Exo-C: Imaging Nearby Worlds

Total Page:16

File Type:pdf, Size:1020Kb

Exo-C: Imaging Nearby Worlds The cost information contained in this document is of a budgetary and planning nature and is intended for informational purposes only. It does not constitute a commitment on the part of JPL and Caltech. © 2014. All rights reserved. Exo-C STDT Interim Report Author List Author List Science and Technology Definition Team Karl Stapelfeldt..................................................................................................................... NASA Goddard (Chair) Ruslan Belikov ...................................................................................................................................... NASA Ames Geoffrey Bryden .................................................................................................................................... JPL/Caltech Kerri Cahoy ........................................................................................................................................................ MIT Supriya Chakrabarti ........................................................................................................................... UMass Lowell Mark Marley .......................................................................................................................................... NASA Ames Michael McElwain ............................................................................................................................ NASA Goddard Victoria Meadows ....................................................................................................................... Univ. of Washingon Eugene Serabyn ................................................................................................................................... JPL/Caltech John Trauger......................................................................................................................................... JPL/Caltech JPL Engineering Design Team Michael Brenner ......................................................................................................................... Exo-C Design Lead Keith Warfield.............................................................................................................................. Probe Study Office Frank Dekens................................................................................................................................ System Engineer Paul Brugarolas ........................................................................................................................... Pointing Engineer Serge Dubovitsky .......................................................................................................................... Flight Operations Robert Effinger ............................................................................................................................. Thermal Engineer Brian Hirsch ............................................................................................................................ Mechanical Engineer Andy Kissel ........................................................................................................................... Engineering Dynamics John Krist ................................................................................................................................... Optical Simulations Jared Lang .................................................................................................................................... System Engineer Joel Nissen ....................................................................................................................... Optical System Engineer Jeff Oseas .......................................................................................................................... Optical Design Engineer Eric Sunada ................................................................................................................................. Thermal Engineer With Additional Contributions by Sean Domagal-Goldman ................................................................................................................. NASA Goddard Marc Kuchner................................................................................................................................... NASA Goddard Peter Lawson ........................................................................................................................................ JPL/Caltech Aki Roberge ..................................................................................................................................... NASA Goddard Jagmit Sandhu ...................................................................................................................................... JPL/Caltech Sara Seager ....................................................................................................................................................... MIT i Exo-C STDT Interim Report 1—Table of Contents 1 Table of Contents 2 Executive Summary ............................................................................................................................................. 2-1 3 State of the Field at the Time of Probe Launch: The Exoplanet Science Landscape in 2024.............................. 3-1 3.1 Indirect Detections Using Stellar Reflex Motion ....................................................................................... 3-1 3.2 Transits .................................................................................................................................................... 3-1 3.3 Exoplanet Imaging Detections.................................................................................................................. 3-1 3.4 Disk Imaging ............................................................................................................................................ 3-2 3.5 Summary .................................................................................................................................................. 3-3 4 Design Reference Mission ................................................................................................................................... 4-1 4.1 Introduction: High-level Statement of Science Goals ............................................................................... 4-1 4.2 Detailed Description of Science Objectives .............................................................................................. 4-2 4.2.1 Exoplanet Target Samples .......................................................................................................... 4-2 4.2.2 Giant Planet Spectra.................................................................................................................... 4-4 4.2.3 Small Planet Spectra ................................................................................................................... 4-8 4.2.4 Debris Disk Imaging................................................................................................................... 4-11 4.3 Measurement Requirements .................................................................................................................. 4-15 4.3.1 Imaging Requirements ............................................................................................................... 4-15 4.3.2 Spectroscopic Requirements ..................................................................................................... 4-17 4.3.3 Mission Lifetime ......................................................................................................................... 4-20 4.4 Derived Instrument Requirements .......................................................................................................... 4-20 4.4.1 Overview .................................................................................................................................... 4-20 4.4.2 Telescope Aperture ................................................................................................................... 4-21 4.4.3 Coronagraphy ............................................................................................................................ 4-21 4.4.4 Wavefront Control ...................................................................................................................... 4-21 4.4.5 Stray Light ................................................................................................................................. 4-21 4.4.6 Imaging ...................................................................................................................................... 4-22 4.4.7 Spectroscopy ............................................................................................................................. 4-22 4.4.8 Detectors ................................................................................................................................... 4-23 4.4.9 Baseline Instrument Concept ..................................................................................................... 4-23 4.5 Mission Lifetime Science Observations Budget ..................................................................................... 4-23 4.6 Science Requirements Flow-Down ........................................................................................................ 4-23 4.6.1 Science Requirements to Mission Requirements .....................................................................
