Adaptive Optics at Optical Wavelengths: Test Observations of Kyoto 3DII Connected to Subaru Telescope AO188
Adaptive Optics at Optical Wavelengths: Test Observations of Kyoto 3DII Connected to Subaru Telescope AO188
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光波长的自适应光学：京都 3DII 连接到斯巴鲁望远镜 AO188 的测试观测
DOI：
10.1088/1538-3873/128/967/095003
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
N.
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文献类型：
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作者：
Matsubayashi;K.; Sugai;H.; Shimono;A.; Akita;A.; Hattori;T.; Hayano;Y.; Minowa;Y.; Takeyama;N.
自适应光学（AO）使我们能够以高空间分辨率观察物体，这在大多数天体物理观测中非常重要。大多数AO系统在近红外波长下工作，但不在光学范围内，因为光学观测需要更高的性能才能获得与近红外观测相同的Strehl比。因此，为了实现光学波长的AO辅助观测，我们将可以执行积分场光谱的京都三维光谱仪II（京都3DII）连接到斯巴鲁望远镜（AO 188）的第二代AO系统。我们开发了一种新的分束器，用于AO 188波前传感器，反射594 nm以下的光，并用于京都3DII透射644 nm以上的光。我们还在斯巴鲁望远镜的Nasmyth焦点上开发了一个京都3DII支架。在测试观测中，组合AO 188-京都3DII的空间分辨率高于自然视宁度条件下的空间分辨率，即使在6500流明。欠采样（1.5 spaxels）的亮导星星（V波段7.0等）的半高全宽为0 farcs 12。
Adaptive optics (AO) enables us to observe objects with high spatial resolution, which is important in most astrophysical observations. Most AO systems are operational at near-infrared wavelengths but not in the optical range, because optical observations require a much higher performance to obtain the same Strehl ratio as near-infrared observations. Therefore, to enable AO-assisted observations at optical wavelengths, we connected the Kyoto Tridimensional Spectrograph II (Kyoto 3DII), which can perform integral field spectroscopy, to the second generation AO system of the Subaru Telescope (AO188). We developed a new beam-splitter that reflects light below 594 nm for the wavefront sensors of AO188 and transmits above 644 nm for Kyoto 3DII. We also developed a Kyoto 3DII mount at the Nasmyth focus of the Subaru Telescope. In test observations, the spatial resolution of the combined AO188–Kyoto 3DII was higher than that in natural seeing conditions, even at 6500 Å. The full width at half maximum of an undersampled (1.5 spaxels) bright guide star (7.0 mag in the V-band) was 0 farcs 12.