用极端自适应光学和光子学增强恒星spectroscopy
Enhancing stellar spectroscopy with extreme adaptive optics and photonics
摘要：
极端自适应光学系统现在在全球范围内运行。这些系统能够进行高阶波前校正，在近红外区域提供90%的Strehl比率。这些系统最初是为了直接成像系外行星，通常配备有先进的日冕仪，抑制轴上的恒星，干涉仪校准波前误差，低阶波前传感器，以稳定任何倾斜/倾斜残差到前所未有的程度。这样的系统是很好的定位，以促进详细的光谱特征微弱的亚恒星同伴在小角度分离的主恒星。此外，点扩散函数增加的光浓度和前所未有的稳定性也在天文学的其他领域创造了机会，包括光谱学。利用这样的Strehl比率，有效地注入到单模光纤或光子灯笼中成为可能。通过衍射限制元件馈入仪器，校准光谱仪的线轮廓变得相当容易，因为模式噪声或光纤输出的不完美干扰不再是问题。它还开辟了利用光子技术的先进功能，固有的可复制性和小，重量轻的足迹来设计和构建未来仪器的可能性。在这项工作中，我们概述了如何极端的自适应光学系统将使先进的光子和衍射限制技术被利用在光谱仪的设计和它将对光谱的影响。我们说明，基于这些技术的仪器的精度，将受到限制的光谱内容和恒星噪声的冷恒星，并能够实现几个m/s的径向速度精度;所需的水平检测外地球附近的M-矮星的HZ。
英文摘要：
Extreme adaptive optics systems are now in operation across the globe. These systems, capable of high order wavefront correction, deliver Strehl ratios of 90% in the near-infrared. Originally intended for the direct imaging of exoplanets, these systems are often equipped with advanced coronagraphs that suppress the on-axis-star, interferometers to calibrate wavefront errors, and low order wavefront sensors to stabilize any tip/tilt residuals to a degree never seen before. Such systems are well positioned to facilitate the detailed spectroscopic characterization of faint substellar companions at small angular separations from the host star. Additionally, the increased light concentration of the point-spread function and the unprecedented stability create opportunities in other fields of astronomy as well, including spectroscopy. With such Strehl ratios, efficient injection into single-mode fibers or photonic lanterns becomes possible. With diffraction-limited components feeding the instrument, calibrating a spectrograph's line profile becomes considerably easier, as modal noise or imperfect scrambling of the fiber output are no longer an issue. It also opens up the possibility of exploiting photonic technologies for their advanced functionalities, inherent replicability, and small, lightweight footprint to design and build future instrumentation. In this work, we outline how extreme adaptive optics systems will enable advanced photonic and diffraction-limited technologies to be exploited in spectrograph design and the impact it will have on spectroscopy. We illustrate that the precision of an instrument based on these technologies, would be limited by the spectral content and stellar noise on cool stars and capable of achieving a radial velocity precision of several m/s; the level required for detecting an exo-Earth in the HZ of a nearby M-dwarf.
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