A review of simulation and performance modeling for the Roman coronagraph instrument
Ewan S. Douglas, Jaren N. Ashcraft, Ruslan Belikov, John Debes, Jeremy Kasdin, John Krist, Brianna I. Lacy, Bijan Nemati, Kian Milani, Leonid Pogorelyuk, A. J. … 展开作者
Ewan S. Douglas, Jaren N. Ashcraft, Ruslan Belikov, John Debes, Jeremy Kasdin, John Krist, Brianna I. Lacy, Bijan Nemati, Kian Milani, Leonid Pogorelyuk, A. J. Eldorado Riggs, Dmitry Savransky, Dan Sirbu
备注：
11 pages, 5 figures
发表信息：
Proc SPIE Volume 11443, Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave
The Nancy Grace Roman Space Telescope Coronagraph Instrument (CGI) will be capable of characterizing exoplanets in reflected light and will demonstrate space technologies essential for future missions to take spectra of Earthlike exoplanets. As the mission and instrument move into the final stages of design, simulation tools spanning from depth of search calculators to detailed diffraction models have been created by a variety of teams. We summarize these efforts, with a particular focus on publicly available datasets and software tools. These include speckle and point-spread-function models, signal-to-noise calculators, and science product simulations (e.g. predicted observations of debris disks and exoplanet spectra). This review is intended to serve as a reference to facilitate engagement with the technical and science capabilities of the CGI instrument.
The Roman Coronagraph Community Participation Program: corgisim - a simulation suite for the Nancy Grace Roman Space Telescope Coronagraph Instrument
University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Aix Marseille Université（艾克斯-马赛大学）；Northwestern University（西北大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；DM Telescopes LLC（DM望远镜有限责任公司）；University of Alabama at Huntsville（阿拉巴马大学亨茨维尔分校）；National Astronomical Observatory of Japan（日本国立天文台）；Space Telescope Science Institute（空间望远镜科学研究所）；California Institute of Technology（加州理工学院）
The Roman Coronagraph Community Participation Program: data reduction pipeline astrometric calibration
Northwestern University（西北大学）；Center for Interdisciplinary Exploration and Research in Astrophysics（天体物理跨学科探索与研究中心）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；University of California Santa Barbara（加州大学圣塔芭芭拉分校）；Space Telescope Science Institute（太空望远镜科学研究所）
The Roman coronagraph instrument will demonstrate high-contrast imaging technology, enabling the imaging of faint debris disks, the discovery of inner dust belts, and planets. Polarization studies of debris disks provide information on dust grains' size, shape, and distribution. The Roman coronagraph uses a polarization module comprising two Wollaston prism assemblies to produce four orthogonally polarized images ($I_{0}$, $I_{90}$, $I_{45}$, and $I_{135}$), each measuring 3.2 arcsecs in diameter and separated by 7.5 arcsecs in the sky. The expected RMS error in the linear polarization fractio…
A Roman Coronagraph Spectroscopic Mode Demonstration
University of Texas-San Antonio（德克萨斯大学圣安东尼奥分校）；Subaru Telescope, National Astronomical Observatory of Japan（昴望远镜，日本国立天文台）；University of California-Santa Cruz（加州大学圣克鲁兹分校）；University of Michigan（密歇根大学）；NASA Goddard Spaceflight Center（美国宇航局戈达德太空飞行中心）；National Astronomical Observatory of Japan（日本国立天文台）
Exozodiacal dust, warm debris from comets and asteroids in and near the habitable zone of stellar systems, reveals the physical processes that shape planetary systems. Scattered light from this dust is also a source of background flux which must be overcome by future missions to image Earthlike planets. This study quantifies the sensitivity of the Nancy Grace Roman Space Telescope Coronagraph to light scattered by exozodi, the zodiacal dust around other stars. Using a sample of 149 nearby stars, previously selected for optimum detection of habitable exoplanets by space observatories, we find t…
Technology and Science Advancing Observations with Roman Coronagraph Informed by Ground-Based High-Contrast Imaging
