Gaia Factsheet
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REVIEW ARTICLE the NASA Spitzer Space Telescope
REVIEW OF SCIENTIFIC INSTRUMENTS 78, 011302 ͑2007͒ REVIEW ARTICLE The NASA Spitzer Space Telescope ͒ R. D. Gehrza Department of Astronomy, School of Physics and Astronomy, 116 Church Street, S.E., University of Minnesota, Minneapolis, Minnesota 55455 ͒ T. L. Roelligb NASA Ames Research Center, MS 245-6, Moffett Field, California 94035-1000 ͒ M. W. Wernerc Jet Propulsion Laboratory, California Institute of Technology, MS 264-767, 4800 Oak Grove Drive, Pasadena, California 91109 ͒ G. G. Faziod Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 ͒ J. R. Houcke Astronomy Department, Cornell University, Ithaca, New York 14853-6801 ͒ F. J. Lowf Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, Arizona 85721 ͒ G. H. Riekeg Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, Arizona 85721 ͒ ͒ B. T. Soiferh and D. A. Levinei Spitzer Science Center, MC 220-6, California Institute of Technology, 1200 East California Boulevard, Pasadena, California 91125 ͒ E. A. Romanaj Jet Propulsion Laboratory, California Institute of Technology, MS 264-767, 4800 Oak Grove Drive, Pasadena, California 91109 ͑Received 2 June 2006; accepted 17 September 2006; published online 30 January 2007͒ The National Aeronautics and Space Administration’s Spitzer Space Telescope ͑formerly the Space Infrared Telescope Facility͒ is the fourth and final facility in the Great Observatories Program, joining Hubble Space Telescope ͑1990͒, the Compton Gamma-Ray Observatory ͑1991–2000͒, and the Chandra X-Ray Observatory ͑1999͒. Spitzer, with a sensitivity that is almost three orders of magnitude greater than that of any previous ground-based and space-based infrared observatory, is expected to revolutionize our understanding of the creation of the universe, the formation and evolution of primitive galaxies, the origin of stars and planets, and the chemical evolution of the universe. -
Asteroseismology with Corot, Kepler, K2 and TESS: Impact on Galactic Archaeology Talk Miglio’S
Asteroseismology with CoRoT, Kepler, K2 and TESS: impact on Galactic Archaeology talk Miglio’s CRISTINA CHIAPPINI Leibniz-Institut fuer Astrophysik Potsdam PLATO PIC, Padova 09/2019 AsteroseismologyPlato as it is : a Legacy with CoRoT Mission, Kepler for Galactic, K2 and TESS: impactArchaeology on Galactic Archaeology talk Miglio’s CRISTINA CHIAPPINI Leibniz-Institut fuer Astrophysik Potsdam PLATO PIC, Padova 09/2019 Galactic Archaeology strives to reconstruct the past history of the Milky Way from the present day kinematical and chemical information. Why is it Challenging ? • Complex mix of populations with large overlaps in parameter space (such as Velocities, Metallicities, and Ages) & small volume sampled by current data • Stars move away from their birth places (migrate radially, or even vertically via mergers/interactions of the MW with other Galaxies). • Many are the sources of migration! • Most of information was confined to a small volume Miglio, Chiappini et al. 2017 Key: VOLUME COVERAGE & AGES Chiappini et al. 2018 IAU 334 Quantifying the impact of radial migration The Rbirth mix ! Stars that today (R_now) are in the green bins, came from different R0=birth Radial Migration Sources = bar/spirals + mergers + Inside-out formation (gas accretion) GalacJc Center Z Sun R Outer Disk R = distance from GC Minchev, Chiappini, MarJg 2013, 2014 - MCM I + II A&A A&A 558 id A09, A&A 572, id A92 Two ways to expand volume for GA • Gaia + complementary photometric information (but no ages for far away stars) – also useful for PIC! • Asteroseismology of RGs (with ages!) - also useful for core science PLATO (miglio’s talk) The properties at different places in the disk: AMR CoRoT, Gaia+, K2 + APOGEE Kepler, TESS, K2, Gaia CoRoT, Gaia+, K2 + APOGEE PLATO + 4MOST? Predicon: AMR Scatter increases towards outer regions Age scatter increasestowars outer regions ExtracGng the best froM GaiaDR2 - Anders et al. -
Tiny "Chipsat" Spacecra Set for First Flight
