The Gemini Planet Imager
The Gemini Planet Imager
复制标题
双子座行星成像仪
DOI：
10.1117/12.672430
复制
发表时间：
2006
影响因子：
7.7
通讯作者：
J. Véran
中科院分区：
文献类型：
--
作者：
B. Macintosh;J. Graham;D. Palmer;R. Doyon;D. Gavel;J. Larkin;B. Oppenheimer;L. Saddlemyer;J. K. Wallace;B. Bauman;J. Evans;Darren Erikson;K. Morzinski;D. Phillion;L. Poyneer;A. Sivaramakrishnan;R. Soummer;S. Thibault;J. Véran
太阳系外行星研究的下一个主要前沿是行星本身的直接成像检测。凭借高阶自适应光学、精心的系统设计和先进的日冕学，8米级望远镜上的AO系统可以实现10-7至10-8的对比度水平，足以探测太阳附近温暖的自发光木星行星。这种直接探测对于当前径向速度勘测无法到达的行星非常敏感，并且可以对行星进行光谱表征，从而为行星形成和其他太阳系的结构提供线索。我们已经开始为双子座天文台建造这样的系统。该仪器被称为双子座行星成像仪 (GPI)，将于 2010 年部署在双子座南望远镜上。它结合了基于 MEMS 的 2000 个执行器的 AO 系统、变迹光瞳 Lyot 日冕仪、用于纳米级实时波前校准的精密红外干涉仪以及用于目标行星检测和表征的红外积分场摄谱仪。 GPI 将能够在 1.65 微米处实现 > 0.9 的斯特列尔比，并观察 I 波段星等小于 8 的大量科学目标。除了行星探测之外，GPI 还将能够对星周尘埃盘进行偏振成像、研究演化恒星以及对明亮目标进行高斯特列尔成像光谱。我们在此介绍 GPI 仪器设计的概述、强调关键技术挑战的误差预算以及系统性能模型。
The next major frontier in the study of extrasolar planets is direct imaging detection of the planets themselves. With high-order adaptive optics, careful system design, and advanced coronagraphy, it is possible for an AO system on a 8-m class telescope to achieve contrast levels of 10-7 to 10-8, sufficient to detect warm self-luminous Jovian planets in the solar neighborhood. Such direct detection is sensitive to planets inaccessible to current radial-velocity surveys and allows spectral characterization of the planets, shedding light on planet formation and the structure of other solar systems. We have begun the construction of such a system for the Gemini Observatory. Dubbed the Gemini Planet Imager (GPI), this instrument should be deployed in 2010 on the Gemini South telescope. It combines a 2000-actuator MEMS-based AO system, an apodized-pupil Lyot coronagraph, a precision infrared interferometer for real-time wavefront calibration at the nanometer level, and a infrared integral field spectrograph for detection and characterization of the target planets. GPI will be able to achieve Strehl ratios > 0.9 at 1.65 microns and to observe a broad sample of science targets with I band magnitudes less than 8. In addition to planet detection, GPI will also be capable of polarimetric imaging of circumstellar dust disks, studies of evolved stars, and high-Strehl imaging spectroscopy of bright targets. We present here an overview of the GPI instrument design, an error budget highlighting key technological challenges, and models of the system performance.