University of Texas at San Antonio（德克萨斯大学圣安东尼奥分校）；National Astronomical Observatory of Japan（日本国立天文台）；NASA Ames Research Center（美国国家航空航天局艾姆斯研究中心）；Astrobiology Center（天体生物学中心）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；College of Optical Sciences, University of Arizona（亚利桑那大学光学科学学院）
CoronaGraph Instrument Reference stars for Exoplanets (CorGI-REx) I. Preliminary Vetting and Implications for the Roman Coronagraph and Habitable Worlds Observatory
The Roman Coronagraph Community Participation Program: Observation planning and data reduction for polarimetric mode
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；National Astronomical Observatory of Japan, NINS（日本国立天文台）；Astrobiology Center, NINS（天体生物学中心）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学）；Sibley School of Mechanical and Aerospace Engineering, Cornell University（康奈尔大学）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Caltech（加州理工学院）；The Graduate Univ. for Advanced Studies（综合研究大学院大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Jet Propulsion Laboratory, California Institute of Technology（喷气推进实验室）；DM Telescopes LLC（DM望远镜有限责任公司）；Department of Astronomy, Graduate School of Science, The University of Tokyo（东京大学）；Northwestern University（西北大学）；Tellus1 Scientific, LLC（Tellus1科学有限公司）
Jointly Modeling Roman Coronagraph Astrometry and Photometry Improves Orbital Parameter Estimates
Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University（西北大学跨学科天体物理探索与研究中心）；Department of Physics and Engineering, University of St. Thomas（圣托马斯大学物理与工程系）；Department of Astronomy and Astrophysics, University of California, Santa Cruz（加州大学圣克鲁斯分校天文与天体物理系）
The Roman Coronagraph Community Participation Program: calibration strategy for the Mueller matrix using on-sky sources
Astrobiology Center（天体生物学中心）；National Astronomical Observatory of Japan（日本国立天文台）；Steward Observatory and the Department of Astronomy, The University of Arizona（亚利桑那大学斯特沃德天文台及天文学系）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Hiroshima Astrophysical Science Center, Hiroshima University（广岛大学广岛天体物理科学中心）；Department of Astronomy, Graduate School of Science, The University of Tokyo（东京大学理学研究科天文学系）；Northwestern University（西北大学）；Center for Interdisciplinary Exploration and Research in Astrophysics（天体物理学跨学科探索与研究中心）；Tellus1 Scientific, LLC（Tellus1科学有限责任公司）；Department of Astronomical Science, The Graduate University for Advanced Studies, SOKENDAI（综合研究大学院大学天文学科学研究科）
The Roman Coronagraph Community Participation Program: pre-launch reference star list and impact of reference star properties on post-processing performance
Steward Observatory and Department of Astronomy, University of Arizona（亚利桑那大学天文台与天文学系）；DM Telescopes LLC（DM望远镜有限责任公司）；NASA Jet Propulsion Laboratory, California Institute of Technology（加州理工学院NASA喷气推进实验室）；Institute for Astronomy, University of Edinburgh, Royal Observatory（爱丁堡大学天文研究所皇家天文台）；Centre for Exoplanet Science , University of Edinburgh（爱丁堡大学系外行星科学中心）；Université Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学、法国国家科学研究中心、IPAG）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Department of Physics and Astronomy, University of Notre Dame（圣母大学物理与天文学系）；NASA Exoplanet Science Institute, IPAC, California Institute of Technology（加州理工学院NASA系外行星科学研究所IPAC）；European Southern Observatory（欧洲南方天文台）；Bay Area Environmental Research Institute（湾区环境研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Wyant College of Optical Sciences, The University of Arizona（亚利桑那大学怀特光学科学学院）；Subaru Telescope, National Observatory of Japan, National Institutes of Natural Sciences（日本国立自然科学院日本国立天文台昴星团望远镜）；Astrobiology Center of NINS（日本国立自然科学院天体生物学中心）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Northrop Grumman Corporation（诺斯罗普·格鲁曼公司）；NASA Ames Research Center（NASA艾姆斯研究中心）；National Astronomical Observator（国家天文观测所）
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）
Exoplanetary science is a very active field of astronomy nowadays, with questions still opened such as how planetary systems form and evolve (occurrence, process), why such a diversity of exoplanets is observed (mass, radius, orbital parameters, temperature, composition), and what are the interactions between planets, circumstellar disk and their host star. Several complementary methods are used for the detection of exoplanets. Among these, imaging aims at the direct detection of the light reflected, scattered or emitted by exoplanets and circumstellar disks. This allows their spectral and pol…
