Sentinel-1 and Sentinel-2 Data for Savannah Land Cover Mapping: Optimising the Combination of Sensors and Seasons
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SPHERE: the Exoplanet Imager for the Very Large Telescope J.-L
Astronomy & Astrophysics manuscript no. paper c ESO 2019 October 4, 2019 SPHERE: the exoplanet imager for the Very Large Telescope J.-L. Beuzit1; 2, A. Vigan2, D. Mouillet1, K. Dohlen2, R. Gratton3, A. Boccaletti4, J.-F. Sauvage2; 7, H. M. Schmid5, M. Langlois2; 8, C. Petit7, A. Baruffolo3, M. Feldt6, J. Milli13, Z. Wahhaj13, L. Abe11, U. Anselmi3, J. Antichi3, R. Barette2, J. Baudrand4, P. Baudoz4, A. Bazzon5, P. Bernardi4, P. Blanchard2, R. Brast12, P. Bruno18, T. Buey4, M. Carbillet11, M. Carle2, E. Cascone17, F. Chapron4, J. Charton1, G. Chauvin1; 23, R. Claudi3, A. Costille2, V. De Caprio17, J. de Boer9, A. Delboulbé1, S. Desidera3, C. Dominik15, M. Downing12, O. Dupuis4, C. Fabron2, D. Fantinel3, G. Farisato3, P. Feautrier1, E. Fedrigo12, T. Fusco7; 2, P. Gigan4, C. Ginski15; 9, J. Girard1; 14, E. Giro19, D. Gisler5, L. Gluck1, C. Gry2, T. Henning6, N. Hubin12, E. Hugot2, S. Incorvaia19, M. Jaquet2, M. Kasper12, E. Lagadec11, A.-M. Lagrange1, H. Le Coroller2, D. Le Mignant2, B. Le Ruyet4, G. Lessio3, J.-L. Lizon12, M. Llored2, L. Lundin12, F. Madec2, Y. Magnard1, M. Marteaud4, P. Martinez11, D. Maurel1, F. Ménard1, D. Mesa3, O. Möller-Nilsson6, T. Moulin1, C. Moutou2, A. Origné2, J. Parisot4, A. Pavlov6, D. Perret4, J. Pragt16, P. Puget1, P. Rabou1, J. Ramos6, J.-M. Reess4, F. Rigal16, S. Rochat1, R. Roelfsema16, G. Rousset4, A. Roux1, M. Saisse2, B. Salasnich3, E. Santambrogio19, S. Scuderi18, D. Segransan10, A. Sevin4, R. Siebenmorgen12 C. Soenke12, E. Stadler1, M. Suarez12, D. Tiphène4, M. Turatto3, S. Udry10, F. Vakili11, L. B. F. M. Waters20; 15, L. -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
Astronomy and Astrophysics
THE DECADE OF DISCOVERY IN ASTRONOMY AND ASTROPHYSICS Astronomy and Astrophysics Survey Committee Board on Physics and Astronomy Commission on Physical Sciences, Mathematics, and Applications National Research Council NATIONAL ACADEMY PRESS Washington, D.C. 1991 NATIONAL ACADEMY PRESS • 2101 Constitution Avenue, NW • Washington, DC 20418 NOTICE: The project that is the subject of this report was approved by the Governing Board of the National Research Council, whose members are drawn from the councils of the National Academy of Sciences, the National Academy of Engineering, and the Institute of Medicine. The members of the committee responsible for the report were chosen for their special compe_nces and with regard for appropriate balance. This report has been reviewed by a group other than the authors according to procedures approved by a Report Review Committee consisting of members of the National Academy of Sciences, the National Academy of Engineering, and the Institute of Medicine. This project was supported by the Department of Energy under Grant No. DE-FGO5- 89ER40421, the National Aeronautics and Space Administration and the National Science Foundation under Grant No. AST-8901685, the Naval Research Laboratory under Contract No. N00173-90-M-9744, and the Smithsonian Institution under Purchase Order No. SF0022430000. Additional support was provided by the Maurice Ewing Earth and Planetary Sciences Fund of the National Academy of Sciences created through a gift from the Palisades Geophysical Institute, Inc., and an anonymous donor. Library of Congress Cataloging-in-Publication Data National Research Council (U.S.). Astronomy and Astrophysics Survey Committee. The decade of discovery in astronomy and astrophysics / Astronomy and Astrophysics Survey Committee, Board on Physics and Astronomy, Commission on Physical Sciences, Mathematics, and Applications, National Research Council. -
