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天文学
天文学是一门涉及外星观测的自然科学。该领域研究近地物体和其他天文现象，以帮助找到宇宙起源的答案，了解我们的太阳系和星系，并发现物质定律。天文学使用各种成像技术，例如太阳成像和光谱学，来研究太阳的活动和地球上方发生极光的大气层等领域。基于图像传感器和相机的成像技术在世界各地被用于望远镜中。
使用超大望远镜进行天文观测
大型望远镜用于观测外行星和原行星系，旨在寻找生命迹象，并通过直接测量宇宙膨胀来研究暗能量的性质。
全世界许多地方均已安装了各种大型望远镜并用于观察太空，例如夏威夷大岛莫纳克亚山顶的斯巴鲁望远镜、三十米望远镜 (TMT)、凯克望远镜和双子座望远镜；智利阿塔卡马沙漠的阿尔玛望远镜；以及加那利群岛拉帕尔马岛上的加纳利大望远镜等。
斯巴鲁望远镜拍摄的仙女座星系 (M31)
使用我们产品的实例：斯巴鲁望远镜
斯巴鲁望远镜是一款大型国家级光学/红外望远镜，位于夏威夷岛莫纳克亚山顶。它是世界上最强大的望远镜之一，用于研究宇宙膨胀的历史和测量暗能量。
我们的图像传感器安装在斯巴鲁望远镜的主焦相机中。此外，我们的图像传感器还将安装在光谱仪中，该光谱仪于 2024 年开始运行；我们的 CMOS 相机还将安装在 ULTIMATE-Subaru（用于超越性探索 (Transcendent Exploration) 的超宽激光断层成像仪和带 AO 的 MOS）自适应光学系统的波前传感器中，该系统将于 2027 年开始运行.
由我们的产品提供支持的斯巴鲁望远镜以及斯巴鲁 2 项目中的主要系统
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天文学是一个进行各种研究以发现和探索未知天体和天文现象的领域。本手册介绍了此类应用的示例，以及适用于每种应用的相机。
自适应光学
使用地面望远镜进行天文观测时，会受到由气温差异和风引起的大气湍流的极大影响，从而导致恒星图像失真。自适应光学技术是一种通过立即校正受干扰的波面，在望远镜的性能极限范围内获得最清晰、最无失真的恒星图像的方法。为了实现实时和高精度的波前校正，用于测量波前湍流的相机必须具备快速读出性能和高分辨率。此外，相机还必须具有高灵敏度，因为在光子数很低的情况下，如较暗的物体或激光人造星，可能需要进行波前校正。
通过自适应光学技术进行波前校正
有无自适应光学技术的比较
*这些图像中出现或不出现大面积红斑的原因是观测时间点不同。这并不是自适应光学技术造成的。
使用自适应光学技术之后有了新的发现。在没有使用自适应光学技术的图像中，由于类星体的颜色完全相同，因此被认为是单个类星体。然而，使用自适应光学技术后，两个独立的类星体清晰地显现出来。此外，在这两个类星体之间还出现了一个星系。
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太阳成像
太阳对地球有很大的影响。在我们努力了解地球和太阳之间的因果关系时，对太阳活动加以成像和了解（例如研究太阳黑子和磁场运动生成耀斑的情况）变得越来越重要。为了密切跟踪太阳耀斑的内部结构及其随时间的变化，需要同时达到高分辨率、高速和高动态范围的探测器。
光学/近红外太阳耀斑监测望远镜（又称 ONSET）
ORCA-Flash4.0 V3 数字 CMOS 相机用于太阳观测
由 ONSET 拍摄的太阳耀斑图像
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上层大气成像
上层大气是 80 至 400 km 高处的大气层。该高度对应于地球大气和外太空之间的边界区域。大气的这一部分处于离子化的等离子体状态。由于等离子体与大气之间的相互作用，在南北极产生了极光。这一高度会在夜间产生微弱的大气光。高灵敏度、高分辨率和高速相机可以测量上层大气的动态。
安装在极光天文台的高速相机*
数字 CMOS 相机 ORCA-Flash 4.0 是 Poker Flat Research Range (PFRR) 的高速相机系统中的一部分。
极光成像*
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天文相机应用案例研究
内容包括与天文学家的珍贵访谈以及我们的相机阵容概览
天文学是一个进行各种研究以发现和探索未知天体和天文现象的领域。本手册介绍了此类应用的示例，以及适用于每种应用的相机。
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