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Gaia and WEAVE/Wxes: Supporting the PLATO Exoplanet Hunter Nicholas Walton Institute of Astronomy University of Cambridge
Gaia and WEAVE/WxES: supporting The PLATO Exoplanet Hunter Nicholas Walton Institute of Astronomy University of Cambridge WEAVE – Gaia – PLATO a winning planet hunter combo • Gaia releases its first all sky astrometric catalogues late 2017 • WEAVE begins on sky operations in 2018 • PLATO begins its planet hunt in 2024 • Why are these events linked? • Finding and characterising extra solar planets requires a detailed knowledge of the host stars • And it helps to know your target stars before you observe them 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 2 PLATO set for 2024 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 3 … but first … Gaia’s role in planets Recall Carme Jordi’s talk earlier this week 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 4 Gaia launched 19 Dec 2013 a powerful complement to PLATO NGC 1818 in LMC 212x212 arcsec2 (~1% of AF FoV) 2.85s integration time 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 5 Gaia End-of-Mission Parallax Errors Apply factors of ~ 0.7 and ~ 0.5 for positions and proper motions Figure from http://www.rssd.esa.int/index.php?project=GAIA&page=Science_Performance Non-uniformity over the sky: 2 70% – 116% 1 PLATO stars 1. bright-star regime (calibration errors, CCD saturation) 2. photon-noise regime, with sky-background noise and electronic noise setting in around G ~ 20 mag (equivalent to V = 20 to 22) 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 6 Gaia Performance (at IOCR) http://www.cosmos.esa.int/web/gaia/science-performance Typical -
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. -
Graham Pointer Phd Thesis
THE MAGNETIC FIELD OF AB DORADÛS Graham Richard Pointer A Thesis Submitted for the Degree of PhD at the University of St Andrews 2001 Full metadata for this item is available in St Andrews Research Repository at: http://research-repository.st-andrews.ac.uk/ Please use this identifier to cite or link to this item: http://hdl.handle.net/10023/12940 This item is protected by original copyright THE UNIVERSITY OF ST. ANDREWS The Magnetic Field of AB Doradûs Graham Richard Pointer Submitted for the degree of Ph.D. May 2001 ProQuest Number: 10171062 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a com plete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest ProQuest 10171062 Published by ProQuest LLO (2017). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States C ode Microform Edition © ProQuest LLO. ProQuest LLO. 789 East Eisenhower Parkway P.Q. Box 1346 Ann Arbor, Ml 48106- 1346 DECLARATION I, Graham Richard Pointer, hereby declare that this thesis, which is approximately 50000 words in length, has been written by me, that it is the record of work carried out by me and that it has not been submitted in any previous application for a higher degree. I was admitted as a research student in September 1997 and as a candidate for the degree of Ph.D . -
Position Angles and Coplanarity of Multiple Systems from Transit Timing (Research Note)
A&A 561, A51 (2014) Astronomy DOI: 10.1051/0004-6361/201321070 & c ESO 2013 Astrophysics Position angles and coplanarity of multiple systems from transit timing (Research Note) Aviv Ofir Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany e-mail: [email protected] Received 9 January 2013 / Accepted 4 September 2013 ABSTRACT Aims. We compare the apparent difference in timing of transiting planets (or eclipsing binaries) that are observed from widely sepa- rated locations (parallactic delay). Methods. A simple geometrical argument allows us to show that the apparent timing difference also depends on the sky position angle of the planetary (or secondary) orbit, relative to the ecliptic plane. Results. Our calculation of the magnitude of the effect for all currently known planets (should they exhibit transits) find that al- most 200 of them – mostly radial-velocity detected planets – have predicted timing effects greater than 1 s. We also compute the theoretical timing precision for the PLATO mission, which will observe a similar stellar population and find that a 1 s effect will frequently be easily observable. We also find that the sky coplanarity of multiple objects in the same system can be probed more easily than the sky position angle of each of the objects separately. Conclusions. We show that a new observable from transit photometry becomes available when very high-precision transit timing is available. We find that there is a good match between projected capabilities of the future space missions PLATO and CHEOPS and the new observable. We specify some initial science questions that this new observable may be able to address. -