7/24/2019 Tiny "Chipsat" Spacecraft Set for First Flight - Scientific American Subscribe S P A C E Tiny "Chipsat" Spacecra Set for First Flight Launch in July will test new way to explore the solar system—and beyond By Nicola Jones, Nature magazine on June 1, 2016 A rearward view of the International Space Station. Credit: NASA/Crew of STS-132 On 6 July, if all goes to plan, a pack of about 100 sticky-note-sized ‘chipsats’ will be launched up to the International Space Station for a landmark deployment. During a brief few days of testing, the minuscule satellites will transmit data on their energy load and orientation before they drift out of orbit and burn up in Earth’s atmosphere. https://www.scientificamerican.com/article/tiny-chipsat-spacecraft-set-for-first-flight/ 1/6 7/24/2019 Tiny "Chipsat" Spacecraft Set for First Flight - Scientific American The chipsats, flat squares that measure just 3.2 centimetres to a side and weigh about 5 grams apiece, were designed for a PhD project. Yet their upcoming test in space is a baby step for the much-publicized Breakthrough Starshot mission, an effort led by billionaire Yuri Milner to send tiny probes on an interstellar voyage. “We’re extremely excited,” says Brett Streetman, an aerospace engineer at the non- profit Charles Stark Draper Laboratory in Cambridge, Massachusetts, who has investigated the feasibility of sending chipsats to Jupiter’s moon Europa. “This will give flight heritage to the chipsat platform and prove to people that they’re a real thing with real potential.” The probes are the most diminutive members of a growing family of small satellites. -
LISA, the Gravitational Wave Observatory
The ESA Science Programme Cosmic Vision 2015 – 25 Christian Erd Planetary Exploration Studies, Advanced Studies & Technology Preparations Division 04-10-2010 1 ESAESA spacespace sciencescience timelinetimeline JWSTJWST BepiColomboBepiColombo GaiaGaia LISALISA PathfinderPathfinder Proba-2Proba-2 PlanckPlanck HerschelHerschel CoRoTCoRoT HinodeHinode AkariAkari VenusVenus ExpressExpress SuzakuSuzaku RosettaRosetta DoubleDouble StarStar MarsMars ExpressExpress INTEGRALINTEGRAL ClusterCluster XMM-NewtonXMM-Newton CassiniCassini-H-Huygensuygens SOHOSOHO ImplementationImplementation HubbleHubble OperationalOperational 19901990 19941994 19981998 20022002 20062006 20102010 20142014 20182018 20222022 XMM-Newton • X-ray observatory, launched in Dec 1999 • Fully operational (lost 3 out of 44 X-ray CCD early in mission) • No significant loss of performances expected before 2018 • Ranked #1 at last extension review in 2008 (with HST & SOHO) • 320 refereed articles per year, with 38% in the top 10% most cited • Observing time over- subscribed by factor ~8 • 2,400 registered users • Largest X-ray catalogue (263,000 sources) • Best sensitivity in 0.2-12 keV range • Long uninterrupted obs. • Follow-up of SZ clusters 04-10-2010 3 INTEGRAL • γ-ray observatory, launched in Oct 2002 • Imager + Spectrograph (E/ΔE = 500) + X- ray monitor + Optical camera • Coded mask telescope → 12' resolution • 72 hours elliptical orbit → low background • P/L ~ nominal (lost 4 out 19 SPI detectors) • No serious degradation before 2016 • ~ 90 refereed articles per year • Obs -
Data Mining in the Spanish Virtual Observatory. Applications to Corot and Gaia
Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society held on September 13 - 17, 2010, in Madrid, Spain. M. R. Zapatero Osorio et al. (eds.) Data mining in the Spanish Virtual Observatory. Applications to Corot and Gaia. Mauro L´opez del Fresno1, Enrique Solano M´arquez1, and Luis Manuel Sarro Baro2 1 Spanish VO. Dep. Astrof´ısica. CAB (INTA-CSIC). P.O. Box 78, 28691 Villanueva de la Ca´nada, Madrid (Spain) 2 Departamento de Inteligencia Artificial. ETSI Inform´atica.UNED. Spain Abstract Manual methods for handling data are impractical for modern space missions due to the huge amount of data they provide to the scientific community. Data mining, understood as a set of methods and algorithms that allows us to recover automatically non trivial knowledge from datasets, are required. Gaia and Corot are just a two examples of actual missions that benefits the use of data mining. In this article we present a brief summary of some data mining methods and the main results obtained for Corot, as well as a description of the future variable star classification system that it is being developed for the Gaia mission. 