DOCSLIB.ORG

CERN - Data Acces, Visualisation & Analysis CERN | July 2017

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
CERN - Data Acces, Visualisation & Analysis CERN | July 2017 Exoplanets CERN - Data acces, Visualisation & Analysis CERN | July 2017 Damien Ségransan, University of Geneva and Geneva planet Search team The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation 55 Cnc DACE aims at federating the European expertise in exoplanets’ research by providing an open access to all type of published (exo)planets data with dedicated visualisation, exchange and analysis tools. (Exo)planets related Data Access - Wide range of published Observational Data such as Radial Velocities and Transit Light Curves - Exoplanets Tables : exoplanets.org & exoplanet.eu - Theoretical data such as planet synthesis populations Visualisation & Statistical Online tools to compare, correlate and combine (Exo)planets data - Javascript visualisation library - Time series, images, correlation plots - Histograms, distribution parameters Direct access to state of the art data analysis tools The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Principe: mesure du décalage Doppler - Jupiter-Soleil : 12 m/s - Saturne-Soleil: 3 m/s - Terre-Soleil : 8 cm/s The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Observatoire de La 1ère planète extrasolaire : Haute-Provence 51 Pegase Tel. de 193 cm The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Comment découvrir une nouvelle planète... The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Quelques années plus tard... The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Fantastique! Mais que se passe-t-il? The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Système multiplanétaire autour de l’étoile de type solaire : HD147018 Période : 44 jours Période : 1000 jours Orbite excentrique Orbite circulaire masse minimum : 2 Mjup masse minimum : 7 Mjup The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation HARPS: précision < 1 m/s - Observatoire de Genève - Physikalisches Institut, Bern - Observatoire Haute-Provence ΔRV =1 m/s - Service d’Aéronomie, Paris - ESO ΔRV =1 m/s Δλ=0.00001 A ΔT =0.01 K 15 nm Δp=0.01 mBar 1/1000 pixel Pression contrôlée Température contrôlée The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation . HD10180 - a 7 planet low mass planetary system 6 Lovis et al., A&A 528, A112, 2011 4 ] s / m [ 2 V RV [m/s] R P = 1.17 .. 2248 days 0 K=0.85 .. 4.5 m/s msin(i)=1.4 .. 65 M 2 213 meas. O-C rms =1.40 m/s 0 50 100 150 200 250 300 350 True Longitude [deg] . 10 5 ] s / m [ 0 C 5 C [m/s] 5 5 O O ] ] 5 ] s s s / / / m m m [ 0 50 100 150 200 250 300 350 [ [ V V 0 V 0 True Longitude [deg] RV [m/s] R R RV [m/s] 0 RV [m/s] R 5 5 5 0 50 100 150 200 250 300 350 0 50 100 150 200 250 300 350 0 50 100 150 200 250 300 350 True Longitude [deg] . True Longitude [deg] . True Longitude [deg] . 8 5 5 ] 8 ] 5 ] s s / s / 6 / m m 6 m [ [ [ 0 0 60 C [m/s] C C C [m/s] C [m/s] C 4 4 O O O O O 4 ] ] 5 ] 5 s s 5 s / / / m m 2 m 0 50 100 150 200 250 300 350 [ [ 2 [ 0 50 100 150 200 250 300 350 2 0 50 100 150 200 250 300 350 V V True Longitude [deg] V True Longitude [deg] True Longitude [deg] RV [m/s] R RV [m/s] R RV [m/s] R 0 0 0 2 2 2 4 4 0 50 100 150 200 250 300 350 0 50 100 150 200 250 300 350 0 50 100 150 200 250 300 350 True Longitude [deg] True Longitude [deg] True Longitude [deg] 5 The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Transit photometry Rs Rp Flux hors du transit Fout 2 δ=(Rp/Rs) =(Fout-Fin)/Fout Flux Flux dans le transit Fin Time HD 209458b Période : 3.524 jours Orbite circulaire Charbonneau et al. 2000 (ApJ 529, L45) demi-grand axe : 0.045Jupiter UA masse minimum : 0.7 Mjup HD 209458b Précision photométrique 0.2–0.4% Petit télescope de 