Arxiv:1809.10688V2 [Astro-Ph.EP] 26 Jun 2019 Ing Nearby Bright Stars (Howell Et Al
Preprint typeset using LATEX style emulateapj v. 12/16/11 A DISCRETE SET OF POSSIBLE TRANSIT EPHEMERIDES FOR TWO LONG PERIOD GAS GIANTS ORBITING HIP 41378 Juliette C. Becker1, Andrew Vanderburg2;?, Joseph E. Rodriguez3, Mark Omohundro4, Fred C. Adams1;5, Keivan G. Stassun6;7, Xinyu Yao8, Joel Hartman9, Joshua Pepper8, Gaspar Bakos9, Geert Barentsen10, Thomas G. Beatty11, Waqas Bhatti8, Ashley Chontos12, Andrew Collier Cameron13, Coel Hellier14, Daniel Huber12, David James3, Rudolf B. Kuhn15, Michael B. Lund6, Don Pollacco16, Robert J. Siverd6, Daniel J. Stevens11;17;18, Jose´ Vin´ıcius de Miranda Cardoso19, Richard West16, 1Astronomy Department, University of Michigan, 1085 S University Avenue, Ann Arbor, MI 48109, USA 2Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 3Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA 4Citizen Scientist 5Physics Department, University of Michigan, Ann Arbor, MI 48109, USA 6Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN:37235, USA 7Department of Physics, Fisk University, 1000 17th Avenue North, Nashville, TN:37208, USA 8Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA 9Department of Astrophysical Sciences, 4 Ivy Lane, Princeton University, Princeton, NJ 08544 10NASA Ames Research Center, Moffett Blvd, Mountain View, CA 94035, USA 11Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 -
Cosmic Evolution Through Uv Surveys (Cetus) Final Report
COSMIC EVOLUTION THROUGH UV SURVEYS (CETUS) FINAL REPORT Thematic Activity: Project (probe mission concept) Program: Electromagnetic observations from space Authors of Final Report: Jonathan Arenberg, Northrop Grumman Corporation Sally Heap, Univ. of Maryland, [email protected] Tony Hull, Univ. of New Mexico Steve Kendrick, Kendrick Aerospace Consulting LLC Bob Woodruff, Woodruff Consulting Scientific Contributors: Maarten Baes, Rachel Bezanson, Luciana Bianchi, David Bowen, Brad Cenko, Yi-Kuan Chiang, Rachel Cochrane, Mike Corcoran, Paul Crowther, Simon Driver, Bill Danchi, Eli Dwek, Brian Fleming, Kevin France, Pradip Gatkine, Suvi Gezari, Lea Hagen, Chris Hayward, Matthew Hayes, Tim Heckman, Edmund Hodges-Kluck, Alexander Kutyrev, Thierry Lanz, John MacKenty, Steve McCandliss, Harvey Moseley, Coralie Neiner, Goren Östlin, Camilla Pacifici, Marc Rafelski, Bernie Rauscher, Jane Rigby, Ian Roederer, David Spergel, Dan Stark, Alexander Szalay, Bryan Terrazas, Jonathan Trump, Arjun van der Wel, Sylvain Veilleux, Kate Whitaker, Isak Wold, Rosemary Wyse Technical Contributors: Jim Burge, Kelly Dodson, Chip Eckles, Brian Fleming, Jamie Kennea, Gerry Lemson, John MacKenty, Steve McCandliss, Greg Mehle, Shouleh Nikzad, Trent Newswander, Lloyd Purves, Manuel Quijada, Ossy Siegmund, Dave Sheikh, Phil Stahl, Ani Thakar, John Vallerga, Marty Valente, the Goddard IDC/MDL. September 2019 Cosmic Evolution Through UV Surveys (CETUS) TABLE OF CONTENTS INTRODUCTION TO CETUS ................................................................................................................ -
Cosmic Vision and Other Missions for Space Science in Europe 2015-2035
Cosmic Vision and other missions for Space Science in Europe 2015-2035 Athena Coustenis LESIA, Observatoire de Paris-Meudon Chair of the Solar System and Exploration Working Group of ESA Member of the Space Sciences Advisory Committee of ESA Cosmic Vision 2015 - 2025 The call The call for proposals for Cosmic Vision missions was issued in March 2007. This call was intended to find candidates for two medium-sized missions (M1, M2 class, launch around 2017) and one large mission (L1 class, launch around 2020). Fifty mission concept proposals were received in response to the first call. From these, five M-class and three L- class missions were selected by the SPC in October 2007 for assessment or feasibility studies. In July 2010, another call was issued, for a medium-size (M3) mission opportunity for a launch in 2022. Also about 50 proposals were received for M3 and 4 concepts were selected for further study. Folie Cosmic Vision 2015 - 2025 The COSMIC VISION “Grand Themes” 1. What are the conditions for planetary formation and the emergence of life ? 2. How does the Solar System work? 3. What are the physical fundamental laws of the Universe? 4. How did the Universe originate and what is it made of? 4 COSMIC VISION (2015-2025) Step 1 Proposal selection for assessment phase in October 2007 . 3 M missions concepts: Euclid, PLATO, Solar Orbiter . 3 L mission concepts: X-ray astronomy, Jupiter system science, gravitational wave observatory . 1 MoO being considered: European participation to SPICA Selection of Solar Orbiter as M1 and Euclid JUICE as M2 in 2011. -
