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Heterodyn Receiver for the Origins Space Telescope Concept 2

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Heterodyn Receiver for the Origins Space Telescope Concept 2 PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie Heterodyn receiver for the Origins Space Telescope concept 2 M. C. Wiedner, Susanne Aalto, Edward G. Amatucci, Andrey Baryshev, Cara Battersby, et al. M. C. Wiedner, Susanne Aalto, Edward G. Amatucci, Andrey Baryshev, Cara Battersby, Victor Belitsky, Edwin A. Bergin, Bruno Borgo, Ruth C. Carter, Asantha Cooray, James A. Corsetti, Elvire De Beck, Yan Delorme, Michael J. Dipirro, Vincent Desmaris, Brian Ellison, Juan-Daniel Gallego, Anna Maria Di Giorgio, Martin Eggens, Maryvonne Gerin, Paul F. Goldsmith, Christophe Goldstein, Frank Helmich, Fabrice Herpin, Richard E. Hills, Michiel R. Hogerheijde, Jean-Michel Huet, Leslie K. Hunt, Willem Jellema, Geert Keizer, Jean-Michel Krieg, Gabby Kroes, Philippe Laporte, André Laurens, David T. Leisawitz, Darek Lis, Gregory E. Martins, Imran Mehdi, Margaret Meixner, Gary Melnick, Stefanie N. Milam, David A. Neufeld, Napoléon Nguyen Tuong, René Plume, Klaus M. Pontoppidan, Benjamin Quertier-Dagorn, Christophe Risacher, Johannes G. Staguhn, Serena Viti, Friedrich Wyrowski, "Heterodyn receiver for the Origins Space Telescope concept 2," Proc. SPIE 10698, Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, 106981B (30 July 2018); doi: 10.1117/12.2313384 Event: SPIE Astronomical Telescopes + Instrumentation, 2018, Austin, Texas, United States Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 10/29/2018 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use Heterodyne Receiver for the Origins Space Telescope Concept 2 M.C. Wiedner*a, Susanne Aaltob, Edward G. Amatuccic, Andrey Baryshevd, Cara Battersbye, Victor Belitskyf, Edwin A. Berging, Bruno Borgoh, Ruth C. Carterc, Asantha Coorayi, James A. Corsettic, Elvire De Beckb, Yan Delormea, Michael J. Dipirroc, Vincent Desmarisf, Brian Ellisonj, Juan-Daniel Gallegok, Anna Maria Di Giorgiol, Martin Eggensm, Maryvonne Gerina, Paul F. Goldsmithn, Christophe Goldsteino, Frank Helmichm, Fabrice Herpinp, Richard E. Hillsq, Michiel R. Hogerheijder, Jean-Michel Huets, Leslie K. Huntt, Willem Jellemam, Geert Keizerm, Jean-Michel Kriega, Gabby Kroesu, Philippe Laportes, André Laurenso, David T. Leisawitzc, Darek Lisa, Gregory E. Martinsc, Imran Mehdin, Margaret Meixnerc,v,w, Gary Melnickx, Stefanie N. Milamc, David A. Neufeldw, Napoléon Nguyen Tuongh, René Plumey, Klaus M. Pontoppidanv, Benjamin Quertier- Dagornp, Christophe Risacherz,aa, Johannes G. Staguhnc,w, Serena Vitiab, Friedrich Wyrowskiz aSorbonne Université, Observatoire de Paris, Université PSL, CNRS, LERMA, F-75014, Paris, France; bDepartment of Space, Earth and Environment, Onsala Space Observatory, Chalmers University of Technology, 439 92, Onsala, Sweden; cNASA Goddard Space Flight Ctr., United States; dKapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV, Groningen, The Netherlands; eDepartment of Physics University of Connecticut 2152 Hillside Road, U-3046 Storrs, CT 06269; fGroup for Advanced Receiver Development (GARD), Department of Space, Earth and Environment, Chalmers University of Technology, 41296, Gothenburg, Sweden; gUniv. of Michigan (United States); Department of Astronomy, University of Michigan, 311 West Hall, 1085 S. University Ave, Ann Arbor, MI 48109, USA; hLESIA, Observatoire de Paris, CNRS, France; iCenter for Cosmology, Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA; jSTFC Rutherford Appleton Laboratory, Harwell Oxford, Didcot OX11 0QX, UK; kCtr. Astronómico de Yebes (Spain); Centro Astronómico de Yebes, Observatorio Astronómico Nacional, Apdo. 148, 19080 Guadalajara, Spain; lIstituto Nazionale di Astrofisica - Istituto di Astrofisica e Planetologia Spaziali, Via Fosso del Cavaliere 100, I-00133 Roma, Italy; mSRON Netherlands Institute for Space Research, Groningen, The Netherlands; nJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA, 91109, USA; oCentre National d'Études Spatiales, 18 Avenue Edouard Belin, 31400 Toulouse, France; pLaboratoire d'astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint- Hilaire, 33615, Pessac, France; qAstrophysics Group, Cavendish Laboratory, University of Cambridge, JJ Thomson Avenue, Cambridge, CB3 0HE, UK; rLeiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands; Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098, XH, Amsterdam, The Netherlands; sGEPI, Observatoire de Paris, CNRS, France; tINAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125, Firenze, Italy; uNOVA-ASTRON, The Netherlands; vSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; wDepartment