1 Introduction Data in Astronomy is growing almost exponentially. Whereas projects like VISTA are pro- viding more than 100 terabytes of data per year, future initiatives like LSST (to be operative in 2014) and SKY (foreseen for 2024) will reach the petabyte level. It is, thus, impossible a manual approach to process the data returned by these surveys. It is impossible a manual approach to process the data returned by these surveys. -
+ New Horizons
Media Contacts NASA Headquarters Policy/Program Management Dwayne Brown New Horizons Nuclear Safety (202) 358-1726 [email protected] The Johns Hopkins University Mission Management Applied Physics Laboratory Spacecraft Operations Michael Buckley (240) 228-7536 or (443) 778-7536 [email protected] Southwest Research Institute Principal Investigator Institution Maria Martinez (210) 522-3305 [email protected] NASA Kennedy Space Center Launch Operations George Diller (321) 867-2468 [email protected] Lockheed Martin Space Systems Launch Vehicle Julie Andrews (321) 853-1567 [email protected] International Launch Services Launch Vehicle Fran Slimmer (571) 633-7462 [email protected] NEW HORIZONS Table of Contents Media Services Information ................................................................................................ 2 Quick Facts .............................................................................................................................. 3 Pluto at a Glance ...................................................................................................................... 5 Why Pluto and the Kuiper Belt? The Science of New Horizons ............................... 7 NASA’s New Frontiers Program ........................................................................................14 The Spacecraft ........................................................................................................................15 Science Payload ...............................................................................................................16 -
The GAIA/CHEOPS Synergy
The GAIA/CHEOPS synergy Valerio Nascimbeni (INAF-OAPD) and the CHEOPS A1 working group CHEOPS Science workshop #3, Madrid 2015 Jun 17-19 Introduction GAIA is the most accurate (~10 μas) astrometric survey ever; it was launched in 2013 and is performing well (though some technical issues) Final catalog is expected in ≥2022, with a few intermediate releases starting from 2016 What planets (or planetary candidates) can GAIA provide to CHEOPS? This was investigated within the CHEOPS A1 WG, designed to 1) build an overview of available targets, 2) monitor present and future planet-search surveys, 3) establishing selection criteria for CHEOPS, 4) and proposing strategies to build the target list. CHEOPS Science workshop #3, Madrid 2015 Jun 17-19 The GAIA/CHEOPS synergy We started reviewing some recent works about the GAIA planet yield: ▶ Casertano+ 2008, A&A 482, 699. “Double-blind test program for astrometric planet detection with GAIA” ▶ Perryman+ 2014, Apj 797, 14. “Astrometric Exoplanet Detection with GAIA” ▶ Dzigan & Zucker 2012, ApJ 753, 1. “Detection of Transiting Jovian Exoplanets by GAIA Photometry” ▶ Sozzetti+ 2014, MNRAS 437, 497, “Astrometric detection of giant planets around nearby M dwarfs: the GAIA potential” ▶ Lucy 2014, A&A 571, 86. “Analysing weak orbital signals in GAIA data” ▶ Sahlmann+ 2015, MNRAS 447, 287. “GAIA's potential for the discovery of circumbinary planets” CHEOPS Science workshop #3, Madrid 2015 Jun 17-19 “Photometric” planets Challenges of GAIA planets discovered by photometry: ▶ GAIA's photometric detection of transiting planets will be limited by precision (1 mmag) and especially by the sparse sampling of the scanning law (Dzigan & Zucker 2012) ▶ Nearly all those planets will be VHJ (P < 3 d); only ~40 of them will be robustly detected and bright enough for CHEOPS (G < 12). -
