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The Status and Future of EUV Astronomy
The status and future of EUV astronomy M. A. Barstow∗, S. L. Casewell Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK J. B. Holberg Lunar and Planetary Laboratory, 1541 East University Boulevard, Sonett Space Sciences Building, University of Arizona, Tucson, AZ 85721, USA M.P. Kowalski Naval Research Laboratory,4555 Overlook Ave SW Washington, DC 20375, USA Abstract The Extreme Ultraviolet wavelength range was one of the final windows to be opened up to astronomy. Nevertheless, it provides very important diagnostic tools for a range of astronomical objects, although the opacity of the interstellar medium restricts the majority of observations to sources in our own galaxy. This review gives a historical overview of EUV astronomy, describes current instrumental capabilities and examines the prospects for future facilities on small and medium-class satellite platforms. Keywords: Extreme Ultraviolet, Spectroscopy, White Dwarfs, Stellar Coronae, Interstellar Medium 1. Introduction arXiv:1309.2181v1 [astro-ph.SR] 9 Sep 2013 The Extreme Ultraviolet (EUV) nominally spans the wavelength range from 100 to 912 A,˚ although for practical purposes the edges are often some- what indistinct as instrument band-passes may extend short-ward into the soft X-ray or long-ward into the far ultraviolet (far-UV). The production of EUV photons is primarily associated with the existence of hot, 105-107 K gas ∗Corresponding Author: [email protected] Preprint submitted to Advances in Space Research October 29, 2018 in the Universe. Sources of EUV radiation can be divided into two main cat- egories, those where the emission arises from recombination of ions and elec- trons in a hot, optically thin plasma, giving rise to emission line spectra, and objects which are seen by thermal emission from an optically thick medium, resulting in a strong continuum spectrum which may contain features arising from transitions between different energy levels or ionisation stages of sev- eral elements. -
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The Multiwavelength Universe
Multiwavelength Astronomy Revealing the Universe in All Its Light Almost everything we know about the universe comes from studying the light emitted or refl ected by objects in space. Apart from a few exceptions, such as the collection of Moon rocks returned by Apollo astronauts, astronomers must rely on collecting and analyzing the faint light from distant objects in order to study the cosmos. This fact is even more remarkable when you consider the vastness of space. Light may travel for billions of years before reaching our telescopes. In the science of astronomy, we generally cannot retrieve samples, study objects in a laboratory, or physically enter an environment for detailed study. Fortunately, light carries a lot of information. By detecting and analyzing the light emitted by an object in space, astronomers can learn about its distance, motion, temperature, density, and chemical composition. Since the light from an object takes time to reach us, it also brings us information about the evolution and history of the universe. When we receive light from an object in space, we are actually performing a type of archaeology by studying the object’s appearance as it was when the light was emitted. For example, when astronomers study a galaxy that is 200 million light-years away, they are examining that galaxy as it looked 200 million years ago. To see what it looks like today, we would have to wait another 200 million years. The Electromagnetic Spectrum Radio MicrowaveInfrared Visible Ultraviolet X-ray Gamma Ray 4 2 -2 -5 -6 -8 -10 -12 1010 110 10 10 10 10 10 Wavelength in centimeters About the size of.. -
Spectra As Windows Into Exoplanet Atmospheres