10cm!! The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation ~3h Jupiter ~1.7% HD 209458b 110 ppm/min The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation ρ = 1.3 g cm-3 ρ = 0.4 g cm-3 Jupiter HD 209458b The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation HR8799 Image dans prisent dans l’infrarouge proche - 1-2.5 microns Rapport de flux entre les planète et l’étoile : 10 000 The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation HR8799 - découverte 2008, Marois. Distance : 129 AL Age : 30 million d’années (Soleil 5 Milliard d’années) Masse : 1.5 Msol Luminosité : 4.9 Lsol Température effective : 7300K (Soleil ~5800K) 4 planètes massives Température : 900-1100 K <=> 630 - 830 ° C Présence de Méthane et CO dans l’atmosphère The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation 1.593 microns) and H3 (1.667 Toute nouvelle Découverte Cheetham, Ségransan et al., Décembre 2016 Distance : 136 AL Age : 5 milliard d’années (comme le Soleil) Masse : 1.0 Msol Luminosité : ~1 Lsol Température effective : 5700 K The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Détection avec SPHERE/VLT 1.593 µm 1.667 µm 1 objet massif et très froid! Température : 400-500 K <=> 130 - 230 ° C Présence de Méthane et CO dans l’atmosphère Séparation 0.53’’ => ~23 UA 1.0-1.3 µm Rapport de flux entre le companion et son étoile : 160 000 - 250 000 The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation Les chasseurs de planètes de l’Université de Genève Les académiques (7) : F. Bouchy, D. Ehrenreich, C. Lovis, F. Pepe, D.Queloz, D. Ségransan, S. Udry, M. Mayor (retraite) Les Post-Docs et collaborateurs scientifiques (~10) : S. Saesen, D. Bayliss, N. Blind, M. Marmier, N. Astudillo, V. Bourrier, H. Cegla, A. Cheetham, J-B. Delisle, X. Dumusque, … Les Doctorants (~15) : E. Cersullo, A. Coffinet, U. Conod, A. Deline, H. Giles, B. Lavie, D. Martin, F. Motalebi, E. Obrzud, S. Peretti, M. Raimbault, J. Rey Cerda, E. Rickmann, T. Roger, A. Wyttenbach The National Centres of Competence in Research (NCCR) are a research instrument of the Swiss National Science Foundation 358 F. Mignard / Advances in Space Research 47 (2011) 356–364 to compute the location of the images during the CCD the relationship between the G magnitude and the more crossing. usual V magnitude as a function of the colour index While the above estimate of astrometric performances V I. One has with a sufficient accuracy for this purpose includes the CCD charge loss resulting from the energetic (JordiÀ and Carrasco, 2007), particles bombardment during the Gaia lifetime, it does G V 0:0107 0:0879 V I 0:1630 V I 2 not take into account other consequences of this bombard- ¼ À À ð À ÞÀ ð À Þ ment like the PSF distortion and the still poorly modelled 0:0086 V I 3 1 effects observed during CCD readouts at high frequency. þ ð À Þ ð Þ These sources of degradation in the CCD performances, meaning that a red star of visual magnitude 15, looks and susceptible of generating bias in image locations and brighter for Gaia than a hotter star of similar visual mag- are being closely investigated by the prime contractor nitude. The standard deviations in Table 2 are averaged (EADS Astrium), ESA and the Data Processing Consor- out over the sky and the actual accuracy in a particular tium. This issue remains today the main instrumental chal- direction on the sky varies slightly with the ecliptic latitude, lenge for Gaia and a serious source of complication for the by a factor of ±20% about the average for the parallax, data processing. In the performances indicated here, a mar- right ascension and proper motion in right ascension, while gin of 20% has already been applied to allow for unmod- the factor is less than 5% for the corresponding quantities elled effects, but in some range of magnitude or colours, in declination.