Recommended publications
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
    [Show full text]
  • RAD750 at Our Website: Click HERE RAD750• Board
    Full-service, independent repair center -~ ARTISAN® with experienced engineers and technicians on staff. TECHNOLOGY GROUP ~I We buy your excess, underutilized, and idle equipment along with credit for buybacks and trade-ins. Custom engineering Your definitive source so your equipment works exactly as you specify. for quality pre-owned • Critical and expedited services • Leasing / Rentals/ Demos equipment. • In stock/ Ready-to-ship • !TAR-certified secure asset solutions Expert team I Trust guarantee I 100% satisfaction Artisan Technology Group (217) 352-9330 | [email protected] | artisantg.com All trademarks, brand names, and brands appearing herein are the property o f their respective owners. Find the BAE Systems RAD750 at our website: Click HERE RAD750 Board Hardware Specification Document Number 234A524 Release Date August 1, 2000 Copyright by BAE SYSTEMS All Rights Reserved Document Number: 234A524 RAD750 CompactPCI Hardware Specification Notices Before using this information and the product it supports, be sure to read the general information on the back cover of this book. Trademarks The following are trademarks of International Business Machines Corporation in the United States, or other countries, or both: IBM IBM Logo PowerPC PowerPC 750 The following are trademarks of BAE SYSTEMS in the United States, or other countries, or both: RAD750 The following are registered trademarks of PCI Industrial Computer Manufacturing Group in the United States, or other countries, or both: PICMG CompactPCI Other company, product, and service names may be trademarks or service marks of others. Preliminary Edition (Version 4.0, 8/1/2000) This unpublished document is the preliminary edition of RAD750 3U CompactPCI board Hardware Specification.
    [Show full text]
  • Microkernel Mechanisms for Improving the Trustworthiness of Commodity Hardware
    Microkernel Mechanisms for Improving the Trustworthiness of Commodity Hardware Yanyan Shen Submitted in fulfilment of the requirements for the degree of Doctor of Philosophy School of Computer Science and Engineering Faculty of Engineering March 2019 Thesis/Dissertation Sheet Surname/Family Name : Shen Given Name/s : Yanyan Abbreviation for degree as give in the University calendar : PhD Faculty : Faculty of Engineering School : School of Computer Science and Engineering Microkernel Mechanisms for Improving the Trustworthiness of Commodity Thesis Title : Hardware Abstract 350 words maximum: (PLEASE TYPE) The thesis presents microkernel-based software-implemented mechanisms for improving the trustworthiness of computer systems based on commercial off-the-shelf (COTS) hardware that can malfunction when the hardware is impacted by transient hardware faults. The hardware anomalies, if undetected, can cause data corruptions, system crashes, and security vulnerabilities, significantly undermining system dependability. Specifically, we adopt the single event upset (SEU) fault model and address transient CPU or memory faults. We take advantage of the functional correctness and isolation guarantee provided by the formally verified seL4 microkernel and hardware redundancy provided by multicore processors, design the redundant co-execution (RCoE) architecture that replicates a whole software system (including the microkernel) onto different CPU cores, and implement two variants, loosely-coupled redundant co-execution (LC-RCoE) and closely-coupled redundant co-execution (CC-RCoE), for the ARM and x86 architectures. RCoE treats each replica of the software system as a state machine and ensures that the replicas start from the same initial state, observe consistent inputs, perform equivalent state transitions, and thus produce consistent outputs during error-free executions.