The Bursty Star Formation History of the Fornax Dwarf Spheroidal Galaxy Revealed with the HST
MNRAS 000,1–20 (2020) Preprint 12 January 2021 Compiled using MNRAS LATEX style file v3.0 The bursty star formation history of the Fornax dwarf spheroidal galaxy revealed with the HST V. Rusakov,1,2,3¢ M. Monelli,4,5 C. Gallart,4,5 T. K. Fritz,4,5 T. Ruiz-Lara,4,5,6 E. J. Bernard,7 S. Cassisi.8,9 1Department of Physics, University of Surrey, Guildford GU2 7XH, UK 2Cosmic Dawn Center (DAWN) 3Niels Bohr Institute, University of Copenhagen, Lyngbyvej 2, DK-2100 Copenhagen Ø, Denmark 4Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain 5Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 6Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, The Netherlands 7Universite Côte dÁzur, Observatoire de la Côte dÁzur, CNRS, Laboratoire Lagrange, France 8INAF - Astronomical Observatory of Abruzzo, Via M. Maggini, I-64100 Teramo, Italy 9INFN, Sezione di Pisa, Largo Pontecorvo 3, 56127 Pisa, Italy Accepted 2020 December 24. Received 2020 December 7; in original form 2020 February 22 ABSTRACT We present a new derivation of the star formation history (SFH) of the dSph galaxy Fornax in two central regions, characterised by unprecedented precision and age resolution. It reveals that star formation has proceeded in sharp bursts separated by periods of low-level or quies- cent activity. The SFH was derived through colour-magnitude diagram (CMD) fitting of two extremely deep Hubble Space Telescope CMDs, sampling the centre and one core radius. The attained age resolution allowed us to single out a major star formation episode at early times, a second strong burst 4.6 ± 0.4 Gyr ago and recent intermittent episodes ∼ 2 − 0.2 Gyr ago. -
Journal of the Association of Lunar & Planetary Observers
ISSN-0039-2502 Journal of the Association of Lunar & Planetary Observers The Strolling Astronomer Volume 46, Number 3, Summer 2004 Now in Portable Document Format (PDF) for MacIntosh and PC-Compatible Computers Inside. * The Perseids are coming! The Perseids are coming! And guess what — almost NO Moon this time! * Some early personal reports on the Venus transit * A report on the 1996 Jupi- ter apparition * A writeup on This Issue’s Cover: A great shot of the Venus transit by Mercury Section Coordinator the Moon’s Frank Melillo from Holtsville, NY, USA. Taken June 8, 10:40 UT (6:40 a.m. local time) using a Celestron 8-inch Schmidt-Cassegrain at f/10 equipped with a Starlight Xpress MX5 CCD Maestlin camera; exposure 0.5 second; some clouds present. For an animation of this image, go to Region http://hometown.aol.com/frankj12/specialtransitpage1.html . plus LOTS of reports about your ALPO section activities and much, much more. The Strolling Astronomer Journal of the In This Issue: Association of Lunar & Inside the ALPO Point of View: It’s Nice to be Noticed – Again..... 1 Planetary Observers, ALPO Founder Walter Haas Injured in Fall..........2 In Memoriam: Janet Mattei .................................2 The Strolling Astronomer ALPO’s L. Garrett: Asteroid Discoverer ...............2 Reminder: Address Changes ...............................2 Volume 46, No. 3, Summer 2004 Report from the ALPO Membership Secretary/ This issue published in July 2004 for distribution in both Treasurer.........................................................2 portable document format (pdf) and also hardcopy for- Interest Section Reports mat. Computing Section .........................................3 ALPO Lunar & Planetary Training Program....3 This publication is the official journal of the Association The Federation of Galaxy Explorers: The Future of Lunar & Planetary Observers (ALPO). -