Load more

Recommended publications
  • Technology Development for Future Sparse Aperture Telescopes and Interferometers in Space
    A Technology Whitepaper submitted to the 2010 Decadal Survey Technology Development for Future Sparse Aperture Telescopes and Interferometers in Space 24 March 2009 NASA Centers: GSFC: Kenneth G. Carpenter, Keith Gendreau, Jesse Leitner, Richard Lyon, Eric Stoneking MSFC: H. Philip Stahl Industrial Partners: Aurora Flight Systems: Joe Parrish LMATC: Carolus J. Schrijver, Robert Woodruff NGST – Amy Lo, Chuck Lillie Seabrook Engineering: David Mozurkewich University/Astronomical Institute Partners: College de France: Antoine Labeyrie MIT: David Miller NOAO: Ken Mighell SAO: Margarita Karovska, James Phillips STScI: Ronald J. Allen UCO/Boulder: Webster Cash Abstract We describe the major technology development efforts that need to occur throughout the 2010 decade in order to enable a wide variety of sparse aperture and interferometric missions in the following decade. These missions are critical to achieving the next major revolution in astronomical observations by dramatically increasing the achievable angular resolution by more than 2 orders of magnitude, over wavelengths stretching from the x-ray and ultraviolet into the infrared and sub-mm. These observations can only be provided by long-baseline interferometers or sparse aperture telescopes in space, since the aperture diameters required are in excess of 500m - a regime in which monolithic or segmented designs are not and will not be feasible - and since they require observations at wavelengths not accessible from the ground. The technology developments needed for these missions are challenging, but eminently feasible with a reasonable investment over the next decade to enable flight in the 2025+ timeframe. That investment would enable tremendous gains in our understanding of the structure of the Universe and of its individual components in ways both anticipated and unimaginable today.
    [Show full text]
  • Exoplanet Community Report
    JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probe­class missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2
    [Show full text]
  • Spectral Analysis of Atmospheres by Nulling Interferometry
    Molecules in the Atmospheres of Extrasolar Planets ASP Conference Series, Vol. 450 J-P. Beaulieu, S. Dieters, and G. Tinetti, eds. c 2011 Astronomical Society of the Pacific Spectral Analysis of Atmospheres by Nulling Interferometry M. Ollivier and S. Jacquinod Institut d’Astrophysique Spatiale - Université de Paris-Sud 11 and CNRS (UMR 8617) Abstract. Nulling interferometry has often been considered as one of the most promising techniques to get spectra, in the thermal infrared spectral range, of exo- planet and particularly telluric ones. The required performance, in terms of nulling depth, spectral bandwidth and stability begins to be achievable in the laboratory. How- ever, concrete observatory projects have strong difficulties to emerge in space agencies programs, because of mission requirements complexity. In this paper, I present the per- formance various scientific objectives need and the state of the art of this technique, including mission aspects. I finally propose elements that could help defining a first space mission project. 1. Nulling Interferometry : Theoretical Aspects 1.1. Principle of Nulling Interferometry Nulling interferometry has been proposed in the late 70s as a possible technique to detect and spectroscopically characterize planets around nearby stars at wavelengths where diffraction prevents from the use of single aperture telescopes (Bracewell 1978). The principle of nulling interferometry in a 2-telescope configuration is described in figure 1 (left). The idea is to use two small telescopes, pointed in the direction of the star and to combine their beams. On the beam combiner the wavefronts from both star and planet create interferences. If we introduce a π phase-shift in one arm of the inter- ferometer, the stellar interference is destructive (the optical path difference is equal to zero).