    [Show full text]
  • Interstellar Medium Sculpting of the HD 32297 Disk
    DRAFT VERSION MAY 31, 2018 Preprint typeset using LATEX style emulateapj v. 7/15/03 INTERSTELLAR MEDIUM SCULPTING OF THE HD 32297 DEBRIS DISK JOHN H. DEBES1,2,ALYCIA J. WEINBERGER3, MARC J. KUCHNER1 Draft version May 31, 2018 ABSTRACT We detect the HD 32297 debris disk in scattered light at 1.6 and 2.05 µm. We use these new observations together with a previous scattered light image of the disk at 1.1 µm to examine the structure and scattering efficiency of the disk as a function of wavelength. In addition to surface brightness asymmetries and a warped morphology beyond ∼1.′′5 for one lobe of the disk, we find that there exists an asymmetry in the spectral features of the grains between the northeastern and southwestern lobes. The mostly neutral color of the disk lobes imply roughly 1 µm-sized grains are responsible for the scattering. We find that the asymmetries in color and morphology can plausibly be explained by HD 32297’s motion into a dense ISM cloud at a relative velocity of15kms−1. We modeltheinteractionofdustgrainswith HIgasin thecloud. We argue that supersonic ballistic drag can explain the morphology of the debris disks of HD 32297, HD 15115, and HD 61005. Subject headings: stars:individual(HD 32297)—stars:individual(HD 15115)—stars:individual(HD 61005)— circumstellar disks—methods:n-body simulations—ISM ′′ 1. INTRODUCTION distances >0. 75 the disk is brighter on the NE side, i.e. re- Debris disks are created by the outgassing and collisions of versed from the asymmetry seen in scattered light images planetesimals that may resemble analogues to the comets, as- (Moerchen et al.
    [Show full text]
  • 100 Closest Stars Designation R.A
    100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79,
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Astrophysics Division Astrophysics Douglas Hudgins Program Scientist, Exoplanet Exploration Program Key NASA/SMD Science Themes
    National Aeronautics and Space Administration NASA and the Search for Life on Planets around Other Stars A presentation to the National Academies Committee on Exoplanet Science Strategy 6 March 2018 Paul Hertz Director, Astrophysics Division Astrophysics Douglas Hudgins Program Scientist, Exoplanet Exploration Program Key NASA/SMD Science Themes Protect and Improve Life on Earth Search for Life Elsewhere Discover the Secrets of the Universe 2 Talk summary 3 NASA’s Exoplanet Exploration Program Space Missions and Mission Studies Public Communications Kepler, WFIRST Decadal Studies K2 Starshade Coronagraph Supporting Research & Technology Key Sustaining Research NASA Exoplanet Science Institute Technology Development Coronagraph Masks Large Binocular Keck Single Aperture Telescope Interferometer Imaging and RV High-Contrast Deployable Archives, Tools, Sagan Fellowships, Imaging Starshades Professional Engagement NN-EXPLORE https://exoplanets.nasa.gov 4 Foundational Documents for the NASA’s Astrophysics Division 5 NASA’s cross-divisional Search for Life Elsewhere ASTROPHYSICS • Exoplanet detection and Planetary SCIENCE/ characterization ASTROBIOLOGY • Stellar characterization • Comparative planetology • Mission data analysis • Planetary atmospheres Hubble, Spitzer, Kepler, • Assessment of observable TESS, JWST, WFIRST, biosignatures etc. • Habitability EARTH SCIENCES • GCM • Planets as systems PLANETARY SCIENCE RESEARCH HELIOPHYSICS • Exoplanet characterization • Stellar characterization • Protoplanetary disks • Stellar winds • Planet formation • Detection of planetary • Comparative planetology magnetospheres 6 Exoplanet Exploration at NASA 2007 - present 7 The Spitzer Space Telescope For the last decade, the Spitzer Space Telescope has used both spectroscopic and photometric measurements in the mid-IR to probe exoplanets and exoplanetary systems. • Spitzer follow up observations of known transiting systems have revealed additional, new planets and helped refine measurements of the size and orbital dynamics of known planets as small as the Earth.
