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High-Contrast Imaging at TMT Gas giants, ice-giants, terrestrial planets, exomoons, polarization, transits, weather, surface mapping, biomarkers, disks, planet formation, … High-Contrast/ExAO breakout session Stanimir Metchev, UWO S. Sengupta O. Guyon O. Guyon PSI PFIX • Drivers: characteriza.on of exoplanets in reflected light and thermal emission • Goal: Biosignatures on terrestrial planets in nearby HZs • Constraining composi.on and forma.on pathways • Circumstellar disks, solar system objects, AGB star ouFlows • General-purpose 2.5-5 um imaging, spectroscopy capabili.es not in first-light instruments • Modularity • Core capabili.es support different science instruments • Upgrade paths to accommodate new technology • Fiber feeds allow straighForward use of instruments deployed and tested on smaller telescopes • Rela.vely compact • Diffrac.on-limited, narrow field-of-view op.cs • Allows for phased development and deployment PSI concept PSI-Green PSI-Red PSI-Blue PSI-Red Woofer DM Cold Vis WFS IR WFS Coronagraph Tweeter Coronagraph DM 8-13 μm Imager Cold 0.6-1.8 μm Coronagraph IFU/Imager 0.6-1.8 μm High-Res 2-5 μm 2-5 μm High-Res IFU/Imager A. Skemer Theral ImagingAlpha of Cent Exoplanets A & B with TMT 8m 30m A Exo-Earth exo-Venus exo-Jupiter exo-Earth B exo-Mars 100h 8m 25h TMT (Chile) C. Marois, NRC-H But also more systems! Proxima Centauri Alpha Cent A Sensitivity limit 8m Alpha Cent B Epsilon Eridani ? Procyon 61 Cygni A 61 Cygni B Epsilon Indi A ? Tau Ceti Sensitivity Groombridge 1618 limit 30m ? Resolution limit 6m Resolution limit 30m Resolution limit 8m C. Marois, NRC-H E. Artigau Discussions • Polarization • Synergy with MICHI (blue MICHI/“Green” PSI) & MIRAO • ASM discussions & requirements • Cooling AO bench for MIRAO? • Parallel observing (blue, green, red PSI). • Expending science team (solar system, BDs, others)? • WP strategy.

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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,
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A Joint ESA-CONSTELLATION Workshop on the Formation of Brown Dwarfs
-ESA- Space Science Faculty Courtesy NASA/JPL-Caltech CONSTELLATION is a European Commission Sixth Framework Marie Curie Research Training Network (contract number MRTN-CT-2006-035890) A joint ESA-CONSTELLATION workshop on the formation of brown dwarfs Contact info: [email protected]! www.rssd.esa.int/BD2009 Gemini Observatory/AURA WORKSHOP Recipes for making brownies: theory vs. observations Scientific Rationale: The origin of Brown Dwarfs (BDs) is an important component of the theory of star formation. Recent ground based and satellite observations are revealing an increasing number of BDs; however, their origin remains somewhat mysterious as their mass is 2 orders of magnitude below the average Jeans mass in star-forming clouds. Explaining why they are so common thus requires detailed understanding of the fragmentation processes during star formation, as well as exploring other formation scenarios. This workshop will focus on recent theoretical and observational progresses in the field of BD formation as well as explore current and future perspectives. Our purpose is to bring together the leading experts working in this field, foster new collabora- tions and, in particular, promote extended interactions among young PhD/post-doc researchers. SOC: L. Spezzi (chair, ESTEC) B. Mer´ın(ESAC) D. Stamatellos (University of Cardiff) V. Konyves (CEA/Saclay,SAp) C. Alves de Oliveira (LAOG, Grenoble) LOC: L. Spezzi (co-chair) J. Walcher (co-chair) G. Beccari Program: 9 September 2009 08:30 - 10:00 Registration + Coffee 10:00 - 10:15 Opening 10:15 - 11:00 I. Bonnell, BD formation, an introductory review Session 1: Observations of BDs Chairman: E. Mouraux 11:00 - 11:30 K.