    [Show full text]
  • OLLI Talk on Exoplanets
    OLLI SC211 SPACE EXPLORATION: THE SEARCH FOR LIFE BEYOND EARTH April 13, 2017 Michal Peri NASA Solar System Ambassador Exoplanet2 Detection • Methods • Missions • Discoveries • Resources Image: C. Pulliam & D. Aguilar/CfA A long history … in our imaginations 3 https://en.wikipedia.org/wiki/Giordano_Bruno#/media/File:Relief_Bruno_Campo_dei_Fiori_n1.jpg Giordano Bruno in his De l'infinito universo et mondi (1584) suggested that "stars are other suns with their own planets” that “have no less virtue nor a nature different to that of our earth" and, like Earth, "contain animals and inhabitants.” For this heresy, he was burned by the inquisition. 3 https://www.loc.gov/today/cyberlc/feature_wdesc.php?rec=7148 5 Detection Methods Radial Velocity 619 planets Gravitational Microlensing 44 planets Direct Imaging 44 planets Transit 2771 planets Velocity generates Doppler 7 Shift Sound star receding star approaching Light wave “stretched” → red shift wave “squashed” → blue shift Orbiting planet causes Doppler shift in starlight 8 https://exoplanets.nasa.gov/interactable/11/ Radial Velocity Method 9 • The most successful method of detecting exoplanets pre-2010 • Doppler shifts in the stellar spectrum reveal presence of planetary companion(s) • Measure lower limit of the planetary mass and orbital parameters Doppler Shift Time Nikole K. Lewis, STScI Radial Velocity Detections Radial Velocity 1992 Planetary Mass 10 Detection Methods Radial Velocity 619 planets Gravitational Microlensing 44 planets Direct Imaging 44 planets Transit 2771 planets • Microlens
    [Show full text]
  • Interferometric Space Missions for Exoplanet Science: Legacy of Darwin/TPF
    Interferometric Space Missions for Exoplanet Science: Legacy of Darwin/TPF D. Defrere` 1, O. Absil1, and C. Beichman2 1 Space sciences, Technologies & Astrophysics Research (STAR) Institute, University of Liege, Liege, Belgium. 2 NASA Exoplanet Science Institute, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, Califor- nia, USA. Abstract DARWIN/TPF is a project of an infrared space-based interferometer designed to directly detect and charac- terize terrestrial exoplanets around nearby stars. Unlike spectro-photometric instruments observing planetary transits, an interferometer does not rely on any particular geometric constraints and could characterize exoplanets with any orbital configuration around nearby stars. The idea to use an infrared nulling interferometer to characterize exoplanets dates back to Bracewell(1978), and was extensively studied in the 1990s and 2000s by both ESA and NASA. The project focuses on the mid-infrared regime (5-20 mm), which provides access to key features of exoplanets, such as their size, their temperature, the presence of an atmosphere, their climate structure, as well as the presence of impor- tant atmospheric molecules such as H2O, CO2,O3, NH3, and CH4. This wavelength regime also provides a favorable planet/star contrast to detect the thermal emission of temperate (∼ 300 K) exoplanets (107 vs 1010 in the visible). In this chapter, we first review the scientific rationale of a mid-infrared nulling interferometer and present how it would provide an essential context for interpreting detections of possible biosignatures. Then, we present the main techno- logical challenges identified during the ESA and NASA studies, and how they have progressed over the last 10 years.
    [Show full text]
  • Infrared Direct Imaging
    Infrared Imaging of Exoplanets William C. Danchi January 5, 2012 ExoPAG #7 In 2009 we had the Exoplanet Community Report: The Infrared Chapter: DetecKng Earth-area Planets is Difficult and the Thermal Infrared is a Good Spectral Region . DetecKng light from planets beyond solar system is hard: – Earth sized planet emits few photons/sec/m2 at 10 μm – Parent star emits 106 more – Planet within 1 AU of star ~ 10-10 ~ 10-7 – Exozodi dust emission in target solar system x 300 brighter than earth-area planet for equiValent of ONE Solar System Zodi Earth Spectrum Peaks in the mid-IR Earth’s spectrum shows absorpKon features from many species, including ozone, nitrous oxide, water Vapor, carbon dioxide, and methane Biosignatures are molecules out of equilibrium such as oxygen, ozone, and methane or nitrous oxide. Spectroscopy with R ~ 50 is adequate to resolVe these features. Terrestrial Planet Finder Interferometer Salient Features • Formaon flying mid-IR nulling Interferometer • Starlight suppression to 10-5 • Heavy launch Vehicle • L2 baseline orbit • 5 year mission life (10 year goal) • PotenKal collaboraon with European Space Agency Science Goals • Detect as many as possible Earth-like planets in the habitable zone of nearby stars Via their thermal emission • Characterize physical properKes of detected Earth-like planets (size, orbital parameters, presence of atmosphere) and make low resoluKon spectral obserVaons looking for eVidence of a habitable planet and bio-markers such as O2, CO2, CH4 and H2O • Detect and characterize the components of nearby planetary systems including disks, terrestrial planets, giant planets and mulKple planet systems • Perform general astrophysics inVesKgaons as capability and Kme permit W.