Table of Contents
PAGE: 1 PAGE: 2 Table of Contents LEXILE® MEASURE 3 Copernicus, King of Craters 870L 4 Catching Andromeda’s Light 890L 6 Merry Christmas from the Moon! 810L ©Highlights for Children, Inc. This item is permitted to be used by a teacher or educator free of charge for classroom use by printing or photocopying one copy for each student in the class. Highlights® Fun with a Purpose® ISBN 978-1-62091-227-0 PAGE: 32 object—either a rocky asteroid or an icy comet—was more than a mile in diameter. Still, there are larger craters on the Moon, so why is Copernicus special? The answer is simple: because the crater faces Earth directly, it looks nice and round, exactly the way everyone thinks a crater should look. But what really makes Coper- nicus special is its halo of rays. These wispy streamers stretch outward in every direction. Like the crater itself, they are brightest when the Moon is full. Take a close look at these feather-like Copernicus splashes. When a big object blasts out a crater, the smallest particles travel farthest from the point of impact. This spray of rock then falls in a splash pattern onto the lunar surface. This material looks bright because it’s made up of crushed and broken rock, which Copernicus, King of Craters By Edmund A. Fortier On the Moon, this crater rules. The best-known impact crater on to the left of the Moon’s center. reflects light better than the dust- Earth is Meteor Crater. It is You’ll see a small bright spot covered lava plain. -
Jjmo News 06 19.Pdf
alactic Observer John J. McCarthy Observatory G Volume 12, No. 6 June 2019 GalacticGalactic MerMergggererers --s DancingDancing withwith thethe STSTARSARS AAAor PLANET Deadly Dos-I-Dos? IS BORN See page 18 inside http://www.mccarthyobservatory.org JJMO June 2019 • 1 The John J. McCarthy Observatory Galactic Observvvererer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Phone/Fax: (860) 354-1595 Production & Design www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky It is through their efforts that the McCarthy Observatory has established itself as a significant educational and Technical Support recreational resource within the western Connecticut Bob Lambert community. Dr. Parker Moreland Steve Barone Peter Gagne Marc Polansky Colin Campbell Louise Gagnon Joe Privitera Dennis Cartolano John Gebauer Danielle Ragonnet Route Mike Chiarella Elaine Green Monty Robson Jeff Chodak Jim Johnstone Don Ross Bill Cloutier Carly KleinStern Gene Schilling Doug Delisle Bob Lambert Katie Shusdock Cecilia Detrich Roger Moore Jim Wood Dirk Feather Parker Moreland, PhD Paul Woodell Randy Fender Allan Ostergren Amy Ziffer In This Issue "OUT THE WINDOW ON YOUR LEFT .................................... 3 SUNRISE AND SUNSET ...................................................... 13 KIES PI LAVA DOME ....................................................... 4 SUMMER NIGHTS ........................................................... 13 -
The Bulge Asymmetries and Dynamical Evolution (Baade) Sio Maser Survey at 86 Ghz with ALMA
DRAFT VERSION SEPTEMBER 6, 2019 Typeset using LATEX twocolumn style in AASTeX62 The Bulge Asymmetries and Dynamical Evolution (BAaDE) SiO Maser Survey at 86 GHz with ALMA ∗ MICHAEL C. STROH,1 YLVA M. PIHLSTRÖM,1 , LORÁNT O. SJOUWERMAN,2 MEGAN O. LEWIS,1 MARK JCLAUSSEN,2 MARK R. MORRIS,3 AND R. MICHAEL RICH3 1Department of Physics & Astronomy, The University of New Mexico, Albuquerque, NM 87131 2National Radio Astronomy Observatory, Array Operations Center, Socorro, NM 87801 3Department of Physics & Astronomy, University of California, Los Angeles, CA 90095 (Accepted August 14th, 2019) ABSTRACT We report on the first 