Laboratory Demonstration of Spatial Linear Dark Field Control For Imaging Extrasolar Planets in Reflected Light
Thayne Currie, Eugene Pluzhnik, Olivier Guyon, Ruslan Belikov, Kelsey Miller, Steven Bos, Jared Males, Dan Sirbu, Charlotte Bond, Richard Frazin, Tyler Groff, B… 展开作者
Thayne Currie, Eugene Pluzhnik, Olivier Guyon, Ruslan Belikov, Kelsey Miller, Steven Bos, Jared Males, Dan Sirbu, Charlotte Bond, Richard Frazin, Tyler Groff, Brian Kern, Julien Lozi, Benjamin Mazin, Bijan Nemati, Barnaby Norris, Hari Subedi, Scott Will
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13 pages, 7 figures, accepted for publication in Publications of the Astronomical Society of the Pacific
Imaging planets in reflected light, a key focus of future NASA missions and ELTs, requires advanced wavefront control to maintain a deep, temporally correlated null of stellar halo -- i.e. a dark hole -- at just several diffraction beam widths. Using the Ames Coronagraph Experiment testbed, we present the first laboratory tests of Spatial Linear Dark Field Control (LDFC) approaching raw contrasts ($\sim$ 5$\times$10$^{-7}$) and separations (1.5--5.2 $λ$/D) needed to image jovian planets around Sun-like stars with space-borne coronagraphs like WFIRST-CGI and image exo-Earths around low-mass stars with future ground-based 30m class telescopes. In four separate experiments and for a range of different perturbations, LDFC largely restores (to within a factor of 1.2--1.7) and maintains a dark hole whose contrast is degraded by phase errors by an order of magnitude. Our implementation of classical speckle nulling requires a factor of 2--5 more iterations and 20--50 DM commands to reach contrasts obtained by spatial LDFC. Our results provide a promising path forward to maintaining dark holes without relying on DM probing and in the low-flux regime, which may improve the duty cycle of high-contrast imaging instruments, increase the temporal correlation of speckles, and thus enhance our ability to image true solar system analogues in the next two decades.
Laboratory demonstration of low order wavefront control using light reflected off the vortex coronagraph
California Institute of Technology（加州理工学院）；Jet Propulsion Laboratory, California Institute of Technology（喷气推进实验室，加州理工学院）；Trinity College Dublin, the University of Dublin（都柏林三一学院，都柏林大学）
Developing Atmospheric Retrieval Methods for Direct Imaging Spectroscopy of Gas Giants in Reflected Light I: Methane Abundances and Basic Cloud Properties
The final design of GMagAO-X: high-contrast imaging at first-light of the GMT
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Leiden Observatory, Leiden University, The Netherlands（莱顿大学莱顿天文台）；James C. Wyant College of Optical Sciences, University of Arizona, USA（亚利桑那大学詹姆斯·C·怀恩特光学科学学院）；Boston Micromachines Corporation, USA（波士顿微机器公司）；Subaru Telescope, National Astronomical Observatory of Japan（日本国立天文台昴星团望远镜）；Astrobiology Center, National Institutes of Natural Sciences, Japan（日本国立自然科学研究所天体生物学中心）
Magellan Adaptive Optics first-light observations of the exoplanet beta Pic b. II. 3-5 micron direct imaging with MagAO+Clio, and the empirical bolometric luminosity of a self-luminous giant planet
The Roman Coronagraph Community Participation Program: early calibration plan and pilot observation of a companion
Space Telescope Science Institute（太空望远镜科学研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；California Institute of Technology（加州理工学院）；University of California, Santa Barbara（加州大学圣巴巴拉分校）；Tellus1 Scientific, LLC（Tellus1科学有限责任公司）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学、法国国家科学研究中心、法国国家空间研究中心、天体物理与行星学实验室）；Northwestern University（西北大学）；DM Telescopes LLC（DM望远镜有限责任公司）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Astrobiology Center of NINS（日本国立自然科学研究所天体生物学中心）；National Astronomical Observatory of Japan（日本国立天文台）；The University of Alabama in Huntsville（阿拉巴马大学亨茨维尔分校）；Johns Hopkins University（约翰斯·霍普金斯大学）；NASA Ames Research Center（美国宇航局艾姆斯研究中心）；University of Edinburgh（爱丁堡大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