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Starshade Rendezvous Probe
Starshade Rendezvous Probe Starshade Rendezvous Probe Study Report Imaging and Spectra of Exoplanets Orbiting our Nearest Sunlike Star Neighbors with a Starshade in the 2020s February 2019 TEAM MEMBERS Principal Investigators Sara Seager, Massachusetts Institute of Technology N. Jeremy Kasdin, Princeton University Co-Investigators Jeff Booth, NASA Jet Propulsion Laboratory Matt Greenhouse, NASA Goddard Space Flight Center Doug Lisman, NASA Jet Propulsion Laboratory Bruce Macintosh, Stanford University Stuart Shaklan, NASA Jet Propulsion Laboratory Melissa Vess, NASA Goddard Space Flight Center Steve Warwick, Northrop Grumman Corporation David Webb, NASA Jet Propulsion Laboratory Study Team Andrew Romero-Wolf, NASA Jet Propulsion Laboratory John Ziemer, NASA Jet Propulsion Laboratory Andrew Gray, NASA Jet Propulsion Laboratory Michael Hughes, NASA Jet Propulsion Laboratory Greg Agnes, NASA Jet Propulsion Laboratory Jon Arenberg, Northrop Grumman Corporation Samuel (Case) Bradford, NASA Jet Propulsion Laboratory Michael Fong, NASA Jet Propulsion Laboratory Jennifer Gregory, NASA Jet Propulsion Laboratory Steve Matousek, NASA Jet Propulsion Laboratory Jonathan Murphy, NASA Jet Propulsion Laboratory Jason Rhodes, NASA Jet Propulsion Laboratory Dan Scharf, NASA Jet Propulsion Laboratory Phil Willems, NASA Jet Propulsion Laboratory Science Team Simone D'Amico, Stanford University John Debes, Space Telescope Science Institute Shawn Domagal-Goldman, NASA Goddard Space Flight Center Sergi Hildebrandt, NASA Jet Propulsion Laboratory Renyu Hu, NASA
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The Hertzsprung - Russell Diagram Today You Will Be Making the Hertzsprung - Russell Diagram
Name: ___________________________________ The Hertzsprung - Russell diagram Today you will be making the Hertzsprung - Russell diagram. The H-R diagram allows astronomers to classify stars into groups. The two axes for this graph will be temperature and magnitude. When we refer to temperature, we are talking about the surface of the star. The surface temperature is much cooler. For example, our sun’s surface temperature is ~5,500K to 6,000 K. Kelvin is a temperature scale very similar to Celsius. Absolute magnitude is a measurement of how bright a star really is. This is determined by its size and by its temperature. Even though it might look bright in our sky, we try to compare all stars as if we were standing the exact same distance away from each one. This magnitude value is stated by calculating how bright the object would shine at a fixed distance away in space, ~32.6 light years (10 parsecs for those wanting another measurement to think about). Main sequence stars Temperature Magnitude Red Giant stars Temperature Magnitude Bellatrix 18000 -2.0 Capella 5000 -0.6 Regulus 12000 -0.6 Pollux 4650 0.8 Spica 19500 -2.0 Arcturus 4500 -0.3 Beta Centauri 21000 -3.0 Aldebaran 3900 -0.2 Achernar 16500 -3.0 Beta Tauri 12000.0 -2 Beta Crucis 21000.0 -3.9 Red Super Giant Alpha Crucis 19500.0 -4 Rigel 11000 -6.8 Vega 9750 0.5 Deneb 8500 -6.9 Castor 9250 0.9 Canopus 7400 -3.1 Beta Carinae 9750.0 -0.4 Antares 3500 -4.5 Sirius A 9250.0 1.5 Betelgeuse 3200 -5.5 Formalhaut 8500 2.0 Altair 7750 2.2 White Dwarfs Procyon A 6500 2.6 Sirius B 8100 11.4 Alpha Centauri A 5750 4.4 Procyon B 6500 13.1 Sun 5750 4.9 Tau Ceti 5344 5.7 Epsilon Eridani 4500 6.1 Epsilon Indi 4250 7 Cygni A 3800 7.5 Cygni B 3700 8 Alpha Centauri B 3900 5.8 Kapteyn's Star 3400 11.2 Lacaille 8760 3200 8.8 Lacaille 21185 3000 10.5 Bernard's Star 2600 13.2 Ross 614A 2500 13.3 Kruger 60B 2500 13.4 Ross 248 2800 14.7 Use the data on the previous page to plot an H-R diagram.
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Another Unit of Distance (I Like This One Better): Light Year
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UNSC Science and Technology Command
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Astrophysics P3 SL [152 Marks]
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Space Resources for Teachers, Space Science, a Guide Outlining Understandings, Fundamental Concepts, and Activities
DOCUMENT RESUME ED 040 047 SE 008 196 !,,ITHOR Thompson, Malcolm TTI,Lr Space Resources for Teachers,Space Science, A Guide Outlining Understandings, FundamentalConcepts, and Activities. INSTITUTION Columbia Univ., New York,N.Y.; National Aeronautics and Space Administration, NewYork, N. Y. Goddard Inst. for Space Studies. PUB DATE 69 NOTE 145p. AVAILABLE FROM Superintendent of Documents,U.S. Government Printing Office, Washington,D.C. 20402 (0-358-779, $2.00) 'DRS PRICE EDRS Price MF -$0.75 HC Not Availablefrom EDRS. DESCRIPTORS *Aerospace Technology, AnnotatedBibliographies, *Astronomy, *College Science,*Instructional Materials, Physical Sciences,Science Activities, *Secondary School Science, TeachingGuides ABSTRACT This instructional andresource guide is designedso that it may be used in thesecondary school or in the firsttwo years of college to presenta series of units in space science,or to supplement existing science andmathematics courses. The guide consists of six units:(1) mea.surement, distance, andsize in astronomy,(2) atoms, spectra, andstars,(3) atomic nuclei and stars,(4) the solar system, (5) the originand evaluation of life, and (6) motion, rockets and gravity.Each unit is divided into the following parts: (a) a list of understandings thata student should have after completing study ofthe unit, (b) a topical outline of the material in the unit, withexpositions, tables, demonstrations,and activities inserted when appropriate,(0 a list of sample questions, (d) problems and projects forfurther exploration,(e) audiovisual aids, (f) an annotated teacher bibliography and (g) an annotated student bibliography. Each of theunits is basically self-contained. However, in general they require additionalknowledge which may be obtained by a study of the earlierunits, from the context of another course, or by a study of the material listedin the bibliographies.