    [Show full text]
  • “Formas Primitivas” De Ideias Oopulares
    A FORMA DAS IDEIAS A Câmara Estenopeica Como Método de Destilação de “Formas Primitivas” de Ideias Populares (Expressões Idiomáticas) Salomé Filipa Pereira Arieira Tese de Doutoramento Directora Mª Sol Alonso Romera Facultad de Bellas Artes de Pontevedra Departamento de Dibujo Setembro 2015 Aos meus dois amores: ao meu marido Tony Oliveira e ao meu filho Gaspar, pelo amor infinito e indescritível com que recheiam os meus dias. Aos meus pais Odete e Filipe, pela coragem exemplar e pelo apoio que me transmitem sempre, desde o meu primeiro momento no mundo. À Diretora desta Tese, Sol Alonso, pela disponibilidade total que demonstrou ao longo destes anos para me guiar e acompanhar, e pela amizade e sabedoria com que desde sempre me presenteou. À Direção da Escola Artística de Soares dos Reis por todo o apoio dado ao longo destes últimos anos. Ao Miguel Paiva, à Luisa Fragoso e ao Leonardo Mira, por toda a colaboração e apoio prestados. Ao Miguel Borges (Cigano) pela disponibilidade demonstrada na cedência dos espaços que serviram de palco a várias imagens estenopeicas do projeto prático desta investigação. À Lurdes Arieira e à Claudia Tomás pelo empréstimo de alguns dos elementos fotografados (máquina de picar AGRADECIMENTOS carne e fichas de póquer). À Joana Castelo e ao David, pela gentileza que tiveram na digitalização dos negativos do projeto prático. À Sara e ao André (Blues Photography) pelo cuidado nas impressões fotográficas do projeto prático (versão impressa). À Eduarda Coelho, por me ter salvo no momento da análise sintática das Expressões Idiomáticas. À Maria Peña, cuja amizade se estende desde o início do Curso de Doutoramento, superanto barreiras físicas e temporais.
    [Show full text]
  • Collisional Modelling of the AU Microscopii Debris Disc
    A&A 581, A97 (2015) Astronomy DOI: 10.1051/0004-6361/201525664 & c ESO 2015 Astrophysics Collisional modelling of the AU Microscopii debris disc Ch. Schüppler1, T. Löhne1, A. V. Krivov1, S. Ertel2, J. P. Marshall3;4, S. Wolf5, M. C. Wyatt6, J.-C. Augereau7;8, and S. A. Metchev9 1 Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany e-mail: [email protected] 2 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile 3 School of Physics, University of New South Wales, NSW 2052 Sydney, Australia 4 Australian Centre for Astrobiology, University of New South Wales, NSW 2052 Sydney, Australia 5 Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24098 Kiel, Germany 6 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 7 Université Grenoble Alpes, IPAG, 38000 Grenoble, France 8 CNRS, IPAG, 38000 Grenoble, France 9 University of Western Ontario, Department of Physics and Astronomy, 1151 Richmond Avenue, London, ON N6A 3K7, Canada Received 14 January 2015 / Accepted 12 June 2015 ABSTRACT AU Microscopii’s debris disc is one of the most famous and best-studied debris discs and one of only two resolved debris discs around M stars. We perform in-depth collisional modelling of the AU Mic disc including stellar radiative and corpuscular forces (stellar winds), aiming at a comprehensive understanding of the dust production and the dust and planetesimal dynamics in the system. Our models are compared to a suite of observational data for thermal and scattered light emission, ranging from the ALMA radial surface brightness profile at 1.3 mm to spatially resolved polarisation measurements in the visible.
    [Show full text]
  • The Constellation Microscopium, the Microscope Microscopium Is A
    The Constellation Microscopium, the Microscope Microscopium is a small constellation in the southern sky, defined in the 18th century by Nicolas Louis de Lacaille in 1751–52 . Its name is Latin for microscope; it was invented by Lacaille to commemorate the compound microscope, i.e. one that uses more than one lens. The first microscope was invented by the two brothers, Hans and Zacharius Jensen, Dutch spectacle makers of Holland in 1590, who were also involved in the invention of the telescope (see below). Lacaille first showed it on his map of 1756 under the name le Microscope but Latinized this to Microscopium on the second edition published in 1763. He described it as consisting of "a tube above a square box". It contains sixty-nine stars, varying in magnitude from 4.8 to 7, the lucida being Gamma Microscopii of apparent magnitude 4.68. Two star systems have been found to have planets, while another has a debris disk. The stars that now comprise Microscopium may formerly have belonged to the hind feet of Sagittarius. However, this is uncertain as, while its stars seem to be referred to by Al-Sufi as having been seen by Ptolemy, Al-Sufi does not specify their exact positions. Microscopium is bordered Capricornus to the north, Piscis Austrinus and Grus to the west, Sagittarius to the east, Indus to the south, and touching on Telescopium to the southeast. The recommended three-letter abbreviation for the constellation, as adopted Seen in the 1824 star chart set Urania's Mirror (lower left) by the International Astronomical Union in 1922, is 'Mic'.
