Appendix C Common Abbreviations & Acronyms
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EOOS Posters Abstracts
Posters Submissions – EOOS Conference 21 23 November 2018 1. Sylvie Pouliquen Ifremer [email protected] Authors: "Gille Reverdin CNRS/INSU email: [email protected] , Pierre-Yves Le Traon Ifremer & Mercator-Ocean email: [email protected]) and the Coriolis 2014-2020 steering committee." Theme: From standalone to integrated ocean and coastal observing platforms Title: Coriolis: an integrated in-situ ocean observation infrastructure for operational oceanography and ocean/climate research "The Coriolis (www.coriolis.eu.org) structure gathers efforts of seven French institutes (CNES, CNRS, IFREMER, IPEV, IRD, Météo-France, SHOM, CEREMA) to organize the in-situ component of the French operational oceanography infrastructure. The objective is to organize the data acquisition and real- time/delayed mode data processing of in-situ measurements required for operational oceanography and ocean/climate research. Coriolis is focused on a limited number of physical and biogeochemical parameters that are acquired systematically and in real time or slightly delayed mode. Coriolis follows a fully open data policy. The framework of collaboration for Coriolis was renewed in 2014 and now covers the time period of 2014 up to 2020. By signing this new agreement, the eight directors of French institutes have clearly stated their willingness to sustain and consolidate further the Coriolis in-situ infrastructure. The new framework agreement strengthens the links between research and operational oceanography. The scope is also extended to integrate the main French contributions to the global and regional in-situ observing systems: Argo, gliders, research vessels, ship of opportunities, drifting buoys, marine mammals, tidal networks and high frequency coastal observatories. -
Overview and Status of the Giant Magellan Telescope Project
Invited Paper Overview and Status of the Giant Magellan Telescope Project Patrick J. McCarthy*,a,b, James Fansona, Rebecca Bernsteina,b, David Ashbyc, Bruce Bigelowa, Nune Boyadjiana, Antonin Boucheza, Eric Chauvina, Eduardo Donosoa, Jose Filgueiraa, Robert Goodricha, Frank Groarka, George Jacobya, Eric Pearcea aGMTO Corporation, 451 N. Halstead St., Suite 250, Pasadena, CA 91107, USA bCarnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101, USA cLarge Binocular Telescope Observatory, Tucson AZ ABSTRACT The Giant Magellan Telescope Project is in the construction phase. Production of the primary mirror segments is underway with four of the seven required 8.4m mirrors at various stages of completion and materials purchased for segments five and six. Development of the infrastructure at the GMT site at Las Campanas is nearing completion. Power, water and data connections sufficient to support the construction of the telescope and enclosure are in place and roads to the summit have been widened and graded to support transportation of large and heavy loads. Construction pads for the support buildings have been graded and the construction residence is being installed. A small number of issues need to be resolved before the final design of the telescope structure and enclosure can proceed and the GMT team is collecting the required inputs to the decision making process. Prototyping activities targeted at the active and adaptive optics systems are allowing us to finalize designs before large scale production of components begins. Our technically driven schedule calls for the telescope to be assembled on site in 2022 and to be ready to receive a subset of the primary and secondary mirror optics late in the year. -
1 Director's Message
1 Director’s Message Laura Ferrarese 3 Rocky Planet Engulfment Explains Stellar Odd Couple Carlos Saffe 7 Astronomers Feast on First Light From Gravitational Wave Event Peter Michaud 11 Science Highlights Peter Michaud 15 On the Horizon Gemini staff contributions 18 News for Users Gemini staff contributions ON THE COVER: GeminiFocus October 2017 Gemini South provided critical GeminiFocus is a quarterly publication observations of the first of the Gemini Observatory electromagnetic radiation from 670 N. A‘ohoku Place, Hilo, Hawai‘i 96720, USA a gravitational wave event. / Phone: (808) 974-2500 / Fax: (808) 974-2589 (See details starting on page 7.) Online viewing address: www.gemini.edu/geminifocus Managing Editor: Peter Michaud Associate Editor: Stephen James O’Meara Designer: Eve Furchgott/Blue Heron Multimedia Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation or the Gemini Partnership. ii GeminiFocus October 2017 Laura Ferrarese Director’s Message The Three Goals of a Year-long Vision Hello, Aloha, and Hola! I am delighted to address the Gemini community from my new role as the Observatory’s Interim Director. I will hold this position for the next year, while the search for a perma- nent Director moves forward. As I write this (beginning of September), I have been in Hilo, Hawai‘i, for almost two months, and it’s been an exciting time. I have enjoyed work- ing with the Gemini staff, whose drive, dedication, and talent were already well known to me from when I chaired the Observatory Oversight Council on behalf of the Association of Universities for Research in Astronomy (AURA). -
