System Development of Micoro-Channel-Spatial Light Modulator for Fast Fourier Transformation

快速傅立叶变换微通道空间光调制器系统开发

• 批准号: 63840002
• 负责人: ISOBE Syuzo
• 金额: $ 4.74万
• 依托单位: National Astronomical Observatory
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Developmental Scientific Research
• 财政年份: 1988
• 资助国家: 日本
• 起止时间: 1988 至 1989
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-63840002/
• 关键词: Interferometry; Speckle Interferometry; Fourier Transformation; Double Stars; Stellar Surface Distribution; Spatial Light Modulator System; スペック干渉; フーリェ変換

Stellar light is disturbed during a passage through atmosphere. We developed a hard-ware system to make real time processing of the disturb images and found that our system is applicable to astronomical image processing as well as to the other purpose.1). We developed a soft-ware to control our Micro-Channel-Spatial Light Modulator (MSLM) bought last fiscal year. Its test measurement was carried out using artificial light, and we found that our system works well. 2) We succeeded to identify each components of double stars with angular separation less than 1 arc-second from video data obtained last fiscal year by the 188 cm telescope at the Okayama Astrophysical Observatory. 3). Further,we set our system of MSLM on the telescope, and detected a fringe of double stars in real time.Through these experiments, we are confident that we solved our target settled in this project. That is, a fourier transformation is applied to input image data in real time using our developing hardware system. We also succeeded to reduce a weight and volume of MSLM, and then make it portable. At the present stage, we took a cycle time of 2 Hz in consideration of life time of MSLM, but to make this system applicable to wider fields such as computer.

恒星光在穿过大气层的过程中受到干扰。我们开发了一个硬件系统对干扰图像进行实时处理，发现我们的系统既适用于天文图像处理，也适用于其他目的。我们开发了一个软件来控制我们上个财年购买的微通道-空间光调制器(MSLM)。它的测试测量是用人造光进行的，我们发现我们的系统工作良好。2)我们成功地从上一财政年度冈山天体物理观测站188厘米望远镜获得的视频数据中识别出角差小于1角秒的双星的各个组成部分。3)。此外，我们将MSLM系统安装在望远镜上，实时探测到了双星的条纹，通过这些实验，我们有信心解决了我们在这个项目中确定的目标。也就是说，利用我们正在开发的硬件系统，对实时输入的图像数据进行傅里叶变换。我们还成功地减轻了MSLM的重量和体积，然后使其便携。在现阶段，考虑到MSLM的寿命，我们采用了2赫兹的周期时间，但为了使该系统适用于更广泛的领域，如计算机。

项目成果

N.Baba;M.Tabata: in the Proceedings of NOAO-ESO conference on high-resolution imaging by interferometry. 447-453 (1988)

N.Baba；M.Tabata：NOAO-ESO 干涉测量高分辨率成像会议记录。

S.Isobe,他7名: "Speckle Observations of Visual and Spectroscopic Binaries.I." Publications of National Astronomical Observatory. 2. (1990)

S. Isobe 和其他 7 人：“视觉和光谱双星的散斑观测。I”，国家天文台出版物 2。（1990 年）

S.Isobe: "Optical interferometer between the JNLT and WMKT on Mauna Kea" in the Proceedings of ESO Conference on very large Telescopes and their instrumentations. 781-785 (1988)

S.Isobe：“莫纳克亚山 JNLT 和 WMKT 之间的光学干涉仪”，欧洲南方天文台超大型望远镜及其仪器会议记录。

N.Baba;M.Tabata;K.Murata: Optical Letters. 13. 616-618 (1988)

N.Baba；M.Tabata；K.Murata：光学信件。

J.Ohtsubo: "Effect of spectral bandwidth on the MTF instellar speckle interferometry" Optical Communication. 65. 79-83 (1988)

J.Ohtsubo：“光谱带宽对 MTF 恒星散斑干涉测量的影响”光通信。