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Title:
High precision astrometry mission for the detection and characterization of nearby habitable planetary systems with the Nearby Earth Astrometric Telescope (NEAT)
Authors:
Malbet, Fabien; Léger, Alain; Shao, Michael; Goullioud, Renaud; Lagage, Pierre-Olivier; Brown, Anthony G. A.; Cara, Christophe; Durand, Gilles; Eiroa, Carlos; Feautrier, Philippe; Jakobsson, Björn; Hinglais, Emmanuel; Kaltenegger, Lisa; Labadie, Lucas; Lagrange, Anne-Marie; Laskar, Jacques; Liseau, René; Lunine, Jonathan; Maldonado, Jesús; Mercier, Manuel; Mordasini, Christoph; Queloz, Didier; Quirrenbach, Andreas; Sozzetti, Alessandro; Traub, Wesley; Absil, Olivier; Alibert, Yann; Andrei, Alexandre Humberto; Arenou, Frédéric; Beichman, Charles; Chelli, Alain; Cockell, Charles S.; Duvert, Gilles; Forveille, Thierry; Garcia, Paulo J. V.; Hobbs, David; Krone-Martins, Alberto; Lammer, Helmut; Meunier, Nadège; Minardi, Stefano; Moitinho de Almeida, André; Rambaux, Nicolas; Raymond, Sean; Röttgering, Huub J. A.; Sahlmann, Johannes; Schuller, Peter A.; Ségransan, Damien; Selsis, Franck; Surdej, Jean; Villaver, Eva; White, Glenn J.; Zinnecker, Hans
Affiliation:
AA(Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), UMR 5274, UJF-Grenoble 1/CNRS-INSU), AB(Institut d'Astrophysique Spatiale (IAS), UMR 8617, Université Paris Sud/CNRS-INSU), AC(Jet Propulsion Laboratory (JPL), California Institute of Technology), AD(Jet Propulsion Laboratory (JPL), California Institute of Technology), AE(Laboratoire AIM, UMR 7158, CEA-IRFU/CNRS-INSU/Université Paris Diderot), AF(Leiden Observatory, Leiden University), AG(Laboratoire AIM, UMR 7158, CEA-IRFU/CNRS-INSU/Université Paris Diderot), AH(Laboratoire AIM, UMR 7158, CEA-IRFU/CNRS-INSU/Université Paris Diderot), AI(Dpto. Física Teórica, Módulo 15, Facultad de Ciencias, Universidad Autónoma de Madrid (UAM)), AJ(Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), UMR 5274, UJF-Grenoble 1/CNRS-INSU), AK(Swedish Space Corporation (SSC)), AL(Centre spatial de Toulouse, Centre National d'Etudes Spatiales (CNES)), AM(Max-Planck-Institut für Astronomie), AN(I. Physikalisches Institut der Universität zu Köln), AO(Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), UMR 5274, UJF-Grenoble 1/CNRS-INSU), AP(Institut de mécanique céleste et de calcul des éphémérides (IMCCE), UMR 8028, UPMC-Paris 6/Observatoire de Paris/CNRS-INSU), AQ(Chalmers University of Technology), AR(Dipartimento di Fisica, University of Rome Tor Vergata), AS(Dpto. Física Teórica, Módulo 15, Facultad de Ciencias, Universidad Autónoma de Madrid (UAM)), AT(Thales Alenia Space), AU(Max-Planck-Institut für Astronomie), AV(Observatoire de Genève, Université de Genève), AW(Landessternwarte, Universität Heidelberg), AX(Osservatorio Astronomico di Torino, INAF), AY(Jet Propulsion Laboratory (JPL), California Institute of Technology), AZ(Département d'Astrophysique, Géophysique et Océanographie, Université de Liège), BA(Physikalisches Institut, University of Bern; Institut UTINAM, UMR 6213, Université de Besançon/Observatoire de Besançon/CNRS-INSU), BB(Osservatorio Astronomico di Torino, INAF; , Observatorio Nacional - Ministério da Ciência e Tecnologia), BC("Galaxie Etoile Physique Instrumentation" (GEPI), UMR 8111, Université Paris 7 Diderot/Observatoire de Paris/CNRS-INSU), BD(NASA Exoplanet Science Institute/IPAC, California Institute of Technology), BE(Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), UMR 5274, UJF-Grenoble 1/CNRS-INSU), BF(Department of Physics & Astronomy, Planetary and Space Sciences Research Institute, The Open University), BG(Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), UMR 5274, UJF-Grenoble 1/CNRS-INSU), BH(Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), UMR 5274, UJF-Grenoble 1/CNRS-INSU), BI(Faculdade de Engenharia, Departamento de Engenharia Fsica, Universidade do Porto), BJ(Lund Observatory, Lund University), BK(Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo; Laboratoire d'Astrophysique de Bordeaux, UMR 5804, Université de Bordeaux 1/Observatoire Aquitain des Sciences de l'Univers/CNRS-INSU), BL(Space Research Institute, Austrian Academy of Sciences), BM(Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), UMR 5274, UJF-Grenoble 1/CNRS-INSU), BN(Institute of Applied Physics, Friedrich Schiller, University Jena), BO(Systems, Instrumentation and