    [Show full text]
  • Arxiv:1904.05358V1 [Astro-Ph.EP] 10 Apr 2019
    Draft version April 12, 2019 Typeset using LATEX default style in AASTeX62 The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics From 10{100 AU Eric L. Nielsen,1 Robert J. De Rosa,1 Bruce Macintosh,1 Jason J. Wang,2, 3, ∗ Jean-Baptiste Ruffio,1 Eugene Chiang,3 Mark S. Marley,4 Didier Saumon,5 Dmitry Savransky,6 S. Mark Ammons,7 Vanessa P. Bailey,8 Travis Barman,9 Celia´ Blain,10 Joanna Bulger,11 Jeffrey Chilcote,1, 12 Tara Cotten,13 Ian Czekala,3, 1, y Rene Doyon,14 Gaspard Duchene^ ,3, 15 Thomas M. Esposito,3 Daniel Fabrycky,16 Michael P. Fitzgerald,17 Katherine B. Follette,18 Jonathan J. Fortney,19 Benjamin L. Gerard,20, 10 Stephen J. Goodsell,21 James R. Graham,3 Alexandra Z. Greenbaum,22 Pascale Hibon,23 Sasha Hinkley,24 Lea A. Hirsch,1 Justin Hom,25 Li-Wei Hung,26 Rebekah Ilene Dawson,27 Patrick Ingraham,28 Paul Kalas,3, 29 Quinn Konopacky,30 James E. Larkin,17 Eve J. Lee,31 Jonathan W. Lin,3 Jer´ ome^ Maire,30 Franck Marchis,29 Christian Marois,10, 20 Stanimir Metchev,32, 33 Maxwell A. Millar-Blanchaer,8, 34 Katie M. Morzinski,35 Rebecca Oppenheimer,36 David Palmer,7 Jennifer Patience,25 Marshall Perrin,37 Lisa Poyneer,7 Laurent Pueyo,37 Roman R. Rafikov,38 Abhijith Rajan,37 Julien Rameau,14 Fredrik T. Rantakyro¨,39 Bin Ren,40 Adam C. Schneider,25 Anand Sivaramakrishnan,37 Inseok Song,13 Remi Soummer,37 Melisa Tallis,1 Sandrine Thomas,28 Kimberly Ward-Duong,25 and Schuyler Wolff41 1Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 2Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 3Department of Astronomy, University of California, Berkeley, CA 94720, USA 4NASA Ames Research Center, Mountain View, CA 94035, USA 5Los Alamos National Laboratory, P.O.
    [Show full text]
  • Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆
    A&A 565, A15 (2014) Astronomy DOI: 10.1051/0004-6361/201323058 & c ESO 2014 Astrophysics Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel J. P. Marshall1,2, A. Moro-Martín3,4, C. Eiroa1, G. Kennedy5,A.Mora6, B. Sibthorpe7, J.-F. Lestrade8, J. Maldonado1,9, J. Sanz-Forcada10,M.C.Wyatt5,B.Matthews11,12,J.Horner2,13,14, B. Montesinos10,G.Bryden15, C. del Burgo16,J.S.Greaves17,R.J.Ivison18,19, G. Meeus1, G. Olofsson20, G. L. Pilbratt21, and G. J. White22,23 (Affiliations can be found after the references) Received 15 November 2013 / Accepted 6 March 2014 ABSTRACT Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3–10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process. Aims. The Herschel DEBRIS, DUNES, and GT programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 μm with the sensitiv- ity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system’s Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis.
    [Show full text]