Towards a Demonstrator for Autonomous Object Detection on Board Gaia Shan Mignot
Towards a demonstrator for autonomous object detection on board Gaia Shan Mignot To cite this version: Shan Mignot. Towards a demonstrator for autonomous object detection on board Gaia. Signal and Image processing. Observatoire de Paris, 2008. English. tel-00340279v2 HAL Id: tel-00340279 https://tel.archives-ouvertes.fr/tel-00340279v2 Submitted on 21 Nov 2008 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. OBSERVATOIRE DE PARIS ECOLE´ DOCTORALE ASTRONOMIE ET ASTROPHYSIQUE D'^ILE-DE-FRANCE Thesis ASTRONOMY AND ASTROPHYSICS Instrumentation Shan Mignot Towards a demonstrator for autonomous object detection on board Gaia (Vers un demonstrateur pour la d´etection autonome des objets `abord de Gaia) Thesis directed by Jean Lacroix then Albert Bijaoui Presented on January 10th 2008 to a jury composed of: Ana G´omez GEPI´ - Observatoire de Paris President Bertrand Granado ETIS - ENSEA Reviewer Michael Perryman ESTEC - Agence Spatiale Europ´eenne Reviewer Daniel Gaff´e LEAT - Universit´ede Nice Sophia-Antipolis Examiner Michel Paindavoine LE2I - Universit´ede Bourgogne Examiner Albert Bijaoui Cassiop´ee- Observatoire de la C^ote d'Azur Director Gregory Flandin EADS Astrium SAS Guest Jean Lacroix LPMA - Universit´eParis 6 Guest Gilles Moury Centre National d'Etudes´ Spatiales Guest Acknowledgements The journey to the stars is a long one. -
ARIEL – 13Th Appleton Space Conference PLANETS ARE UBIQUITOUS
Background image credit NASA ARIEL – 13th Appleton Space Conference PLANETS ARE UBIQUITOUS OUR GALAXY IS MADE OF GAS, STARS & PLANETS There are at least as many planets as stars Cassan et al, 2012; Batalha et al., 2015; ARIEL – 13th Appleton Space Conference 2 EXOPLANETS TODAY: HUGE DIVERSITY 3700+ PLANETS, 2700 PLANETARY SYSTEMS KNOWN IN OUR GALAXY ARIEL – 13th Appleton Space Conference 3 HUGE DIVERSITY: WHY? FORMATION & EVOLUTION PROCESSES? MIGRATION? INTERACTION WITH STAR? Accretion Gaseous planets form here Interaction with star Planet migration Ices, dust, gas ARIEL – 13th Appleton Space Conference 4 STAR & PLANET FORMATION/EVOLUTION WHAT WE KNOW: CONSTRAINTS FROM OBSERVATIONS – HERSCHEL, ALMA, SOLAR SYSTEM Measured elements in Solar system ? Image credit ESA-Herschel, ALMA (ESO/NAOJ/NRAO), Marty et al, 2016; André, 2012; ARIEL – 13th Appleton Space Conference 5 THE SUN’S PLANETS ARE COLD SOME KEY O, C, N, S MOLECULES ARE NOT IN GAS FORM T ~ 150 K Image credit NASA Juno mission, NASA Galileo ARIEL – 13th Appleton Space Conference 6 WARM/HOT EXOPLANETS O, C, N, S (TI, VO, SI) MOLECULES ARE IN GAS FORM Atmospheric pressure 0.01Bar H2O gas CO2 gas CO gas CH4 gas HCN gas TiO gas T ~ 500-2500 K Condensates VO gas H2S gas 1 Bar Gases from interior ARIEL – 13th Appleton Space Conference 7 CHEMICAL MEASUREMENTS TODAY SPECTROSCOPIC OBSERVATIONS WITH CURRENT INSTRUMENTS (HUBBLE, SPITZER,SPHERE,GPI) • Precision of 20 ppm can be reached today by Hubble-WFC3 • Current data are sparse, instruments not absolutely calibrated • ~ 40 planets analysed -
The Spitzer Space Telescope and the IR Astronomy Imaging Chain
Spitzer Space Telescope (A.K.A. The Space Infrared Telescope Facility) The Infrared Imaging Chain Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 1/38 The infrared imaging chain Generally similar to the optical imaging chain... 1) Source (different from optical astronomy sources) 2) Object (usually the same as the source in astronomy) 3) Collector (Spitzer Space Telescope) 4) Sensor (IR detector) 5) Processing 6) Display 7) Analysis 8) Storage ... but steps 3) and 4) are a bit more difficult! Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 2/38 The infrared imaging chain Longer wavelength – need a bigger telescope to get the same resolution or put up with lower resolution Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 3/38 Emission of IR radiation Warm objects emit lots of thermal infrared as well as reflecting it Including telescopes, people, and the Earth – so collection of IR radiation with a telescope is more complicated than an optical telescope Optical image of Spitzer Space Telescope launch: brighter regions are those which reflect more light IR image of Spitzer launch: brighter regions are those which emit more heat Infrared wavelength depends on temperature of object Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 4/38 Atmospheric absorption The atmosphere blocks most infrared radiation Need a telescope in space to view the IR properly Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 5/38 -
