IRTF上的MIT光学快速成像系统（MORIS）的第一个结果：冥王星的恒星掩星和系外行星XO-2 b的transit
First results from the MIT Optical Rapid Imaging System (MORIS) on the IRTF: a stellar occultation by Pluto and a transit by exoplanet XO-2b
摘要：
我们介绍了一种高速可见光成像仪：MORIS（MIT光学快速成像系统）。MORIS安装在夏威夷莫纳克亚山的3米红外望远镜设施（IRTF）上。它的主要组件是Andor iXon相机，具有近60 arcsec的平方视场，具有高量子效率，低读取噪声，低暗电流，全帧读出速率范围从所需的慢到最大值3.5 Hz至35 Hz（取决于模式;读取噪声分别为6 e-/像素和49 e-/像素，电子倍增增益=1）。用户可选择的合并和子帧可以将节奏增加到几百Hz。电子倍增模式可以用于光子计数，以牺牲动态范围为代价有效地将读取噪声降低到亚电子水平。使用全球定位系统，数据立方体或单个帧可以被触发到几纳秒的精度。MORIS安装在SpeX的侧面出射窗上（Rayner et al. 2003），允许同时进行近红外和可见光观测。在这里，我们描述的组件，设置和测量的特点MORIS。我们还报告了第一次科学观测的结果：2008年6月24日冥王星的恒星掩星和XO-2b的太阳系外行星凌日。冥王星掩星是一颗R等15.8的恒星，其信噪比为35/大气标度高度，中时误差为0.32 s。XO-2b凌日仪在2分钟内达到0.5毫米级的测光精度，并具有23秒的中间计时精度。
英文摘要：
We present a high-speed, visible-wavelength imaging instrument: MORIS (the MIT Optical Rapid Imaging System). MORIS is mounted on the 3-m Infrared Telescope Facility (IRTF) on Mauna Kea, HI. Its primary component is an Andor iXon camera, a nearly 60 arcsec square field of view with high quantum efficiency, low read noise, low dark current, and full-frame readout rates ranging from as slow as desired to a maximum of between 3.5 Hz and 35 Hz (depending on the mode; read noise of 6e-/pixel and 49 e-/pixel with electron-multiplying gain=1, respectively). User-selectable binning and subframing can increase the cadence to a few hundred Hz. An electron-multiplying mode can be employed for photon counting, effectively reducing the read noise to sub-electron levels at the expense of dynamic range. Data cubes, or individual frames, can be triggered to several nanosecond accuracy using the Global Positioning System. MORIS is mounted on the side-facing exit window of SpeX (Rayner et al. 2003), allowing simultaneous near-infrared and visible observations. Here we describe the components, setup, and measured characteristics of MORIS. We also report results from the first science observations: the 24 June 2008 stellar occultation by Pluto and an extrasolar planetary transit by XO-2b. The Pluto occultation, of a 15.8 R magnitude star, has signal-to-noise ratio of 35 per atmospheric scale height and a midtime error of 0.32 s. The XO-2b transit reaches photometric precision of 0.5 millimagnitudes in 2 minutes and has a midtime timing precision of 23 seconds.
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