Operating in an unprecedented contrast regime ($10^{-7}$ to $10^{-9}$), the Roman Coronagraph Instrument (CGI) will serve as a pathfinder for key technologies needed for future Earth-finding missions. The Roman Exoplanet Imaging Data Challenge (Roman EIDC) was a community engagement effort that tasked participants with extracting exoplanets and their orbits for a 47 UMa-like target star, given: (1) 15 years of simulated precursor radial velocity (RV) data, and (2) six epochs of simulated imaging taken over the course of the Roman mission. The Roman EIDC simulated images include 4 epochs with C…
We present a new instrument, the "Stellar Double Coronagraph" (SDC), a flexible coronagraphic platform. Designed for Palomar Observatory's 200" Hale telescope, its two focal and pupil planes allow for a number of different observing configurations, including multiple vortex coronagraphs in series for improved contrast at small angles. We describe the motivation, design, observing modes, wavefront control approaches, data reduction pipeline, and early science results. We also discuss future directions for the instrument.
The coronagraphic instrument currently proposed for the WFIRST-AFTA mission will be the first example of a space-based coronagraph optimized for extremely high contrasts that are required for the direct imaging of exoplanets reflecting the light of their host star. While the design of this instrument is still in progress, this early stage of development is a particularly beneficial time to consider the operation of such an instrument. In this paper, we review current or planned operations on the Hubble Space Telescope (HST) and the James Webb Space Telescope (JWST) with a focus on which operat…
The Gemini Planet Imager (GPI) is a next-generation, facility instrument currently being commissioned at the Gemini South observatory. GPI combines an extreme adaptive optics system and integral field spectrograph (IFS) with an apodized-pupil Lyot coronagraph (APLC) producing an unprecedented capability for directly imaging and spectroscopically characterizing extrasolar planets. GPI's operating goal of $10^{-7}$ contrast requires very precise alignments between the various elements of the coronagraph (two pupil masks and one focal plane mask) and active control of the beam path throughout the…
An Updated Model for Epsilon Eridani b and Prospects for Imaging with the Roman Coronagraph
Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；University of Victoria（维多利亚大学）；NRC Herzberg Astronomy and Astrophysics（加拿大国家研究委员会赫兹伯格天文与天体物理研究所）；University of Texas at Austin（德克萨斯大学奥斯汀分校）；California Institute of Technology（加州理工学院）；Cornell University（康奈尔大学）；Space Telescope Science Institute（太空望远镜科学研究所）
The World Space Observatory for Ultraviolet (WSO-UV) is an orbital optical telescope with a 1.7 m-diameter primary mirror currently under development. The WSO-UV is aimed to operate in the 115-310 nm UV spectral range. Its two major science instruments are UV spectrographs and a UV imaging field camera with filter wheels. The WSO-UV project is currently in the implementation phase, with a tentative launch date in 2023. Recently, two additional instruments devoted to exoplanets have been proposed for WSO-UV, which are the focus of this paper. UVSPEX, a UV-Spectrograph for Exoplanets, aims to de…
Despite promising astrometric signals, to date there has been no success in direct imaging of a hypothesized third member of the Sirius system. Using the Clio instrument and MagAO adaptive optics system on the Magellan Clay 6.5 m telescope, we have obtained extensive imagery of Sirius through a vector apodizing phase plate (vAPP) coronagraph in a narrowband filter at 3.9 microns. The vAPP coronagraph and MagAO allow us to be sensitive to planets much less massive than the limits set by previous non-detections. However, analysis of these data presents challenges due to the target's brightness a…