Modeling (SIM), Faculdade de Ciências da Universidade de Lisboa), BP(Institut de mécanique céleste et de calcul des éphémérides (IMCCE), UMR 8028, UPMC-Paris 6/Observatoire de Paris/CNRS-INSU), BQ(Laboratoire d'Astrophysique de Bordeaux, UMR 5804, Université de Bordeaux 1/Observatoire Aquitain des Sciences de l'Univers/CNRS-INSU), BR(Leiden Observatory, Leiden University), BS(Observatoire de Genève, Université de Genève), BT(Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris 7 Diderot/Université Pierre et Marie Curie/Observatoire de Paris/CNRS-INSU, UMR 8109), BU(Observatoire de Genève, Université de Genève), BV(Laboratoire d'Astrophysique de Bordeaux, UMR 5804, Université de Bordeaux 1/Observatoire Aquitain des Sciences de l'Univers/CNRS-INSU), BW(Département d'Astrophysique, Géophysique et Océanographie, Université de Liège), BX(Dpto. Física Teórica, Módulo 15, Facultad de Ciencias, Universidad Autónoma de Madrid (UAM)), BY(Department of Physics & Astronomy, The Open University; Rutherford Laboratory, Space Science & Technology Department, CCLRC Rutherford Appleton Laboratory), BZ(Deutsches SOFIA Institut, Institut für Raumfahrtsysteme, Universität Stuttgart; , SOFIA Science Center, NASA-Ames)
Publication:
Experimental Astronomy, Volume 34, Issue 2, pp.385-413 (ExA Homepage)
Publication Date:
10/2012
Origin:
SPRINGER
Keywords:
Exoplanets, Planetary systems, Planetary formation, Astrometry, Space Mission
Abstract Copyright:
(c) 2012: Springer Science+Business Media B.V.
DOI:
10.1007/s10686-011-9246-1
Bibliographic Code:
2012ExA....34..385M

Abstract

A complete census of planetary systems around a volume-limited sample of solar-type stars (FGK dwarfs) in the Solar neighborhood ( d <= 15 pc) with uniform sensitivity down to Earth-mass planets within their Habitable Zones out to several AUs would be a major milestone in extrasolar planets astrophysics. This fundamental goal can be achieved with a mission concept such as NEAT---the Nearby Earth Astrometric Telescope. NEAT is designed to carry out space-borne extremely-high-precision astrometric measurements at the 0.05 muas (1 sigma) accuracy level, sufficient to detect dynamical effects due to orbiting planets of mass even lower than Earth's around the nearest stars. Such a survey mission would provide the actual planetary masses and the full orbital geometry for all the components of the detected planetary systems down to the Earth-mass limit. The NEAT performance limits can be achieved by carrying out differential astrometry between the targets and a set of suitable reference stars in the field. The NEAT instrument design consists of an off-axis parabola single-mirror telescope (D = 1 m), a detector with a large field of view located 40 m away from the telescope and made of 8 small movable CCDs located around a fixed central CCD, and an interferometric calibration system monitoring dynamical Young's fringes originating from metrology fibers located at the primary mirror. The mission profile is driven by the fact that the two main modules of the payload, the telescope and the focal plane, must be located 40 m away leading to the choice of a formation flying option as the reference mission, and of a deployable boom option as an alternative choice. The proposed mission architecture relies on the use of two satellites, of about 700 kg each, operating at L2 for 5 years, flying in formation and offering a capability of more than 20,000 reconfigurations. The two satellites will be launched in a stacked configuration using a Soyuz ST launch vehicle. The NEAT primary science program will encompass an astrometric survey of our 200 closest F-, G- and K-type stellar neighbors, with an average of 50 visits each distributed over the nominal mission duration. The main survey operation will use approximately 70% of the mission lifetime. The remaining 30% of NEAT observing time might be allocated, for example, to improve the characterization of the architecture of selected planetary systems around nearby targets of specific interest (low-mass stars, young stars, etc.) discovered by Gaia, ground-based high-precision radial-velocity surveys, and other programs. With its exquisite, surgical astrometric precision, NEAT holds the promise to provide the first thorough census for Earth-mass planets around stars in the immediate vicinity of our Sun.
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