2014 Science with the Hubble Space
Beyond HST: The Universe in High-Definition – UVOIR Space Astronomy in 2030 Julianne Dalcanton & Marc Postman Science with HST IV Meeting Rome, Italy March 18, 2014 Long History of Large Space UVOIR Telescope Concepts • VLST – 10m-16m concept (ca. 1989) • SUVO – 4m concept (ca. 1998-1999) • Workshop on 10m - 30m VLST (2003) • MUST – 10m concept (ca. 2004-2005) • ATLAST – 8m-16m concepts (ca. 2008-2010) • EUVO – European 8m concept (ca. 2013) • Modular Assembled 20m concept (ca. 2013) Scientifically compelling for over 2 decades! (Average Aperture Diameter – 13.5 meters) “Can we find another planet like Earth orbiting a nearby star? To find such a planet would complete the revolution, started by Copernicus nearly 500 years ago, that displaced the Earth as the center of the universe… The observational challenge is great but armed with new technologies… astronomers are poised to rise to it.” - U.S. 2010 Astronomy Decadal Review This is a question whose answer is sought by all of humanity and the search will demand international cooperation. The path has been laid ! for characterizing Earth 2.0 Kepler Hubble Spitzer CoRoT Ground-based Coronagraphs Gaia WFIRST 30-m class telescopes TESS JWST PLATO !"#$%&'('$)*+%&'($,)(%&$+-%$%&'('./$ Thick Atmosphere Methane Oxygen Fraction with terrestrial planets = !Earth FractionWater with detectable biosignature = fBio OpticalIf : ! Near-Infrared $ f ~ 1 then D ~ 4m Earth Bio0'12'($('#-2%#$ 8-meterTel 16-meter The signature of life is encoded inf the < 1 then D 8m spectrum! Earthof the Earth$ Bio $ tel ~ 70 !Earth $ fBio << 1 then DTel ~ 16m a > 12 Earths $ 60 50 40 30 # 4 Earths 20 4-meter 10 of total integration time of total integration time 0 Above: Distribution of all FGK stars within 45 pc of the Sun Number of Exo-Earths in 1 year 2-m 4-m 8-m 16-m where a R=70 spectrum of an Earth-twin could be acquired Telescope Size in <500 ksec shown as a function of telescope aperture. -
PLATO Revealing Habitable Worlds Around Solar-Like Stars
ESA-SCI(2017)1 April 2017 PLATO Revealing habitable worlds around solar-like stars Definition Study Report European Space Agency PLATO Definition Study Report page 2 The front page shows an artist’s impression reflecting the diversity of planetary systems and small planets expected to be discovered and characterised by PLATO (©ESA/C. Carreau). PLATO Definition Study Report page 3 PLATO Definition Study – Mission Summary Key scientific Detection of terrestrial exoplanets up to the habitable zone of solar-type stars and goals characterisation of their bulk properties needed to determine their habitability. Characterisation of hundreds of rocky (including Earth twins), icy or giant planets, including the architecture of their planetary system, to fundamentally enhance our understanding of the formation and the evolution of planetary systems. These goals will be achieved through: 1) planet detection and radius determination (3% precision) from photometric transits; 2) determination of planet masses (better than 10% precision) from ground-based radial velocity follow-up, 3) determination of accurate stellar masses, radii, and ages (10% precision) from asteroseismology, and 4) identification of bright targets for atmospheric spectroscopy. Observational Ultra-high precision, long (at least two years), uninterrupted photometric monitoring in the concept visible band of very large samples of bright (V ≤11-13) stars. Primary data High cadence optical light curves of large numbers of bright stars. products Catalogue of confirmed planetary systems fully characterised by combining information from the planetary transits, the seismology of the planet-host stars, and the ground-based follow-up observations. Payload Payload concept • Set of 24 normal cameras organised in 4 groups resulting in many wide-field co-aligned telescopes, each telescope with its own CCD-based focal plane array; • Set of 2 fast cameras for bright stars, colour requirements, and fine guidance and navigation. -
The PLATO Payload and Data Processing System Spacewire