Copyrighted Material
Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
Dod Space Technology Guide
Foreword Space-based capabilities are integral to the U.S.’s national security operational doctrines and processes. Such capa- bilities as reliable, real-time high-bandwidth communica- tions can provide an invaluable combat advantage in terms of clarity of command intentions and flexibility in the face of operational changes. Satellite-generated knowledge of enemy dispositions and movements can be and has been exploited by U.S. and allied commanders to achieve deci- sive victories. Precision navigation and weather data from space permit optimal force disposition, maneuver, decision- making, and responsiveness. At the same time, space systems focused on strategic nuclear assets have enabled the National Command Authorities to act with confidence during times of crisis, secure in their understanding of the strategic force postures. Access to space and the advantages deriving from operat- ing in space are being affected by technological progress If our Armed Forces are to be throughout the world. As in other areas of technology, the faster, more lethal, and more precise in 2020 advantages our military derives from its uses of space are than they are today, we must continue to dynamic. Current space capabilities derive from prior invest in and develop new military capabilities. decades of technology development and application. Joint Vision 2020 Future capabilities will depend on space technology programs of today. Thus, continuing investment in space technologies is needed to maintain the “full spectrum dominance” called for by Joint Vision 2010 and 2020, and to protect freedom of access to space by all law-abiding nations. Trends in the availability and directions of technology clearly suggest that the U.S. -
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. -
Gemini North Telescope
Gemini North Telescope Image Credit: Gemini Observatory/AURA/Joy Pollard Gemini Observatory Legacy Image Gemini North Telescope Gemini Observatory Facts The Gemini Observatory is operated by the Association of Universities for The 8-meter Frederick C. Gillett Gemini North telescope is PRIMARY MIRRORS: Research in Astronomy, Inc., under a cooperative agreement with the located near the summit of Hawaii’s Maunakea — a long Diameter: 8.1 meters; 26.57 feet; 318.84 inches National Science Foundation on behalf Mass: 22.22 metric tonnes; 24.5 U.S. tons of the Gemini Partnership. dormant volcano rising 4,205 meters into the dry, stable air Composition: Corning Ultra-Low Expansion (ULE) Glass of the North Pacific. Gemini North was designed and built, Surface Accuracy: 15.6 nm RMS (between 1/1000 - 1/10,000 in part, to provide the best image quality possible from the thickness of human hair) ground for telescopes of its size. TELESCOPE STRUCTURES: United States Four significant features help the telescope achieve this Height: 21.7 meters; 71.2 feet; 7 stories (from “Observing Floor”) goal: (1) An ~20-centimeter-thin primary mirror on a bed of Weight: 380 metric tonnes; 419 U.S. tons Optomechanical Design: Cassegrain ; Alt-azimuth 120 hydraulic actuators; (2) a 1-meter-diameter secondary DOMES: Canada mirror capable of rapid tip-tilt corrective motions; (3) vents on the cylindrical walls to provide a smooth flow of air Height: 46 meters; 151 feet; 15 stories (from ground) above the primary mirror, and to regulate the temperature Weight: 780 metric tonnes; 860 U.S. tons (moving mass) Rotation: 360 degrees in 2 minutes of the air above the mirror to match the outside Thermal Vents: 10 meters; 32.8 feet (width – fully open) temperature; and (4) an adaptive optics system which Brazil GEOGRAPHICAL DATA: can correct for image blurring caused by atmospheric Elevation: Gemini North: 4,214 meters; 13,824 feet turbulence. -
Chapter 3: Familiarizing Yourself with the Night Sky
