Research and Scientific Support Department 2003 – 2004
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ESA Missions AO Analysis
ESA Announcements of Opportunity Outcome Analysis Arvind Parmar Head, Science Support Office ESA Directorate of Science With thanks to Kate Isaak, Erik Kuulkers, Göran Pilbratt and Norbert Schartel (Project Scientists) ESA UNCLASSIFIED - For Official Use The ESA Fleet for Astrophysics ESA UNCLASSIFIED - For Official Use Dual-Anonymous Proposal Reviews | STScI | 25/09/2019 | Slide 2 ESA Announcement of Observing Opportunities Ø Observing time AOs are normally only used for ESA’s observatory missions – the targets/observing strategies for the other missions are generally the responsibility of the Science Teams. Ø ESA does not provide funding to successful proposers. Ø Results for ESA-led missions with recent AOs presented: • XMM-Newton • INTEGRAL • Herschel Ø Gender information was not requested in the AOs. It has been ”manually” derived by the project scientists and SOC staff. ESA UNCLASSIFIED - For Official Use Dual-Anonymous Proposal Reviews | STScI | 25/09/2019 | Slide 3 XMM-Newton – ESA’s Large X-ray Observatory ESA UNCLASSIFIED - For Official Use Dual-Anonymous Proposal Reviews | STScI | 25/09/2019 | Slide 4 XMM-Newton Ø ESA’s second X-ray observatory. Launched in 1999 with annual calls for observing proposals. Operational. Ø Typically 500 proposals per XMM-Newton Call with an over-subscription in observing time of 5-7. Total of 9233 proposals. Ø The TAC typically consists of 70 scientists divided into 13 panels with an overall TAC chair. Ø Output is >6000 refereed papers in total, >300 per year ESA UNCLASSIFIED - For Official Use -
No. 40. the System of Lunar Craters, Quadrant Ii Alice P
NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates. -
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. -
Chance, Luck and Statistics : the Science of Chance
University of Calgary PRISM: University of Calgary's Digital Repository Alberta Gambling Research Institute Alberta Gambling Research Institute 1963 Chance, luck and statistics : the science of chance Levinson, Horace C. Dover Publications, Inc. http://hdl.handle.net/1880/41334 book Downloaded from PRISM: https://prism.ucalgary.ca Chance, Luck and Statistics THE SCIENCE OF CHANCE (formerly titled: The Science of Chance) BY Horace C. Levinson, Ph. D. Dover Publications, Inc., New York Copyright @ 1939, 1950, 1963 by Horace C. Levinson All rights reserved under Pan American and International Copyright Conventions. Published in Canada by General Publishing Company, Ltd., 30 Lesmill Road, Don Mills, Toronto, Ontario. Published in the United Kingdom by Constable and Company, Ltd., 10 Orange Street, London, W.C. 2. This new Dover edition, first published in 1963. is a revised and enlarged version ot the work pub- lished by Rinehart & Company in 1950 under the former title: The Science of Chance. The first edi- tion of this work, published in 1939, was called Your Chance to Win. International Standard Rook Number: 0-486-21007-3 Libraiy of Congress Catalog Card Number: 63-3453 Manufactured in the United States of America Dover Publications, Inc. 180 Varick Street New York, N.Y. 10014 PREFACE TO DOVER EDITION THE present edition is essentially unchanged from that of 1950. There are only a few revisions that call for comment. On the other hand, the edition of 1950 contained far more extensive revisions of the first edition, which appeared in 1939 under the title Your Chance to Win. One major revision was required by the appearance in 1953 of a very important work, a life of Cardan,* a brief account of whom is given in Chapter 11. -
Metallicities of the Β Cephei Stars from Low-Resolution Ultraviolet Spectra