SPECIAL FEATURE: PERSPECTIVE PERSPECTIVE SPECIAL FEATURE: Spectra as windows into exoplanet atmospheres Adam S. Burrows1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved December 2, 2013 (received for review April 11, 2013) Understanding a planet’s atmosphere is a necessary condition for understanding not only the planet itself, but also its formation, structure, evolution, and habitability. This requirement puts a premium on obtaining spectra and developing credible interpretative tools with which to retrieve vital planetary information. However, for exoplanets, these twin goals are far from being realized. In this paper, I provide a personal perspective on exoplanet theory and remote sensing via photometry and low-resolution spectroscopy. Although not a review in any sense, this paper highlights the limitations in our knowledge of compositions, thermal profiles, and the effects of stellar irradiation, focusing on, but not restricted to, transiting giant planets. I suggest that the true function of the recent past of exoplanet atmospheric research has been not to constrain planet properties for all time, but to train a new generation of scientists who, by rapid trial and error, are fast establishing a solid future foundation for a robust science of exoplanets. planetary science | characterization The study of exoplanets has increased expo- by no means commensurate with the effort exoplanetology, and this expectation is in part nentially since 1995, a trend that in the short expended. true. The solar system has been a great, per- term shows no signs of abating. Astronomers An important aspect of exoplanets that haps necessary, teacher. -
Consolidated Financial Statements and Consolidated Management Report for the Year Ended December 31, 2017 And
Sacyr Group (Sacyr, S.A. and Subsidiaries) Consolidated Financial Statements and Consolidated Management Report for the year ended December 31, 2017 and AUDITORS’ REPORT ON THE CONSOLIDATED FINANCIAL STATEMENTS Audit Report on Financial Statements issued by an Independent Auditor SACYR, S.A. AND SUBSIDIARIES Consolidated Financial Statements and Consolidated Management Report for the year ended December 31, 2017 Translation of a report and financial statements originally issued in Spanish. In the event of discrepancy, the Spanish-language version prevails (See Note 42) AUDIT REPORT ON CONSOLIDATED FINANCIAL STATEMENTS ISSUED BY AN INDEPENDENT AUDITOR To the shareholders of SACYR, S.A.: Audit report on the consolidated financial statements Opinion We have audited the consolidated financial statements of SACYR, S.A. (the parent) and its subsidiaries (the Group), which comprise the consolidated statement of financial position at December 31, 2017, the separate consolidated income statement, the consolidated statement of comprehensive income, the consolidated statement of cash flows, the consolidated statement of changes in equity, and the notes thereto, for the year then ended. In our opinion, the accompanying consolidated financial statements give a true and fair view, in all material respects, of consolidated equity and the consolidated financial position of the Group at December 31, 2017 and of its financial performance and its consolidated cash flows, for the year then ended in accordance with International Financial Reporting Standards, as adopted by the European Union (IFRS-EU), and other provisions in the regulatory framework applicable in Spain. Basis for opinion We conducted our audit in accordance with prevailing audit regulations in Spain. Our responsibilities under those standards are further described in the Auditor’s responsibilities for the audit of the consolidated financial statements section of our report. -
UV and Infrared Astronomy