    [Show full text]
  • The Fourier–Kelvin Stellar Interferometer (FKSI)
    C. R. Physique 8 (2007) 396–407 http://france.elsevier.com/direct/COMREN/ Optical techniques for direct imaging of exoplanets/Techniques optiques pour l’imagerie directe des exoplanètes The Fourier–Kelvin Stellar Interferometer (FKSI)—A practical infrared space interferometer on the path to the discovery and characterization of Earth-like planets around nearby stars a, b William C. Danchi ∗, Bruno Lopez a NASA Goddard Space Flight Center, Exoplanets and Stellar Astrophysics, Code 667, Greenbelt, MD 20771, USA b Observatoire de la Côte d’Azur, UMR 6203, BP 4229, 06304 Nice cedex 4, France Available online 11 June 2007 Abstract During the last few years, considerable effort has been directed towards large-scale (>$1 billion USD) missions to detect and characterize Earth-like planets around nearby stars, such as the Terrestrial Planet Finder Interferometer (TPF-I) and Darwin mis- sions. However, technological issues such as formation flying, cryocooling, null depth for broadband signals, control of systematic noise sources, budgetary pressures, and shifting science priorities at NASA and ESA, will prevent these missions from entering Phase A until the middle of the next decade. A simplified nulling interferometer operating in the near- to mid-infrared (e.g. 3–8 microns), like the Fourier–Kelvin Stellar Interferometer (FKSI), can characterize the atmospheres of a large sample of the kno∼ wn planets. Many other scientific problems can be addressed with a system like FKSI, including the imaging of debris disks, active galactic nuclei, and low mass companions around nearby stars. We discuss the rationale, both scientific and technological, for a competed mission in the $450–600 million (USD) range, of which FKSI is an example.
    [Show full text]
  • Natural Moons Dynamics and Astrometry
    OBSERVATOIRE DE PARIS MEMOIRE D’HABILITATION A DIRIGER DES RECHERCES Présenté par Valéry LAINEY Natural moons dynamics and astrometry Soutenue le 29 mai 2017 Jury: Anne LEMAITRE (Rapporteur) François MIGNARD (Rapporteur) William FOLKNER (Rapporteur) Doris BREUER (Examinatrice) Athéna COUSTENIS (Examinatrice) Carl MURRAY (Examinateur) Francis NIMMO (Examinateur) Bruno SICARDY (Président) 2 Index Curriculum Vitae 5 Dossier de synthèse 11 Note d’accompagnement 31 Coordination d’équipes et de réseaux internationaux 31 Encadrement de thèses 34 Tâches de service 36 Enseignement 38 Résumé 41 Annexe 43 Lainey et al. 2007 : First numerical ephemerides of the Martian moons Lainey et al. 2009 : Strong tidal dissipation in Io and Jupiter from astrometric observations Lainey et al. 2012 : Strong Tidal Dissipation in Saturn and Constraints on Enceladus' Thermal State from Astrometry Lainey et al. 2017 : New constraints on Saturn's interior from Cassini astrometric data Lainey 2008 : A new dynamical model for the Uranian satellites 3 4 Curriculum Vitae Name: Valéry Lainey Address: IMCCE/Observatoire de Paris, 77 Avenue Denfert-Rochereau, 75014 Paris, France Email: [email protected]; Tel.: (+33) (0)1 40 51 22 69 Birth: 19/08/1974 Qualifications: Ph.D. Observatoire de Paris, December 2002 Title of thesis: “Théorie dynamique des satellites galiléens" Master degree “Astronomie fondamentale, mécanique céleste et géodésie” Observatoire de Paris 1998. Academic Career: Sep. 2006 - Present Astronomer at the Paris Observatory Apr. 2004 - Aug. 2006 Post-doc position at the Royal Observatory of Belgium Jun. 2003 - Mar. 2004 Post-doc position at the Paris Observatory Mar. - May 2003 Invited fellow at the Indian Institute of Astrophysics Dec. 2002 - Feb.