A&A 433, 659–669 (2005) Astronomy DOI: 10.1051/0004-6361:20040396 & c ESO 2005 Astrophysics Metallicities of the β Cephei stars from low-resolution ultraviolet spectra E. Niemczura and J. Daszynska-Daszkiewicz´ Astronomical Institute, Wrocław University, ul. Kopernika 11, 51-622 Wrocław, Poland e-mail: [email protected] Received 5 March 2004 / Accepted 22 November 2004 Abstract. We derive basic stellar parameters (angular diameters, effective temperatures, metallicities) and interstellar reddening for all β Cephei stars observed during the IUE satellite mission, including those belonging to three open clusters. The parameters are derived by means of an algorithmic procedure of fitting theoretical flux distributions to the low-resolution IUE spectra and ground-based spectrophotometric observations. Since the metallicity has a special importance for pulsating B-type stars, we focus our attention in particular on this parameter. Key words. stars: early-type – stars: abundances – stars: variables: general 1. Introduction In this paper we analyze the IUE (International Ultraviolet Explorer) data combined with ground-based spectrophotomet- β Cephei variables are a well-known group of early B-type ric observations of β Cephei stars. The ultraviolet (UV) part pulsating stars. Their pulsations are driven by the classical of the spectra of main-sequence B-type stars is very rich in κ-mechanism, operating in the layer of the metal opacity bump lines of the iron-group elements. Because the greatest amount ≈ × 5 at T 2 10 K caused by the large number of absorption of energy for these objects is emitted in the spectral region be- lines of the iron-group elements. -
The High Energy Astrophysics Division Newsletter
SPRING 2017 The High Energy Astrophysics Division Newsletter In this Issue: View from the Chair — special advertising section — hidden black holes revealed, and others — second running — finding a path through spacetime — announcing mysteries under the ice — performance enhancements for Chandra — milestones for XMM — the hunt continues for Swift — ULXNS — on the trail of the wild neutrino with INTEGRAL — searching at home with Fermi — energetic electrons seen at the ISS — news from the cosmos — of scientific interest — a Universe of learning — NICER launch prep — SRG progress — the wisdom of Athena — the slant on IXPE — the XARM — building CTA — all-seeing Lynx — in memoriam From the Chair for the discovery of merging black hole binaries, and for beginning the new era of gravitational-wave astronomy. CHRIS REYNOLDS (U. MD) Prof. González will give the Rossi Prize Lecture at the All systems are go for our 16th Divisional meeting to 231st AAS meeting to be held at National Harbor, MD be held in Sun Valley, Idaho, 20-24 August 2017! Regis- in January 2018. Please join me in congratulating all of tration and abstract submission is now open and we’re this year’s HEAD prize winners. looking forward to an exciting scientific program cover- ing all aspects of high-energy astrophysics, kicked off by The past few months has been eventful in the world a total solar eclipse! of high-energy astrophysics missions. NICER and ISS- CREAM are at the Kennedy Space Center and ready for One of the most important aspects of these meet- launch to the International Space Station. Further in the ings is the chance to honor a new batch of HEAD future, NASA has formally selected the Imaging X-ray Po- prize winners. -
The Ohio State University Astronomy Department Columbus, Ohio 43210
The Ohio State University Astronomy Department Columbus, Ohio 43210 Abstract Zheng Zheng. Justin Oelgoetz is an OSU Chemical This annual report covers the period 2002 September Physics graduate student working on his Ph.D. thesis through 2003 August. with Pradhan. The Masters Degree was awarded to Fields, Mar- 1 PERSONNEL shall, and Onken. During the period covered by this report, the regu- Osmer represents OSU on the Board of Directors lar academic staff of the Department of Astronomy in- of the Large Binocular Telescope Corporation. He is cluded Richard Boyd, Darren DePoy, Jay Frogel, An- a member of the Publications Board of the American drew Gould, Eric Herbst, Smita Mathur, Jordi Miralda- Astronomical Society and also serves on the Board of Escud´e, Gerald Newsom, Patrick Osmer (chairperson), Directors of Research Corporation. Bradley Peterson, Marc Pinsonneault, Richard Pogge, Peterson completed a term as a member of the NASA Anil Pradhan, Barbara Ryden, Robert Scherrer, Kris- Structure and Evolution of the Universe Subcommittee. ten Sellgren, Gary Steigman, Donald Terndrup, Terrance He continues to serve as a member of the Astronomy Walker, and David Weinberg. In addition, Christopher and Astrophysics Advisory Committee (AAAC), which Kochanek has been appointed Ohio Eminent Scholar in was established by Congress to facilitate greater coop- the Department of Astronomy, starting October 1, 2003. eration between the National Science Foundation and Boyd was on leave, serving in the Physics Division of NASA. Peterson is OSU’s institutional representative to the National Science Foundation in Washington, D.C. the AURA Board and this year he was elected to the as Program Director for Nuclear Physics and for Par- Space Telescope Institute Council (STIC). -