The Sun As a Gravitational Lens : a Target for Space Missions a Target
“New Trends in Astrodynamics and Applications - V” Po litecn ico di Mil ano, Mil ano (It al y) , 30 J une, 1 -2 Ju ly 2008 The Sun as a Gravitational Lens : A Target for Space Missions Reaching 550 AU to 1000 AU Claudio Maccone Member of the International Academy of Astronautics Home Paggpe: http://www.maccone.com/ E-mail: [email protected] 1 Gravitational Lens of the Sun Figure 1: Basic geometry of the gravitational lens of the Sun: the minimal focal length at 550 AU and the FOCAL spacecraft position. 2 Gravitational Lens of the Sun • The geometry of the Sun gravitational lens is easily described: incoming electromagnetic waves (arriving, for instance, from the center of the Galaxy) pass outside the Sun and pass wihiithin a certain distance r of its center. • Then a basic result following from General Relativity shows that the corresponding dfltideflection angle ()(r) at the distance r from the Sun center is given by (Einstein, 1907): 4GM α (r ) = Sun . c 2 r 3 Gravitational Lens of the Sun • Let’s set the following parameters for the Sun: 1. Assumed Mass of the Sun: 1.9889164628 . 1030 kg, that is μSun = 132712439900 kg3s-2 2. Assumed Radius of the Sun: 696000 km 3. Sun Mean Density: 1408.316 kgm-3 4. Sc hwarzsc hild radi us of th e S un: 2 .953 k m One then finds the BASIC RESULT: MINIMAL FOCAL DISTANCE OF THE SUN: 548.230 AU ~ 3.17 light days ~ 13. 86 times th e Sun-to-Plut o di st ance. -
On the Verge of an Astronomy Cubesat Revolution
On the Verge of an Astronomy CubeSat Revolution Evgenya L. Shkolnik Abstract CubeSats are small satellites built in standard sizes and form fac- tors, which have been growing in popularity but have thus far been largely ignored within the field of astronomy. When deployed as space-based tele- scopes, they enable science experiments not possible with existing or planned large space missions, filling several key gaps in astronomical research. Unlike expensive and highly sought-after space telescopes like the Hubble Space Telescope (HST), whose time must be shared among many instruments and science programs, CubeSats can monitor sources for weeks or months at time, and at wavelengths not accessible from the ground such as the ultraviolet (UV), far-infrared (far-IR) and low-frequency radio. Science cases for Cube- Sats being developed now include a wide variety of astrophysical experiments, including exoplanets, stars, black holes and radio transients. Achieving high- impact astronomical research with CubeSats is becoming increasingly feasible with advances in technologies such as precision pointing, compact sensitive detectors, and the miniaturisation of propulsion systems if needed. CubeSats may also pair with the large space- and ground-based telescopes to provide complementary data to better explain the physical processes observed. A Disruptive & Complementary Innovation Fifty years ago, in December 1968, National Aeronautics and Space Admin- istration (NASA) put in orbit the first satellite for space observations, the Orbiting Astronomical Observatory 2. Since then, astronomical observation from space has always been the domain of big players. Space telescopes are arXiv:1809.00667v1 [astro-ph.IM] 3 Sep 2018 usually designed, built, launched and managed by government space agencies such as NASA, the European Space Agency (ESA) and the Japan Aerospace School of Earth and Space Exploration; Interplanetary Initiative { Arizona State Univer- sity, Tempe, AZ 85287.