Why Put a Telescope In Space? • Access to light that does not penetrate the atmosphere • No seeing. A telescope can reach the diffraction limit: 1.22 l/D radians Astronomy in Space. I. UV Astronomy Ultraviolet Astronomy 912-3650 Å (Lyman Limit to Balmer jump) • Continuua of hot stars (spectral types O,B,A) • H I Lyman lines (1-n transitions) • Resonance lines of Li-like ions C IV, N V, O VI • H2 Lyman and Werner bands Normal incidence optics • Special UV-reflective coatings The Far Ultraviolet 912 to 1150 Å • Defined by Lyman limit, MgF cutoff at 1150 Å • LiF + Al reflects longward of 1050 Å • SiC reflects at shorter wavelengths The Astronomy Quarterly, Vol. 7, pp. 131-142, 1990 0364-9229f90 $3.00+.00 Printed in the USA. All rights reserved. Copyright (c) 1990 Pergamon Press plc ASTRONOMICAL ADVANTAGES History OFAN • 9/1/1946: Lyman Spitzer EXTRA-TERRESTRIAL OBSERVATORY proposed a Space Telescope in LYMAN SPITZER, Jr. ’ a Report to project Rand This study points out, in a very preliminary way, the results that might be expected from astronomical measurements made with a satellite • 1966: Spitzer (Princeton) vehicle. The discussion is divided into three parts, corresponding to three different assumptions concerning the amount of instrumentation provided. chairs NASA Ad Hoc In the first section it is assumed that no telescope is provided; in the second a 10-&h reflector is assumed; in the third section some of the results Committee on the "Scientific obtainable with a large reflecting telescope, many feet in diameter, and revolving about the earth above the terrestrial atmosphere, are briefly Uses of the Large Space sketched. -
GRAVITY ASTROPHYSICS a Plan for the 1990S
ULTRAVIOLET, VISIBLE, and GRAVITY ASTROPHYSICS A Plan for the 1990s (NASA-NP-I52) ULTRAVIOLET, N94-24973 VISI3LE, ANO GRAVITY ASTROPHYSICS: A PLAN FOR THE 1990'S (NASA) 76 p Unclas HI190 0207794 ORIGINAL PAGE COLOR PHOTOGRAPH National Aeronautics and Space Administration I-oreword N ASA'sprioritiesOfficefrom oftheSpaceU.S. NationalScience Academyand Applicationsof Sciences.(OSSA)Guidancereceivesto theadviceOSSAon Astrophysicsscientific strategyDivision,and in particular, is provided by dedicated Academy committees, ad hoc study groups and, at 10-year intervals, by broadly mandated astronomy and astrophysics survey committees charged with making recommen- dations for the coming decade. Many of the Academy's recommendations have important implications for the conduct of ultraviolet and visible-light astronomy from space. Moreover, these areas are now poised for an era of rapid growth. Through technological progress, ultraviolet astronomy has already risen from a novel observational technique four decades ago to the mainstream of astronomical research today. Recent developments in space technology and instrumen- tation have the potential to generate comparably dramatic strides in observational astronomy within the next 10 years. In 1989, the Ultraviolet and Visible Astrophysics Branch of the OSSA Astrophysics Division recognized the need for a new, long-range plan that would implement the Academy's recommendations in a way that yielded the most advantageous use of new technology. NASA's Ultraviolet, Visible, and Gravity Astrophysics Management Operations Working Group was asked to develop such a plan for the 1990s. Since the Branch holds programmatic responsibility for space research in gravitational physics and relativity, as well as for ultraviolet and visible-light astrophysics, missions in those areas were also included. -
Essential Radio Astronomy
February 2, 2016 Time: 09:25am chapter1.tex © Copyright, Princeton University Press. No part of this book may be distributed, posted, or reproduced in any form by digital or mechanical means without prior written permission of the publisher. 1 Introduction 1.1 AN INTRODUCTION TO RADIO ASTRONOMY 1.1.1 What Is Radio Astronomy? Radio astronomy is the study of natural radio emission from celestial sources. The range of radio frequencies or wavelengths is loosely defined by atmospheric opacity and by quantum noise in coherent amplifiers. Together they place the boundary be- tween radio and far-infrared astronomy at frequency ν ∼ 1 THz (1 THz ≡ 1012 Hz) or wavelength λ = c/ν ∼ 0.3 mm, where c ≈ 3 × 1010 cm s−1 is the vacuum speed of light. The Earth’s ionosphere sets a low-frequency limit to ground-based radio astronomy by reflecting extraterrestrial radio waves with frequencies below ν ∼ 10 MHz (λ ∼ 30 m), and the ionized interstellar medium of our own Galaxy absorbs extragalactic radio signals below ν ∼ 2 MHz. The radio band is very broad logarithmically: it spans the five decades between 10 MHz