    [Show full text]
  • Final Program
    8–12 JANUARY 2018 KISSIMMEE, FL SEIZING THE NEXT DIGITAL TRANSFORMATION See what’s in Check pages 169-172 for details. scitech.aiaa.org #aiaaSciTech A CLEAR VISION FOR THE FUTURE. AT LOCKHEED MARTIN, WE’RE ENGINEERING A BETTER TOMORROW.® Lockheed Martn Skunk Works® has been a trusted partner in creatng revolutonary aircraf and technologies for nearly 75 years. It took a clear vision to produce the world’s fastest jet aircraf, frst producton stealth fghter and highest fying manned aircraf. And it’s that same vision that will allow Skunk Works to contnue developing the world’s most advanced aircraf well into the future. Learn more at lockheedmartn.com/skunkworks © 2017 LOCKHEED MARTIN CORPORATION Contents Contents ............................................................3 Please be advised that AIAA’s partner for our forums is no longer supporting the conference Organizing Committee ...................................4 app. The full program can be found online here: http://aiaa-mst18.abstractcentral.com/itin.jsp Welcome ...........................................................5 or by scanning the QR code. AIAA is currently investigating a new conference app for future Sponsors and Supporters ...............................6 forums and would like your feedback regarding tools you would like to see included in the app. Pre-Forum Activities .......................................7 AIAA staff will be in the HUB on Wednesday, 0930–1130 hrs, to gather feedback from attendees. Please join us. Forum Overview ...........................................
    [Show full text]
  • Super Earth Explorer : SEE - COAST
    Super Earth Explorer : SEE - COAST J. Schneider, P. Riaud, A. Boccaletti D. Mawet, G. Tinetti Observatoire de Paris & IAP - France Institut d’Astrophysique de Liege - Belgium A. Boccaletti In Spirit of Bernard Lyot, Berkeley, 2007 Cosmic Vision Cosmic Vision is the ESA roadmap for 2015-2025 - call for proposal in early 2007 - several mission class (Astrophysics, Solar System, Fundamental Physics) : - medium : < 300M€ - launch 2018 - large : < 650M€ - launch 2020 - xlarge : > 650M€ - launch >2020 (+ other space agencies) - proposal submission by June 2007 - down-selection by the end of 2007 (3 M missions out of 40) - assessment phase by ESA in 2008 - 2009 : 2M missions out of 3 - definition study 2009 - 2010 - 2011 : 1M mission out of 2 - launch (medium class) : 2018 Exoplanet proposals (main ones) : - Pegase (technology demonstrator, 2/3 spacecrafts) : medium class - PLATO (improved CoRoT) : medium class - DARWIN (4/5 spacecrafts) : xlarge => room/need for a scientific precursor to DARWIN : SEE-COAST A. Boccaletti In Spirit of Bernard Lyot, Berkeley, 2007 SEE - COAST management SEE-COAST stands for : Super Earth Explorer - Coronagraphic Off-Axis Space Telescope - a scientific precursor to DARWIN - a technological precursor to TPF-C PI : J. Schneider (Obs. Paris) A large European consortium : (France, Belgium, Switzerland, Italy, Nederland, UK, Germany) ULg / CSL / LESIA / LUTH / LUAN / ETH-Zurich / IAP / Obs. Geneva U. Bern / UCL / ROE / U. Hertfords. / MSSL / SRON / Astron / U. Utrecht LAOG / ONERA / DLR / U. Vienna / U. Nantes / U. Torino
    [Show full text]
  • Pegase: a Space-Based Nulling Interferometer