The PLATO Payload and Data Processing System SpaceWire network Mauro Focardi Rosario Cosentino Stefano Pezzuto INAF-OAA INAF-FGG INAF-IAPS Arcetri Astrophysical Observatory Galileo Galilei Foundation Inst. of Space Astrophysics and Planetology Firenze, Italy La Palma - Canary Islands, Spain Roma, Italy [email protected] [email protected] [email protected] David Biondi Giovanni Giusi Luca Serafini INAF-IAPS INAF-IAPS KI Inst. of Space Astrophysics and Planetology Inst. of Space Astrophysics and Planetology Kayser Italia Roma, Italy Roma, Italy Livorno, Italy [email protected] [email protected] l.serafi[email protected] Carlo Del Vecchio Blanco Donatella Vangelista Matteo Rotundo KI KI Department of Information Engineering Kayser Italia Kayser Italia University of Pisa Livorno, Italy Livorno, Italy Pisa, Italy [email protected] [email protected] [email protected] Luca Fanucci Daniele Davalle and the PLATO DPS Team Department of Information Engineering IngeniArs coordinated by DLR University of Pisa IngeniArs S.r.l German Aerospace Center Pisa, Italy Pisa, Italy Berlin, Germany [email protected] [email protected] Abstract—PLATO [1] has been selected and adopted by ESA conceived for the study of planetary systems formation and as the third medium-class Mission (M3) of the Cosmic Vision evolution and to answer fundamental questions concerning the Program, to be launched in 2026 with a Soyuz-Fregat rocket existence of other planetary systems like our own, including from the French Guiana. Its Payload (P/L) is based on a suite of 26 telescopes and cameras in order to discover and the presence of new worlds in the habitable zone of Sun- characterise, thanks to ultra-high accurate photometry and the like stars. -
EPSC2018-1115-2, 2018 European Planetary Science Congress 2018 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2018
EPSC Abstracts Vol. 12, EPSC2018-1115-2, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Ultra-short Period Rocky Super-Earths Luca Malavolta (1,2) , Andrew W. Mayo (3,4) , Tom Louden (5) , Vinesh M. Rajpaul (6) , Aldo S. Bonomo (7) , Lars A. Buchhave (4) , Laura Kreidberg (3,8) , Martti H. Kristiansen (9,10), Mercedes Lopez-Morales (3) , Annelies Mortier (11) , Andrew Vanderburg (3,12) , Adrien Coffinet (13), David Ehrenreich (13) , Christophe Lovis (13), Francois Bouchy (13), David Charbonneau (3) , David R. Ciardi (14), Andrew Collier Cameron (11) , Rosario Cosentino (15), Ian J. M. Crossfield (16,17), Mario Damasso (7) , Courtney D. Dressing (18) , Xavier Dumusque(13) , Mark E. Everett (19) , Pedro Figueira (20), Aldo F. M. Fiorenzano (15), Erica J. Gonzales (16,28), Raphaëlle D. Haywood (3,27) , Avet Harutyunyan (15), Lea Hirsch (18) , Steve B. Howell (21) , John Asher Johnson (3) , David W. Latham (3) , Eric Lopez (22), Michel Mayor (13), Giusi Micela (23), Emilio Molinari (15,24) , Valerio Nascimbeni (1,2) , Francesco Pepe (13), David F. Phillips (3) , Giampaolo Piotto (1,2) , Ken Rice (25), Dimitar Sasselov (3) , Damien Ségransan (13) , Alessandro Sozzetti (7) , Stéphane Udry (13), and Chris Watson (26) (1) Dipartimento di Fisica e Astronomia “Galileo Galilei,” Università di Padova, Italy ([email protected]) (2) INAF— Osservatorio Astronomico di Padova, Italy (3) Harvard-Smithsonian Center for Astrophysics, USA (4) Centre for Star and Planet Formation, Denmark (5) Department -
View of Earth’S Magnetosphere
Science Committee Report Dr. Byron Tapley, Vice Chair Science Committee Members Wes Huntress, Chair Byron Tapley, (Vice Chair) University of Texas-Austin, Chair of Earth Science Alan Boss, Carnegie Institution, Chair of Astrophysics Ron Greeley, Arizona State University, Chair of Planetary Science Gene Levy, Rice University, Chair of Planetary Protection Roy Torbert, University of New Hampshire, Chair of Heliophysics Noel Hinners, Independent Consultant Michael Turner, University of Chicago Charlie Kennel, Chair of Space Studies Board (ex officio member) 2 Agenda • Science Results • Programmatic Status • Findings & Recommendations 3 ICESCAPE 2010 MODIS Aqua July 8, 2010 June 23, Chukchi Sea 2010 Sampled optically complex waters (cruise track in blue) • Phytoplankton • CDOM • Some sediments Very productive ecosystem Phytoplankton biomass highly variable • Spatially • Temporally Even higher concentrations of phytoplankton just below sea surface (20-50 m) • Among highest in world Brown = land Gray = sea ice Chlorophyll a 0.01 0.1 1 10 4 30 GRIP Aircraft Coordination Coordination of a combined 5 NASA and NOAA aircraft in Hurricane Karl on 16 September 2010 at ~1955 UTC NASA’s Interstellar Boundary Explorer (IBEX) Spacecraft Reveals A New View of Earth’s Magnetosphere • Since its October 2008 launch, NASA's IBEX spacecraft has mapped the invisible interactions occurring at the edge of the solar system. The images reveal that the interactions between our home in the galaxy and interstellar space are surprisingly structured and intense. • Recently,