학술논문
Wide Field Infrared Survey Telescope (WFIRST) Observatory Overview
Document Type
Report
Author
Casey, T; Armani, N; Alexander, W; Bartusek, L; Blaurock, C; Braun, D; Carra, A; Content, D; Conturie, Y; Cottingham, C; Demers, R; Dipirro, M; Effinger, R; Egerman, R; Forkl, F; Gao, G; Godo, S; Gygax, J; Hagopian, J; Hahm, T; Hawk, J; Hobbs, G; Jackson, C; Jurling, A; Kern, B; Kruk, J; Li, X; Liu, A; Marx, C; Marzouk, M; McDonald, C; Melton, M; Mondello, J; Noecker, C; Pasquale, B; Peabody, H; Poberezhskiy, I; Powell, C; Rosanova, G; Ruffa, J; Smith, J; Tang, H; Tolman, C; Whipple, A; Wilson, T; Vess, M; Voyer, P
Source
Subject
Language
English
Abstract
NASA's Wide Field Infrared Survey Telescope (WFIRST) is being designed to deliver unprecedented capability in dark energy and exoplanet science, and to host a technology demonstration coronagraph for exoplanet imaging and spectroscopy. The observatory design has matured since 2013; we present a comprehensive description of the observatory configuration as refined during the WFIRST Phase-A study. The observatory is based on an existing, repurposed 2.4 meter space telescope coupled with a 288 megapixel near-infrared (0.6 to 2 microns) HgCdTe focal plane array with multiple imaging and spectrographic modes. Together they deliver a 0.28 square degree field of view, which is approximately 100 times larger than the Hubble Space Telescope, and a sensitivity that enables rapid science surveys. In addition, the coronagraph technology demonstration will prove the feasibility of new techniques for exoplanet discovery, imaging, and spectral analysis. A composite truss structure meters both instruments to the telescope assembly, and the instruments and the spacecraft are flight serviceable. We present configuration changes since 2013 that improved interfaces, improved testability, and reduced technical risk. We provide an overview of our Integrated Modeling results, performed at an unprecedented level for a phase-A study, to illustrate performance margins with respect to static wavefront error, jitter, and thermal drift.