Chapter 3: Familiarizing Yourself With the Night Sky Introduction People of ancient cultures viewed the sky as the inaccessible home of the gods. They observed the daily motion of the stars, and grouped them into patterns and images. They assigned stories to the stars, relating to themselves and their gods. They believed that human events and cycles were part of larger cosmic events and cycles. The night sky was part of the cycle. The steady progression of star patterns across the sky was related to the ebb and flow of the seasons, the cyclical migration of herds and hibernation of bears, the correct times to plant or harvest crops. Everywhere on Earth people watched and recorded this orderly and majestic celestial procession with writings and paintings, rock art, and rock and stone monuments or alignments. When the Great Pyramid in Egypt was constructed around 2650 BC, two shafts were built into it at an angle, running from the outside into the interior of the pyramid. The shafts coincide with the North-South passage of two stars important to the Egyptians: Thuban, the star closest to the North Pole at that time, and one of the stars of Orion’s belt. Orion was The Ishango Bone, thought to be a 20,000 year old associated with Osiris, one of the Egyptian gods of the lunar calendar underworld. The Bighorn Medicine Wheel in Wyoming, built by Plains Indians, consists of rocks in the shape of a large circle, with lines radiating from a central hub like the spokes of a bicycle wheel. -
Wide-Field Infrared Survey Explorer Launch Press
PRess KIT/DECEMBER 2009 Wide-field Infrared Survey Explorer Launch Contents Media Services Information ................................................................................................................. 3 Quick Facts ............................................................................................................................................. 4 Mission Overview .................................................................................................................................. 5 Why Infrared? ....................................................................................................................................... 10 Science Goals and Objectives ......................................................................................................... 12 Spacecraft ............................................................................................................................................. 16 Science Instrument ............................................................................................................................. 19 Infrared Missions: Past and Present ............................................................................................... 23 NASA’s Explorer Program ................................................................................................................. 25 Program/Project Management .......................................................................................................... 27 Media Contacts J.D. Harrington -
Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
Detection of Large-Scale X-Ray Bubbles in the Milky Way Halo
Detection of large-scale X-ray bubbles in the Milky Way halo P. Predehl1†, R. A. Sunyaev2,3†, W. Becker1,4, H. Brunner1, R. Burenin2, A. Bykov5, A. Cherepashchuk6, N. Chugai7, E. Churazov2,3†, V. Doroshenko8, N. Eismont2, M. Freyberg1, M. Gilfanov2,3†, F. Haberl1, I. Khabibullin2,3, R. Krivonos2, C. Maitra1, P. Medvedev2, A. Merloni1†, K. Nandra1†, V. Nazarov2, M. Pavlinsky2, G. Ponti1,9, J. S. Sanders1, M. Sasaki10, S. Sazonov2, A. W. Strong1 & J. Wilms10 1Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany. 2Space Research Institute of the Russian Academy of Sciences, Moscow, Russia. 3Max-Planck-Institut für Astrophysik, Garching, Germany. 4Max-Planck-Institut für Radioastronomie, Bonn, Germany. 5Ioffe Institute, St Petersburg, Russia. 6M. V. Lomonosov Moscow State University, P. K. Sternberg Astronomical Institute, Moscow, Russia. 7Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia. 8Institut für Astronomie und Astrophysik, Tübingen, Germany. 9INAF-Osservatorio Astronomico di Brera, Merate, Italy. 10Dr. Karl-Remeis-Sternwarte Bamberg and ECAP, Universität Erlangen-Nürnberg, Bamberg, Germany. †e-mail: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]; [email protected] The halo of the Milky Way provides a laboratory to study the properties of the shocked hot gas that is predicted by models of galaxy formation. There is observational evidence of energy injection into the halo from past activity in the nucleus of the Milky Way1–4; however, the origin of this energy (star formation or supermassive-black-hole activity) is uncertain, and the causal connection between nuclear structures and large-scale features has not been established unequivocally.