One important frontier for astronomical adaptive optics (AO) involves methods such as Multi-Object AO and Multi-Conjugate AO that have the potential to give a significantly larger field of view than conventional AO techniques. A second key emphasis over the next decade will be to push astronomical AO to visible wavelengths. We have conducted the first laboratory simulations of wide-field, laser guide star adaptive optics at visible wavelengths on a 10-meter-class telescope. These experiments, utilizing the UCO/Lick Observatory's Multi-Object / Laser Tomography Adaptive Optics (MOAO/LTAO) testbed, demonstrate new techniques in wavefront sensing and control that are crucial to future on-sky MOAO systems. We (1) test and confirm the feasibility of highly accurate atmospheric tomography with laser guide stars, (2) demonstrate key innovations allowing open-loop operation of Shack-Hartmann wavefront sensors (with errors of ~30 nm) as will be needed for MOAO, and (3) build a complete error budget model describing system performance. The AO system maintains a performance of 32.4% Strehl on-axis, with 24.5% and 22.6% at 10" and 15", respectively, at a science wavelength of 710 nm (R-band) over the equivalent of 0.8 seconds of simulation. The MOAO-corrected field of view is ~25 times larger in area than that limited by anisoplanatism at R-band. Our error budget is composed of terms verified through independent, empirical experiments. Error terms arising from calibration inaccuracies and optical drift are comparable in magnitude to traditional terms like fitting error and tomographic error. This makes a strong case for implementing additional calibration facilities in future AO systems, including accelerometers on powered optics, 3D turbulators, telescope and LGS simulators, and external calibration ports for deformable mirrors.
Spectroscopy using a visible photonic lantern at the Subaru telescope: Laboratory characterization and first on-sky demonstration on Ikiiki (α Leo) and `Aua (α Ori)
Visible absorptions of potential diffuse ISM hydrocarbons: C$_9$H$_9$ and C$_9$H$_5$ radicals
本文报道了在碳氢化合物放电源的超声膨胀中，实验室检测到了以前未观察到的共振稳定的C $_9$ H $_5$和C $_9$ H $_9$自由基。这些基团被暂时指定为乙炔基取代的N-C $_9$ H $_5$和乙烯基取代的苄基C $_9$ H $_9$。它们的特征是可见光吸收带，与一些非常弱的扩散星际带一致，朝向HD 183143和HD 204827。
PALM-3000: Exoplanet Adaptive Optics for the 5-meter Hale Telescope
我们描述和报告的第一个结果从PALM-3000，第二代天文自适应光学设施的5.1米海尔望远镜在帕洛玛天文台。PALM-3000被设计用于在明亮恒星周围的近红外波段对棕矮星和大型行星质量体进行高对比度成像和发射光谱分析，但也支持V ~ 17的一般自然导星使用。PALM-3000使用其独特的66 x 66致动器可变形反射镜，迄今已证明在1角秒视宁度条件下残余波前误差为141 nm RMS。PALM-3000可以在2.2微米的观察波长下在6.4 x 6.4弧秒的工作区域上提供相位共轭校正，或者在大约一半的该场上提供全电场（幅度和相位）校正。通过优化的后端仪器，PALM-3000在经过观察后散斑抑制处理后，能够在约1角秒的角间距下实现高达10 e-7的对比度。在对自适应光学系统进行优化的同时，我们已经成功地委托了五台后端科学仪器，并与美国自然历史博物馆和喷气推进实验室的合作伙伴一起开始了一项重大的系外行星特征调查，即1640项目。
3.5-meter Segmented-Mirror Robotic Space Telescope Mission White Paper IV. Key Scientific Mission: Solar-System Small Bodies and Planetary Defense
Korea Institute for Advanced Study（韩国高等研究院）；Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究所）；University of Ulsan（蔚山科学技术院）；University of Science and Technology（科学技术联合大学院大学）；Kyungpook National University（庆北国立大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Pusan National University（釜山国立大学）；Korea National University of Education（韩国国立教育大学）；Seoul National University（首尔国立大学）；Yonsei University（延世大学）
Performance Simulations for Kola: Achieving High-Resolution, Visible-Light AO Correction Over a 1 Arcminute Field
University of California, Berkeley（加州大学伯克利分校）；California Institute of Technology（加州理工学院）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；University of Hawai‘i at Mānoa（夏威夷大学马诺阿分校）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