1,432 sources observed using the Atacama Large Millimeter/submillimeter Array (ALMA), from the Bulge Asymmetries and Dynamical Evolution (BAaDE) survey, which aims to obtain tens of thousands of line-of-sight velocities from SiO masers in Asymptotic Giant Branch (AGB) stars in the Milky Way. A 71% detection rate of 86 GHz SiO masers is obtained from the infrared color-selected sample, and increases to 80% when considering the likely oxygen-rich stars using Midcourse Space Experiment (MSX) col- ors isolated in a region where [D] - [E] ≤ 1:38. Based on Galactic distributions, the presence of extended CS emission, and likely kinematic associations, the population of sources with [D] - [E] > 1:38 probably consists of young stellar objects, or alternatively, planetary nebulae. For the SiO detections we examined whether indi- vidual SiO transitions provide comparable stellar line-of-sight velocities, and found that any SiO transition is suitable for determining a stellar AGB line-of-sight velocity. Finally, we discuss the relative SiO detection rates and line strengths in the context of current pumping models. -
The Messenger
THE MESSENGER ( , New Meteorite Finds At Imilac No. 47 - March 1987 H. PEDERSEN, ESO, and F. GARe/A, elo ESO Introduction hand, depend more on the preserving some 7,500 meteorites were recovered Stones falling from the sky have been conditions of the terrain, and the extent by Japanese and American expeditions. collected since prehistoric times. They to which it allows meteorites to be spot They come from a smaller, but yet un were, until recently, the only source of ted. Most meteorites are found by known number of independent falls. The extraterrestrial material available for chance. Active searching is, in general, meteorites appear where glaciers are laboratory studies and they remain, too time consuming to be of interest. pressed up towards a mountain range, even in our space age, a valuable However, the blue-ice fields of Antarctis allowing the ice to evaporate. Some source for investigation of the solar sys have proven to be a happy hunting have been Iying in the ice for as much as tem's early history. ground. During the last two decades 700,000 years. It is estimated that, on the average, each square kilometre of the Earth's surface is hit once every million years by a meteorite heavier than 500 grammes. Most are lost in the oceans, or fall in sparsely populated regions. As a result, museums around the world receive as few as about 6 meteorites annually from witnessed falls. Others are due to acci dental finds. These have most often fallen in prehistoric times. Each of the two groups, 'falls' and 'finds', consists of material from about one thousand catalogued, individual meteorites. -
The Isabel Williamson Lunar Observing Program
The Isabel Williamson Lunar Observing Program by The RASC Observing Committee Revised Third Edition September 2015 © Copyright The Royal Astronomical Society of Canada. All Rights Reserved. TABLE OF CONTENTS FOR The Isabel Williamson Lunar Observing Program Foreword by David H. Levy vii Certificate Guidelines 1 Goals 1 Requirements 1 Program Organization 2 Equipment 2 Lunar Maps & Atlases 2 Resources 2 A Lunar Geographical Primer 3 Lunar History 3 Pre-Nectarian Era 3 Nectarian Era 3 Lower Imbrian Era 3 Upper Imbrian Era 3 Eratosthenian Era 3 Copernican Era 3 Inner Structure of the Moon 4 Crust 4 Lithosphere / Upper Mantle 4 Asthenosphere / Lower Mantle 4 Core 4 Lunar Surface Features 4 1. Impact Craters 4 Simple Craters 4 Intermediate Craters 4 Complex Craters 4 Basins 5 Secondary Craters 5 2. Main Crater Features 5 Rays 5 Ejecta Blankets 5 Central Peaks 5 Terraced Walls 5 ii Table of Contents 3. Volcanic Features 