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Curriculum Vitae Date: 4/03/2013 Initials
Curriculum Vitae Date: 4/03/2013 Initials: Gordon Arthur Hunter WALKER Born: 30 January 1936 Married: Sigrid Helene Fischer, April 1962 Children: Nicholas and Eric Languages: English, French, and German. POST-SECONDARY EDUCATION University of Edinburgh Hon.B.Sc. Natural Philosophy 1958 University of Cambridge (Caius) Ph.D. Astrophysics 1962 PROFESSIONAL EMPLOYMENT Radcliffe Observatory, Pretoria Research Assistant 1960-61 DAO, Victoria NRC Fellow 1962-63 DAO, Victoria Scientific Officer 3 1963-69 University of Texas Visiting Lecturer 1965 (Spring) University of Victoria Visiting Lecturer 1966 (Spring) UBC Associate Professor April 1, 1969 Director, Institute 1972-78 Astronomy and Space Science Professor July 1, 1974-97 Professor Emeritus July 1 1997 { HIA/NRC Guest-worker 1998 { UVic Adjunct Professor April 23 2004 { INTERNATIONAL PROJECTS Scientific Advisory Committee of the CFHT 1972-79 Project Scientist for `Starlab' an Australian, Canadian, NASA, space telescope proposal until Canada withdrew in 1984 CFHT Board of Directors 1986-91 Canadian Project Scientist (1989-90): EUVITA - far ultraviolet astronomical satellite experiment joint with USSR, Switzerland, USA. Canadian Project Scientist (1990{97): Gemini - twin 8 metre optical telescopes (1 in Hawaii, 1 in Chile) joint with USA, U.K., Chile, Australia, Argentina, Brazil. Gemini Scientific Advisory Committee 1991{97 Gemini Board of Directors 1991{97 1 MOST Science team (1997{2009): a Canadian satellite launched in 2003 for ultra-precise photom- etry of bright stars, with collaboration from Austria. Gemini/NSF Visiting Committee 2004 AURA Source Selection Board for future Gemini Instrumentation 2004 TMT - chair HROS Review Panel 2005 chair Gemini Source Selection Board for HRNIRS 2005 chair Gemini Source Selection Board for PRVS 2006 member SPIRou Preliminary Design Revue Committee 2012 - a high resolution visible/infrared spectropolarimeter proposed for CFHT RESEARCH CAREER My fascination with astronomy began at age 7 when my father explained that stars were very distant suns.
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Extrasolar Planets and Their Host Stars
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Curriculum Vitae
Curriculum Vitae Prof. Dr. Kevin Heng University of Bern Center for Space and Habitability Gesellschaftsstrasse 6, CH-3012, Bern, Switzerland http://www.kevinheng.com Research Interests Theory, simulation and phenomenology of exoplanetary atmospheres: radiative transfer, chemistry, inversion methods, ﬂuid dynamics. Analytical methods. Applications of machine learning, statistics and high performance computing. Exoplanet science for CHEOPS, TESS, HST, JWST and LUVOIR missions. Habitability: geochemical cycles and biosignatures. Pedagogy and epistemology. Epidemiology. Science writing. Group Leader: Exoplanets & Exoclimes Group (5 postdocs, 4 Ph.D students, 1 Master student). Center Director: two fellowship programs (10 independent fellows). 1. Training, Education and Awards 1.1. Academic Positions 2022 onwards: Chair Professor (Lehrstuhlinhaber)1 of Theoretical Astrophysics of Extrasolar Planets, Ludwig Maximilian University of Munich 2016–2022: Executive Director, Center for Space and Habitability, University of Bern 2015–2022: Professor2 of Astronomy & Planetary Science, University of Bern 2013–2015: Tenure-Track Assistant Professor, University of Bern 2010–2012: Zwicky Prize Fellow, ETH Zurich,¨ Institute for Astronomy 2009–2010: Frank & Peggy Taplin Member, Institute for Advanced Study at Princeton 2007–2009: Member, Institute for Advanced Study at Princeton 1.2. Honorary/Visiting Positions 2020–2022: Honorary Professor3, University of Warwick 2017: Visiting Professor4, Johns Hopkins University 2007: Visitor, Max Planck Institutes for Astrophysics (MPA) and Extraterrestrial Physics (MPE) 1.3. Education 2007: Ph.D, astrophysics, JILA and University of Colorado at Boulder 2006: Chef Track Diploma, Culinary School of the Rockies5, Colorado 2005: M.S., astrophysics, JILA and University of Colorado at Boulder 2003: B.Sc (Hons), physics, National University of Singapore Email address: [email protected], [email protected] (Prof.
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