permanent white spot BE (front) and FA (rear) were captured by CH4, and then In the latter half of March 2000, two permanent white spots merged to form the current Oval BA.