5 Domes 5 Rilles 5 Dark Mantling Materials 6 Caldera 6 4. Tectonic Features 6 Wrinkle Ridges 6 Faults or Rifts 6 Arcuate Rilles 6 Erosion & Destruction 6 Lunar Geographical Feature Names 7 Key to a Few Abbreviations Used 8 Libration 8 Observing Tips 8 Acknowledgements 9 Part One – Introducing the Moon 10 A – Lunar Phases and Orbital Motion 10 B – Major Basins (Maria) & Pickering Unaided Eye Scale 10 C – Ray System Extent 11 D – Crescent Moon Less than 24 Hours from New 11 E – Binocular & Unaided Eye Libration 11 Part Two – Main Observing List 12 1 – Mare Crisium – The “Sea of Cries” – 17.0 N, 70-50 E; -
Observing the Lunar Libration Zones
Observing the Lunar Libration Zones Alexander Vandenbohede 2005 Many Look, Few Observe (Harold Hill, 1991) Table of Contents Introduction 1 1 Libration and libration zones 3 2 Mare Orientale 14 3 South Pole 18 4 Mare Australe 23 5 Mare Marginis and Mare Smithii 26 6 Mare Humboldtianum 29 7 North Pole 33 8 Oceanus Procellarum 37 Appendix I: Observational Circumstances and Equipment 43 Appendix II: Time Stratigraphical Table of the Moon and the Lunar Geological Map 44 Appendix III: Bibliography 46 Introduction – Why Observe the Libration Zones? You might think that, because the Moon always keeps the same hemisphere turned towards the Earth as a consequence of its captured rotation, we always see the same 50% of the lunar surface. Well, this is not true. Because of the complicated motion of the Moon (see chapter 1) we can see a little bit around the east and west limb and over the north and south poles. The result is that we can observe 59% of the lunar surface. This extra 9% of lunar soil is called the libration zones because the motion, a gentle wobbling of the Moon in the Earth’s sky responsible for this, is called libration. In spite of the remainder of the lunar Earth-faced side, observing and even the basic task of identifying formations in the libration zones is not easy. The formations are foreshortened and seen highly edge-on. Obviously, you will need to know when libration favours which part of the lunar limb and how much you can look around the Moon’s limb. -
Griffith Observer Cumulative Index
Griffith Observer Cumulative Index author title mo year key words Anonymous The Romance of the Calendar 2 1937 calendar, Julian, Gregorian Anonymous Other Worlds than Ours 3 1937 Planets, Solar System Anonymous The S ola r Fa mily 3 1937 Planets, Solar System Roya l Elliott Behind the Sciences 3 1937 GO, pla ne ta rium, e xhibits , Ge ologica l Clock Anonymous The Stars of Spring 4 1937 Cons te lla tions , S ta rs , Anonymous Pronunciation of Star and 4 1937 Cons te lla tions , S ta rs Constellation Names Anonymous The Cycle of the Seasons 5 1937 Seasons, climate Anonymous The Ice Ages 5 1937 United States, Climate, Greenhouse Gases, Volcano, Ice Age Anonymous New Meteorites at the Griffith 5 1937 Meteorites Observatory Anonymous Conditions of Eclipse 6 1937 Solar eclipse, June 8, Occurrences 1937, Umbra, Sun, Moon Anonymous Ancient and Modern Eclipse 6 1937 Chinese, Observation, Observations Eclips e , Re la tivity Anonymous The Sky as Seen from 6 1937 Stars, Celestial Sphere, Different Latitudes Equator, Pole, Latitude Anonymous Laws of Polar Motion 6 1937 Pole, Equator, Latitude Anonymous The Polar Aurora 7 1937 Northern lights, Aurora Anonymous The Astrorama 7 1937 Star map, Planisphere, Astrorama Anonymous The Life Story of the Moon 8 1937 Moon, Earth's rotation, Darwin Anonymous Conditions on the Moon 8 1937 Moon, Temperature, Anonymous The New Comet 8 1937 Come t Fins le r Anonymous Comets 9 1937 Halley's Comet, Meteor Anonymous Meteors 9 1937 Meteor Crater, Shower, Leonids Anonymous Comet Orbits 9 1937 Comets, Encke Anonymous