and 1 THz at the low-frequency end of the electromagnetic spectrum. Nearly everything emits radio waves at some level, via a wide variety of emission mechanisms. Few astronomical radio sources are obscured because radio waves can penetrate interstellar dust clouds and Compton-thick layers of neutral gas. Because only optical and radio observations can be made from the ground, pioneering radio astronomers had the first opportunity to explore a “parallel universe” containing unexpected new objects such as radio galaxies, quasars, and pulsars, plus very cold sources such as interstellar molecular clouds and the cosmic microwave background radiation from the big bang itself. -
Source of Knowledge, Techniques and Skills That Go Into the Development of Technology, and Prac- Tical Applications
DOCUMENT RESUME ED 027 216 SE 006 288 By-Newell, Homer E. NASA's Space Science and Applications Program. National Aeronautics and Space Administration, Washington, D.C. Repor t No- EP -47. Pub Date 67 Note-206p.; A statement presented to the Committee on Aeronautical and Space Sciences, United States Senate, April 20, 1967. EDRS Price MF-$1.00 HC-$10.40 Descriptors-*Aerospace Technology, Astronomy, Biological Sciences, Earth Science, Engineering, Meteorology, Physical Sciences, Physics, *Scientific Enterprise, *Scientific Research Identifiers-National Aeronautics and Space Administration This booklet contains material .prepared by the National Aeronautic and Space AdMinistration (NASA) office of Space Science and Applications for presentation.to the United States Congress. It contains discussion of basic research, its valueas a source of knowledge, techniques and skillsthat go intothe development of technology, and ioractical applications. A series of appendixes permitsa deeper delving into specific aspects of. Space science. (GR) U.S. DEPARTMENT OF HEALTH, EDUCATION & WELFARE OFFICE OF EDUCATION THIS DOCUMENT HAS BEEN REPRODUCED EXACTLY AS RECEIVEDFROM THE PERSON OR ORGANIZATION ORIGINATING IT.POINTS OF VIEW OR OPINIONS STATED DO NOT NECESSARILY REPRESENT OFFICIAL OMCE OFEDUCATION POSITION OR POLICY. r.,; ' NATiONAL, AERONAUTICS AND SPACEADi4N7ISTRATION' , - NASNS SPACE SCIENCE AND APPLICATIONS PROGRAM .14 A Statement Presented to the Committee on Aeronautical and Space Sciences United States Senate April 20, 1967 BY HOMER E. NEWELL Associate Administrator for Space Science and Applications National Aeronautics and Space Administration Washington, D.C. 20546 +77.,M777,177,,, THE MATERIAL in this booklet is a re- print of a portion of that which was prepared by NASA's Office of Space Science and Ap- -olications for presentation to the Congress of the United States in the course of the fiscal year 1968 authorization process. -
Observing Photons in Space
—1— Observing photons in space For the truth of the conclusions of physical science, observation is the supreme court of appeals Sir Arthur Eddington Martin C.E. HuberI, Anuschka PauluhnI and J. Gethyn TimothyII Abstract This first chapter of the book ‘Observing Photons in Space’ serves to illustrate the rewards of observing photons in space, to state our aims, and to introduce the structure and the conventions used. The title of the book reflects the history of space astronomy: it started at the high-energy end of the electromagnetic spectrum, where the photon aspect of the radiation dominates. Nevertheless, both the wave and the photon aspects of this radiation will be considered extensively. In this first chapter we describe the arduous efforts that were needed before observations from pointed, stable platforms, lifted by rocket above the Earth’s atmosphere, became the matter of course they seem to be today. This exemplifies the direct link between technical effort — including proper design, construction, testing and calibration — and some of the early fundamental insights gained from space observations. We further report in some detail the pioneering work of the early space astronomers, who started with the study of γ- and X-rays as well as ultraviolet photons. We also show how efforts to observe from space platforms in the visible, infrared, sub-millimetre and microwave domains developed and led to today’s emphasis on observations at long wavelengths. The aims of this book This book conveys methods and techniques for observing photons1 in space. ‘Observing’ photons implies not only detecting them, but also determining their direction at arrival, their energy, their rate of arrival, and their polarisation. -