Constraints on the Timescale of Animal Evolutionary History
Palaeontologia Electronica palaeo-electronica.org Constraints on the timescale of animal evolutionary history Michael J. Benton, Philip C.J. Donoghue, Robert J. Asher, Matt Friedman, Thomas J. Near, and Jakob Vinther ABSTRACT Dating the tree of life is a core endeavor in evolutionary biology. Rates of evolution are fundamental to nearly every evolutionary model and process. Rates need dates. There is much debate on the most appropriate and reasonable ways in which to date the tree of life, and recent work has highlighted some confusions and complexities that can be avoided. Whether phylogenetic trees are dated after they have been estab- lished, or as part of the process of tree finding, practitioners need to know which cali- brations to use. We emphasize the importance of identifying crown (not stem) fossils, levels of confidence in their attribution to the crown, current chronostratigraphic preci- sion, the primacy of the host geological formation and asymmetric confidence intervals. Here we present calibrations for 88 key nodes across the phylogeny of animals, rang- ing from the root of Metazoa to the last common ancestor of Homo sapiens. Close attention to detail is constantly required: for example, the classic bird-mammal date (base of crown Amniota) has often been given as 310-315 Ma; the 2014 international time scale indicates a minimum age of 318 Ma. Michael J. Benton. School of Earth Sciences, University of Bristol, Bristol, BS8 1RJ, U.K. [email protected] Philip C.J. Donoghue. School of Earth Sciences, University of Bristol, Bristol, BS8 1RJ, U.K. [email protected] Robert J. -
On the Detection of Exoplanets Via Radial Velocity Doppler Spectroscopy
The Downtown Review Volume 1 Issue 1 Article 6 January 2015 On the Detection of Exoplanets via Radial Velocity Doppler Spectroscopy Joseph P. Glaser Cleveland State University Follow this and additional works at: https://engagedscholarship.csuohio.edu/tdr Part of the Astrophysics and Astronomy Commons How does access to this work benefit ou?y Let us know! Recommended Citation Glaser, Joseph P.. "On the Detection of Exoplanets via Radial Velocity Doppler Spectroscopy." The Downtown Review. Vol. 1. Iss. 1 (2015) . Available at: https://engagedscholarship.csuohio.edu/tdr/vol1/iss1/6 This Article is brought to you for free and open access by the Student Scholarship at EngagedScholarship@CSU. It has been accepted for inclusion in The Downtown Review by an authorized editor of EngagedScholarship@CSU. For more information, please contact [email protected]. Glaser: Detection of Exoplanets 1 Introduction to Exoplanets For centuries, some of humanity’s greatest minds have pondered over the possibility of other worlds orbiting the uncountable number of stars that exist in the visible universe. The seeds for eventual scientific speculation on the possibility of these "exoplanets" began with the works of a 16th century philosopher, Giordano Bruno. In his modernly celebrated work, On the Infinite Universe & Worlds, Bruno states: "This space we declare to be infinite (...) In it are an infinity of worlds of the same kind as our own." By the time of the European Scientific Revolution, Isaac Newton grew fond of the idea and wrote in his Principia: "If the fixed stars are the centers of similar systems [when compared to the solar system], they will all be constructed according to a similar design and subject to the dominion of One." Due to limitations on observational equipment, the field of exoplanetary systems existed primarily in theory until the late 1980s. -
Exploration of Mars by the European Space Agency 1