of Physics and Astronomy, The Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA; xHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 66, Cambridge, MA 02138, USA; yDepartment of Physics & Astronomy and the Institute for Space Imaging Sciences, University of Calgary, Calgary, AB T2N 1N4, Canada; zMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany; aaIRAM, 300 rue de la Piscine, 38406 St. Martin d'Hères, France; abDepartment of Physics and Astronomy, University College London, Gower street, London, WC1E 6BT, UK; Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, edited by Makenzie Lystrup, Howard A. MacEwen, Giovanni G. Fazio, Proc. of SPIE Vol. 10698, 106981B © 2018 SPIE · CCC code: 0277-786X/18/$18 · doi: 10.1117/12.2313384 Proc. of SPIE Vol. 10698 106981B-1 Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 10/29/2018 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use ABSTRACT The Origins Space Telescope (OST) is a NASA study for a large satellite mission to be submitted to the 2020 Decadal Review. The proposed satellite has a fleet of instruments including the HEterodyne Receivers for OST (HERO). HERO is designed around the quest to follow the trail of water from the ISM to disks around protostars and planets. HERO will perform high-spectral resolution measurements with 2x9 pixel focal plane arrays at any frequency between 468GHz to 2,700GHz (617 to 111 μm). HERO builds on the successful Herschel/HIFI heritage, as well as recent technological innovations, allowing it to surpass any prior heterodyne instrument in terms of sensitivity and spectral coverage. Keywords: heterodyne receivers, far-IR instrumentation, space mission, focal plane arrays, decadal survey 1. INTRODUCTION The Origins Space Telescope (OST) is one of four science and technology definition studies selected by NASA for the 2020 Astronomy and Astrophysics Decadal survey. The OST is designed to address three major science questions: Are we alone in the Universe? How do planets become habitable? How do stars, galaxies, black holes, and the elements of life form from the cosmic dawn to today?[1]. To answer these questions the OST team proposes a large cooled space telescope for observations at near- to mid-IR wavelengths at unprecedented sensitivity[2] and has performed corresponding studies for two candidate concepts. Concept 1 uses a cooled 9.1m primary mirror[3] to feed five very versatile instruments. Concept 2 is a cooled, but smaller 5.9m primary mirror, optimized to achieve most of the key science goals of Concept 1 with four instruments. Concept 2 of the OST is an on-axis telescope whose 5.9m primary mirror has a collecting area equivalent to that of JWST. To mimimize far-IR background radiation, the telescope is cooled to 4K by sunshields, a cold baffle and cryocoolers[4,5]. OST is designed to operate between 5µm and 600µm. The key science questions influenced the design of the four instruments, but each retains a degree of flexibility, and thus opening an immense discovery space: The OST Survey Spectrometer[6] (OSS, resolution R ≈ 300 (for 25-580 μm) , R ~ 40,000 (at 112 μm/ λ for 25-580 μm) and R~325 000 (at 112 μm/ λ for 25-300 μm)) will provide imaging and spectroscopy over large extragalactic fields and study protoplanetary disks. The Mid-Infrared Imager, Spectrometer and Coronagraph (MISC) [7] instrument (R ≈ 300) will conduct transit and emission spectroscopy of Jupiter to Earth-sized exoplanets with simultaneous wavelength coverage from 5-25 μm. MISC also has an imaging spectrometer (R~ 5 to 10) and imager, that doubles as a guide system for the observatory. OST’s Far-Infrared Imaging Polarimeter (FIP) [8] conducts 50, 100, 250, and 500 μm imaging and polarimetry of wide extragalactic fields and star-forming regions in our Galaxy. The HEterodyne Receiver for OST (HERO, resolution R~105 -107 at wavelengths between 111 μm and 617 μm) measures the kinematics of gas in the interstellar medium and protoplanetary disks and solar system objects. The HEterodyne Receiver for OST (HERO) performs high-spectral resolution measurements across continuous frequency range of 468GHz to 2,700GHz via a multi-band 2x9 pixel focal plane array (FPA) architecture. Its design utilises considerable heterodyne receiver heritage associated with both spaceborne and ground-based instrumentation and encompasses the latest research and development work in the field. Lightweight optics send the sky signal and the local oscillator to focal plane heterodyne arrays with 9 pixels in two polarizations. Broadband amplifier multiplier chains provide a necessary local oscillator (LO) reference
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