The Space Infrared Interferometric Telescope (SPIRIT): High- Resolution Imaging and Spectroscopy in the Far-Infrared
Leisawitz, D. et al., J. Adv. Space Res., in press (2007), doi:10.1016/j.asr.2007.05.081 The Space Infrared Interferometric Telescope (SPIRIT): High- resolution imaging and spectroscopy in the far-infrared David Leisawitza, Charles Bakera, Amy Bargerb, Dominic Benforda, Andrew Blainc, Rob Boylea, Richard Brodericka, Jason Budinoffa, John Carpenterc, Richard Caverlya, Phil Chena, Steve Cooleya, Christine Cottinghamd, Julie Crookea, Dave DiPietroa, Mike DiPirroa, Michael Femianoa, Art Ferrera, Jacqueline Fischere, Jonathan P. Gardnera, Lou Hallocka, Kenny Harrisa, Kate Hartmana, Martin Harwitf, Lynne Hillenbrandc, Tupper Hydea, Drew Jonesa, Jim Kellogga, Alan Koguta, Marc Kuchnera, Bill Lawsona, Javier Lechaa, Maria Lechaa, Amy Mainzerg, Jim Manniona, Anthony Martinoa, Paul Masona, John Mathera, Gibran McDonalda, Rick Millsa, Lee Mundyh, Stan Ollendorfa, Joe Pellicciottia, Dave Quinna, Kirk Rheea, Stephen Rineharta, Tim Sauerwinea, Robert Silverberga, Terry Smitha, Gordon Staceyf, H. Philip Stahli, Johannes Staguhn j, Steve Tompkinsa, June Tveekrema, Sheila Walla, and Mark Wilsona a NASA’s Goddard Space Flight Center, Greenbelt, MD b Department of Astronomy, University of Wisconsin, Madison, Wisconsin, USA c California Institute of Technology, Pasadena, CA, USA d Lockheed Martin Technical Operations, Bethesda, Maryland, USA e Naval Research Laboratory, Washington, DC, USA f Department of Astronomy, Cornell University, Ithaca, USA g Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA h Astronomy Department, University of Maryland, College Park, Maryland, USA i NASA’s Marshall Space Flight Center, Huntsville, Alabama, USA j SSAI, Lanham, Maryland, USA ABSTRACT We report results of a recently-completed pre-Formulation Phase study of SPIRIT, a candidate NASA Origins Probe mission. SPIRIT is a spatial and spectral interferometer with an operating wavelength range 25 - 400 µm. -
Hobart Northern Suburbs Light Rail – Business Case Peer Review
Tasmanian Government Department of Infrastructure, Energy and Resources 11 December 2012 Hobart Northern Suburbs Light Rail Business Case Peer Review AECOM Hobart Northern Suburbs Light Rail Hobart Northern Suburbs Light Rail Business Case Peer Review Prepared for Tasmanian Government Department of Infrastructure, Energy and Resources Prepared by AECOM Australia Pty Ltd Level 8, 540 Wickham Street, PO Box 1307, Fortitude Valley QLD 4006, Australia T +61 7 3553 2000 F +61 7 3553 2050 www.aecom.com ABN 20 093 846 925 11 December 2012 60277500 AECOM in Australia and New Zealand is certified to the latest version of ISO9001 and ISO14001. © AECOM Australia Pty Ltd (AECOM). All rights reserved. AECOM has prepared this document for the sole use of the Client and for a specific purpose, each as expressly stated in the document. No other party should rely on this document without the prior written consent of AECOM. AECOM undertakes no duty, nor accepts any responsibility, to any third party who may rely upon or use this document. This document has been prepared based on the Client’s description of its requirements and AECOM’s experience, having regard to assumptions that AECOM can reasonably be expected to make in accordance with sound professional principles. AECOM may also have relied upon information provided by the Client and other third parties to prepare this document, some of which may not have been verified. Subject to the above conditions, this document may be transmitted, reproduced or disseminated only in its entirety. \\aubne1fp003\Projects\Projects\60277500\6.