The MIRI Coronagraphs
The Mid-Infrared Instrument for the James Webb Space Telescope, V: Predicted Performance of the MIRI Coronagraphs A. Boccaletti1, P.-O. Lagage2, P. Baudoz1,C.Beichman3.4.5,P.Bouchet2,C.Cavarroc6,D. Dubreuil2, Alistair Glasse7,A.M.Glauser8,D.C.Hines9, C.-P. Lajoie9, J. Lebreton3,4,M. D. Perrin9,L.Pueyo9,J.M.Reess1,G.H.Rieke10, S. Ronayette2,D.Rouan1,R. Soummer9, and G. S. Wright7 ABSTRACT The imaging channel on the Mid-Infrared Instrument (MIRI) is equipped with four coronagraphs that provide high contrast imaging capabilities for studying faint point sources and extended emission that would otherwise be overwhelmed by a bright point-source in its vicinity. Such bright sources might include stars that are orbited by exoplanets and circumstellar material, mass-loss envelopes around post-main-sequence stars, the near-nuclear environments in active galax- ies, and the host galaxies of distant quasars. This paper describes the coron- agraphic observing modes of MIRI, as well as performance estimates based on measurements of the MIRI flight model during cryo-vacuum testing. A brief 1LESIA, Observatoire de Paris-Meudon, CNRS, Universit´e Pierre et Marie Curie, Universit´eParis Diderot, 5 Place Jules Janssen, F-92195 Meudon, France 2Laboratoire AIM Paris-Saclay, CEA-IRFU/SAp, CNRS, Universit´e Paris Diderot, F-91191 Gif-sur- Yvette, France 3Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA 4NASA Exoplanet Science Institute, California Institute of Technology, 770 S. Wilson Ave., Pasadena, CA 91125, USA 5Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91107, USA 6Laboratoire AIM Paris-Saclay, CEA-IRFU/SAp, CNRS, Universit´e Paris Diderot, F-91191 Gif-sur- Yvette, France 7UK Astronomy Technology Centre, STFC, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 8ETH Zurich, Institute for Astronomy, Wolfgang-Pauli-Str.
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