Directly imaging Earth-like exoplanets (``exoEarths'') with a coronagraph instrument on a space telescope requires a stable wavefront with optical path differences limited to tens of picometers RMS during exposure times of a few hours. While the structural dynamics of a segmented mirror can be directly stabilized with telescope metrology, another possibility is to use a closed-loop wavefront sensing and control system in the coronagraph instrument that operates during the science exposures to actively correct the wavefront and relax the constraints on the stability of the telescope. In this pa…
We present a MIR coronagraph to target the direct observation of extrasolar planets for SPICA, in which a coronagraph is currently regarded as an option of the focal plane instruments. The primary target of the SPICA coronagraph is the direct observation of Jovian exo-planets. A strategy of the baseline survey and the specifications for the coronagraph instrument for the survey are introduced together. The main wavelengths and the contrast required for the observations are 3.5-27um, and 10^{-6}, respectively.Laboratory experiments were performed with a visible laser to demonstrate the principl…
The SPICA coronagraph instrument (SCI) provides high-contrast imaging and moderate resolution (R < 200) spectroscopy at the wavelength range from 3.5 to 27 μm. Based on the planet evolutional model calculated by Burrows et al. (2003), SCI will search for gas giant planets down to one Jupiter mass around nearby young (1 Gyr) stars and two Jupiter masses around nearby old (5 Gyr) stars. SCI also allows to characterizing those planets of less than 1 Gyr by spectroscopic observations to reveal the nature of planetary formation and evolution. Focusing on the high sensitivity and high contrast at wa…
The Astro2020 decadal survey recommended an infrared, optical, ultra-violet (IR/O/UV) telescope with a $\sim$6~m inscribed diameter and equipped with a coronagraph instrument to directly image exoEarths in the habitable zone of their host star. A telescope of such size may need to be segmented to be folded and then carried by current launch vehicles. However, a segmented primary mirror introduces the potential for additional mid spatial frequency optical wavefront instabilities during the science operations that would degrade the coronagraph performance. A coronagraph instrument with a wavefro…
Reflected starlight measurements will open a new path in the characterization of directly imaged exoplanets. However, we still lack a population study of known targets amenable to this technique. Here, we investigate which of the about 4300 exoplanets confirmed to date are accessible to the Roman Space Telescope's coronagraph (CGI) in reflected starlight at reference wavelengths $λ$=575, 730 and 825 nm. We carry out a population study and also address the prospects for phase-curve measurements. We used the NASA Exoplanet Archive as a reference for planet and star properties, and explored the i…
Several concepts now exist for small, space-based missions to directly characterize exoplanets in reflected light. Here, we develop an instrument noise model suitable for studying the spectral characterization potential of a coronagraph-equipped, space-based telescope. We adopt a baseline set of telescope and instrument parameters appropriate for near-future planned missions like WFIRST-AFTA, including a 2 m diameter primary aperture, an operational wavelength range of 0.4-1.0 um, and an instrument spectral resolution of 70, and apply our baseline model to a variety of spectral models of diffe…
The Wide Field Infrared Survey Telescope (WFIRST) Coronagraph Instrument (CGI) will be the first high-performance stellar coronagraph using active wavefront control for deep starlight suppression in space, providing unprecedented levels of contrast, spatial resolution, and sensitivity for astronomical observations in the optical. One science case enabled by the CGI will be taking images and(R~50)spectra of faint interplanetary dust structures present in the habitable zone of nearby sunlike stars (~10 pc) and within the snow-line of more distant ones(~20pc), down to dust density levels commensu…
