发表机构
Université Côte d’Azur, Observatoire de la Côte d’Azur; OGS Technologies（蔚蓝海岸大学，蔚蓝海岸天文台; OGS科技公司）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
CHARA阵列的SPICA设备套件含可见光光谱仪与近红外 fringe 跟踪器，实现0.2毫角秒高分辨率可见光成像，已投入运行，仍需优化灵敏度与高分辨率性能。
AI 中文摘要
名为“利用共相阵列进行恒星参数与成像（SPICA）”的设备套件，在位于加利福尼亚州威尔逊山的CHARA阵列焦点处安装了两台干涉仪设备。SPICA由SPICA-VIS和SPICA-FT组成：SPICA-VIS是一款光纤馈送的六光束可见光光谱仪，具备三种光谱分辨率；SPICA-FT是一款六光束近红外 fringe 跟踪器，用于 fringe 的快速稳定。SPICA正开启可见光域成像的应用，其角分辨率可达前所未有的0.2毫角秒。该设备围绕赫茨普龙-罗素图上恒星基本参数的大规模巡天而设计，旨在理解恒星物理标准经验关系随活动产生的偏差，包括临边昏暗、多星系统、自转、星风及周边环境。SPICA采用了可见光波段的电子倍增探测器和近红外波段的电子雪崩光电二极管阵列等先进技术，还得益于该阵列一米望远镜上新启用的自适应光学系统。可见光设备SPICA-VIS的模块优化了单模光纤的光注入，用于空间滤波后再在像面进行色散。 fringe 跟踪器SPICA-FT在H波段对六束光进行群延迟和相位延迟跟踪，可采用一体化或ABCD编码方式处理 fringe 信号。SPICA已实现天空观测运行，在低光谱分辨率模式下，尤其针对恒星参数干涉巡天（ISSP），其性能接近预期水平；但在灵敏度方面达到最终性能、支持更高光谱分辨率运行仍需进一步工作。
英文摘要
The suite called Stellar Parameters and Images with a Cophased Array (SPICA) has two interferometric instruments installed at the focus of the CHARA Array located at Mount Wilson, CA. SPICA is made of SPICA-VIS, a fiber-fed six-beam visible spectrograph with three spectral resolutions, and SPICA-FT, a six-beam near-infrared fringe tracker for the fast stabilization of the fringes. SPICA is opening access to imaging in the visible domain with an unprecedented angular resolution down to 0.2 milliarcseconds. It has been designed around a large survey of fundamental parameters of stars over the Hertzsprung- Russell diagram, aiming at understanding the deviations from the standard empirical relations of stellar physics as a function of activity: limb darkening, multiplicity, rotation, winds, and environments. SPICA makes use of the advanced technologies in electron multiplying detectors in the visible and electron- avalanche photodiode arrays in the near-infrared. It benefits from the newly commissioned adaptive optics on the one-meter telescopes of the array. The modules of the visible instrument, SPICA-VIS, optimize the injection of light into single-mode fibers for spatial filtering before spectral dispersion in the image plane. The fringe tracker, SPICA-FT, performs group-delay and phase-delay tracking for six beams in the H band. SPICA-FT can use an all-in-one or ABCD encoding of the fringe signals. SPICA is operational on sky and is close to reaching the expected performance in low spectral resolution, in particular, for the Interferometric Survey of Stellar Parameters (ISSP). More work is still needed to achieve the ultimate performance in terms of sensitivity and to allow operations with higher spectral resolutions.