Exploration of Mars by the European Space Agency Alejandro Cardesín ESA Science Operations Mars Express, ExoMars 2016 IAC Winter School, November 20161 Credit: MEX/HRSC History of Missions to Mars Mars Exploration nowadays… 2000‐2010 2011 2013/14 2016 2018 2020 future … Mars Express MAVEN (ESA) TGO Future ESA (ESA- Studies… RUSSIA) Odyssey MRO Mars Phobos- Sample Grunt Return? (RUSSIA) MOM Schiaparelli ExoMars 2020 Phoenix (ESA-RUSSIA) Opportunity MSL Curiosity Mars Insight 2020 Spirit The data/information contained herein has been reviewed and approved for release by JPL Export Administration on the basis that this document contains no export‐controlled information. Mars Express 2003-2016 … First European Mission to orbit another Planet! First mission of the “Rosetta family” Up and running since 2003 Credit: MEX/HRSC First European Mission to orbit another Planet First European attempt to land on another Planet Original mission concept Credit: MEX/HRSC December 2003: Mars Express Lander Release and Orbit Insertion Collission trajectory Bye bye Beagle 2! Last picture Lander after release, release taken by VMC camera Insertion 19/12/2003 8:33 trajectory Credit: MEX/HRSC Beagle 2 was found in January 2015 ! Only 6km away from landing site OK Open petals indicate soft landing OK Antenna remained covered Lessons learned: comms at all time! Credit: MEX/HRSC Mars Express: so many missions at once Mars Mission Phobos Mission Relay Mission Credit: MEX/HRSC Mars Express science investigations Martian Moons: Phobos & Deimos: Ionosphere, surface, -
Mars Exploration - a Story Fifty Years Long Giuseppe Pezzella and Antonio Viviani
Chapter Introductory Chapter: Mars Exploration - A Story Fifty Years Long Giuseppe Pezzella and Antonio Viviani 1. Introduction Mars has been a goal of exploration programs of the most important space agencies all over the world for decades. It is, in fact, the most investigated celestial body of the Solar System. Mars robotic exploration began in the 1960s of the twentieth century by means of several space probes sent by the United States (US) and the Soviet Union (USSR). In the recent past, also European, Japanese, and Indian spacecrafts reached Mars; while other countries, such as China and the United Arab Emirates, aim to send spacecraft toward the red planet in the next future. 1.1 Exploration aims The high number of mission explorations to Mars clearly points out the impor- tance of Mars within the Solar System. Thus, the question is: “Why this great interest in Mars exploration?” The interest in Mars is due to several practical, scientific, and strategic reasons. In the practical sense, Mars is the most accessible planet in the Solar System [1]. It is the second closest planet to Earth, besides Venus, averaging about 360 million kilometers apart between the furthest and closest points in its orbit. Earth and Mars feature great similarities. For instance, both planets rotate on an axis with quite the same rotation velocity and tilt angle. The length of a day on Earth is 24 h, while slightly longer on Mars at 24 h and 37 min. The tilt of Earth axis is 23.5 deg, and Mars tilts slightly more at 25.2 deg [2]. -
Sulfur Hazes in Giant Exoplanet Atmospheres: Impacts on Reflected
Draft version February 28, 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 SULFUR HAZES IN GIANT EXOPLANET ATMOSPHERES: IMPACTS ON REFLECTED LIGHT SPECTRA Peter Gao1,2,3, Mark S. Marley, and Kevin Zahnle NASA Ames Research Center Moffett Field, CA 94035, USA Tyler D. Robinson4,5 Department of Astronomy and Astrophysics University of California Santa Cruz Santa Cruz, CA 95064, USA Nikole K. Lewis Space Telescope Science Institute Baltimore, MD 21218, USA 1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 2NASA Postdoctoral Program Fellow [email protected] 4Sagan Fellow 5NASA Astrobiology Institute’s Virtual Planetary Laboratory ABSTRACT Recent work has shown that sulfur hazes may arise in the atmospheres of some giant exoplanets due to the photolysis of H2S. We investigate the impact such a haze would have on an exoplanet’s geometric albedo spectrum and how it may affect the direct imaging results of WFIRST, a planned NASA space telescope. For temperate (250 K < Teq < 700 K) Jupiter–mass planets, photochemical destruction of H2S results in the production of 1 ppmv of S8 between 100 and 0.1 mbar, which, if cool enough, ∼ will condense to form a haze. Nominal haze masses are found to drastically alter a planet’s geometric albedo spectrum: whereas a clear atmosphere is dark at wavelengths between 0.5 and 1 µm due to molecular absorption, the addition of a sulfur haze boosts the albedo there to 0.7 due to scattering. ∼ Strong absorption by the haze shortward of 0.4 µm results in albedos <0.1, in contrast to the high albedos produced by Rayleigh scattering in a clear atmosphere.