    Pegase: a space-based nulling interferometer a b b c c c c,g J.M. Le Duigou* , M. Ollivier , A. Léger , F. Cassaing , B. Sorrente , B. Fleury , G. Rousset , O. Absild, D. Mourarde, Y. Rabbiae, L. Escarrate, F. Malbetf, D. Rouang, R. Clédassoua, M. Delpecha, P. Duchona, B. Meyssignaca, P.-Y. Guidottia, N. Goriusa a Centre National d’Etudes Spatiale (CNES), b Institut d’Astrophysique Spatiale (IAS), c Office National d’Etudes et de Recherches Aéronautiques (ONERA), d Université de Liège, e Observatoire de la Côte d’Azur (OCA), f Laboratoire d’Astrophysique de l’Observatoire de Grenoble (LAOG), g Observatoire de Paris ABSTRACT The space based mission Pegase was proposed to CNES in the framework of its call for scientific proposals for formation flying missions. This paper presents a summary of the phase-0 performed in 2005. The main scientific goal is the spectroscopy of hot Jupiters (Pegasides) and brown dwarfs from 2.5 to 5 µm. The mission can extend to other objectives such as the exploration of the inner part of protoplanetary disks, the study of dust clouds around AGN,... The instrument is basically a two-aperture (D=40 cm) interferometer composed of three satellites, two siderostats and one beam- combiner. The formation is linear and orbits around L2, pointing in the anti-solar direction within a +/-30° cone. The baseline is adjustable from 50 to 500 m in both nulling and visibility measurement modes. The angular resolution ranges from 1 to 20 mas and the spectral resolution is 60. In the nulling mode, a 2.5 nm rms stability of the optical path difference (OPD) and a pointing stability of 30 mas rms impose a two level control architecture.
    [Show full text]
  • The ASTRONET Infrastructure Roadmap
    The ASTRONET Infrastructure Roadmap: A Strategic Plan for European Astronomy The ASTRONET Infrastructure Roadmap: A Strategic Plan for European Astronomy European for Plan A Strategic Roadmap: Infrastructure The ASTRONET The ASTRONET Infrastructure Roadmap This document has been created by the Infrastructure Roadmap Working Group and Panels under the auspices of ASTRONET, acting on behalf of the following member agencies: ARRS (SI), BMBF and PT-DESY (DE), IA CAS (CZ), CNRS/INSU (FR), DFG (DE), ESA (INT), ESO (INT), ESF (EE), FWF (AT), GNCA (GR), HAS (HU), SAS (SK), INAF (IT), LAS (LT), MICINN (ES), MPG (DE), NCBiR (PL), NOTSA (Nordic), NWO (NL), RSA (RO), SER (CH), SRC (SE), STFC (UK), UAS (UA). Editors: Michael F. Bode, Maria J. Cruz & Frank J. Molster ISBN: 978-3-923524-63-1 Acknowledgments: The ASTRONET project has been made possible via the generous support of the European Commission through Framework Programme 6. We gratefully acknowledge the tremendous amount of work that has been undertaken by the total of over 60 scientists and programme managers from across Europe who have given their time to the formulation of the Infrastructure Roadmap with dedication and enthusiasm. We acknowledge the help received from the ‘computergroep’ of the Leiden Observatory in setting up and hosting the web-based discussion forum. We also thank the Liverpool John Moores University Conference and Events team, Computing and Information Services department and the staff and students of the LJMU Astrophysics Research Institute who helped with the organisation and running of the Roadmap Symposium, and the astronomical community at large for their invaluable input to the whole process.
    [Show full text]