行星形成成像仪（PFI）的结构设计研究和技术路线图
Architecture design study and technology roadmap for the Planet Formation Imager (PFI)
摘要：
行星形成成像仪（PFI）项目已经成立了一个技术工作组（TWG），以探索可能的设施架构，以满足PFI的主要科学目标，即在附近的恒星形成区域原位成像行星形成。在太阳系尺度上对尘埃排放敏感和解决形成巨行星周围的希尔球的目标可以通过热红外中的亚毫弧秒成像来最好地实现。利用8-13微米的大气窗口，一个大约有20个孔径（包括10公里基线）的地基长基线干涉仪将具有必要的分辨率，可以对金牛座T金牛座盘的0.1毫角秒（0.014 AU）结构进行成像。即使使用大型望远镜，该阵列也不会具有直接跟踪我们主要目标的中红外条纹的灵敏度，并且需要近红外条纹跟踪系统。虽然使用现代中红外激光梳技术的外差架构仍然是一个有竞争力的选择（特别是对于有趣的24和40μm大气窗口），但PFI科学工作组（SWG）对CO/H2O振动水平的3-5μm观测的优先级推动了TWG需要使用潜在冷却光学器件的真空管道光束传输。我们在这里提出了一个模拟的L-和N-波段PFI观测的一个现实的4行星盘模拟的初步研究，发现21 × 2.5米PFI可以很容易地发现吸积原行星在L和N-波段，但只能看到非吸积行星在L波段。（摘要见PDF）
英文摘要：
The Planet Formation Imager (PFI) Project has formed a Technical Working Group (TWG) to explore possible facility architectures to meet the primary PFI science goal of imaging planet formation in situ in nearby star- forming regions. The goals of being sensitive to dust emission on solar system scales and resolving the Hill-sphere around forming giant planets can best be accomplished through sub-milliarcsecond imaging in the thermal infrared. Exploiting the 8-13 micron atmospheric window, a ground-based long-baseline interferometer with approximately 20 apertures including 10km baselines will have the necessary resolution to image structure down 0.1 milliarcseconds (0.014 AU) for T Tauri disks in Taurus. Even with large telescopes, this array will not have the sensitivity to directly track fringes in the mid-infrared for our prime targets and a fringe tracking system will be necessary in the near-infrared. While a heterodyne architecture using modern mid-IR laser comb technology remains a competitive option (especially for the intriguing 24 and 40μm atmospheric windows), the prioritization of 3-5μm observations of CO/H2O vibrotational levels by the PFI-Science Working Group (SWG) pushes the TWG to require vacuum pipe beam transport with potentially cooled optics. We present here a preliminary study of simulated L- and N-band PFI observations of a realistic 4-planet disk simulation, finding 21x2.5m PFI can easily detect the accreting protoplanets in both L and N-band but can see non-accreting planets only in L band. (abridged -- see PDF for full abstract)
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