Annual Report / Rapport Annuel / Jahresbericht 1998

Total Page:16

File Type:pdf, Size:1020Kb

Annual Report / Rapport Annuel / Jahresbericht 1998 Annual Report / Rapport annuel / Jahresbericht 1998 EUROPEAN SOUTHERN OBSERVATORY COVER COUVERTURE UMSCHLAG Impressive images were obtained soon after Des images impressionnantes ont été reçues Beeindruckende Aufnahmen wurden ge- the multi-mode VLT Infrared Spectrometer peu de temps après l’installation de l’ins- macht kurz nachdem im November 1998 And Array Camera (ISAAC) instrument trument multi-mode ISAAC (« Infrared das Multimodus-Instrument ISAAC („Infra- was mounted at the first VLT 8.2-m Unit Spectrometer And Array Camera») au pre- red Spektrometer And Array Camera“) am mier télescope VLT de 8,2 mètres (UT1) en Telescope (UT1) in November 1998. This ersten der VLT-Teleskope (UT1) installiert colour composite image of the RCW38 star- novembre 1998. Cette image couleur com- worden war. Diese Farbaufnahme des forming complex combines Z (0.95 µm), H posite du complexe de formation stellaire (1.65 µm) and Ks (2.16 µm) exposures of a RCW38 combine des images prises en Z Sternentstehungsgebiets RCW38 ist zusam- few minutes each. Stars which have recent- (0,95 µm), H (1,65 µm) et Ks (2,16 µm), mengesetzt aus Einzelaufnahmen in Z (0,95 ly formed in clouds of gas and dust in this ayant un temps d’exposition de quelques µm), H (1,65 µm) und Ks (2,16 µm) von je region 5000 light-years away are still heav- minutes chacune. Les étoiles, récemment einigen Minuten Belichtungszeit. Die vor ily obscured and cannot be seen at optical formées dans les nuages de gaz et de pous- kurzem in den Gas- und Staubwolken dieser wavelengths but become visible at infrared sières dans cette région éloignée de 5000 5000 Lichtjahre entfernten Gegend ent- wavelengths where the obscuration is sub- années-lumière, sont extrêmement enfouies standenen Sterne sind immer noch stark stantially lower. The diffuse radiation is et ne peuvent être vues à des longueurs verdunkelt und bei optischen Wellenlängen d’onde visibles. Elles deviennent visibles en mostly atomic and molecular hydrogen line unsichtbar; sie werden jedoch im Infraroten emission. The field of view is 2.5 × 2.5 ar- infrarouge parce que l’obscuration y est sichtbar, da hier die Absorption deutlich cmin with N at the top and E to the left and nettement plus faible. Les radiations dif- the image quality is set by the FWHM see- fuses sont surtout des raies d’émission geringer ist. Die diffuse Strahlung ist meist ing of 0.4″. d’hydrogène atomiques et moléculaire. Le Linienemission von atomarem und moleku- champ de vue est de 2.5′ × 2.5′ avec le nord larem Wasserstoff. Das Bildfeld ist 2,5′ × en haut et l’est à gauche. La qualité d’ima- 2,5′ groß, Norden ist oben und Osten links; ge est limitée par le seeing à 0.4″. die Bildqualität ist durch das Seeing mit 0,4″ Halbwertsbreite begrenzt. Annual Report / Rapport annuel / Jahresbericht 1998 presented to the Council by the Director General présenté au Conseil par le Directeur général dem Rat vorgelegt vom Generaldirektor Prof. Dr. R. Giacconi EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l’Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre Table Table Inhalts- of Contents des matières verzeichnis FOREWORD . 5 PRÉFACE . 5 VORWORT . 5 INTRODUCTION . 9 INTRODUCTION . 9 EINLEITUNG . 9 RESEARCH HIGHLIGHTS . 13 POINTS CULMINANTS HÖHEPUNKTE Symposia and Workshops . 29 DE RECHERCHE . 13 DER FORSCHUNG . 13 Conférences et colloques . 29 Konferenzen und Workshops . 29 ST–ECF . 31 ST–ECF . 31 ST–ECF . 31 FACILITIES . 35 INSTALLATIONS . 35 EINRICHTUNGEN . 35 VLT . 35 VLT . 35 VLT . 35 VLT Instruments . 39 Instruments VLT . 39 VLT-Instrumentierung . 39 VLT Interferometer . 43 L’interférométrie du VLT . 43 VLT-Interferometer . 43 La Silla Observatory . 46 Observatoire de La Silla . 46 Observatorium La Silla . 46 Office of the VLT Programme Bureau du « VLT Programme Büro des VLT-Programm- Scientist . 53 Scientist » . 53 wissenschaftlers . 53 DATA MANAGEMENT GESTION DE DONNÉES DATENVERWALTUNG AND OPERATIONS . 56 ET OPÉRATIONS . 56 UND BETRIEB . 56 Systems Engineering Group . 56 Groupe ingénierie système . 56 „System Engineering“-Gruppe . 56 Science Archive Group . 57 Le Groupe des archives „Science Archive“-Gruppe . 57 The User Support Group (USG) 59 scientifiques . 57 „User Support“-Gruppe (USG) . 59 Data Pipeline Group . 62 Le groupe de support aux „Data Pipeline“-Gruppe . 62 Data Flow Operations . 63 utilisateurs (USG) . 59 „Data Flow Operations“-Gruppe 63 POSSII Survey . 64 Groupe pipeline de données . 62 POSSII-Himmels- Opérations de flot de donnés . 63 durchmusterung . 64 L’étude POSSII . 64 RELATIONS WITH CHILE . 65 RELATIONS AVEC LE CHILI . 65 BEZIEHUNGEN ZU CHILE . 65 OUTREACH ACTIVITIES . 67 EDUCATION ET RELATIONS BILDUNG UND PUBLIQUES . 67 ÖFFENTLICHKEITSARBEIT . 67 GOVERNING BODIES . 71 CORPS DIRIGEANTS . 71 FÜHRUNGSGREMIEN . 71 Council . 71 Le Conseil . 71 Der Rat . 71 Finance Committee . 73 Comité des Finances . 73 Finanzausschuß . 73 Scientific Technical Committee . 74 Comité scientifique et technique . 74 Wissenschaftlich- Technischer Ausschuß . 74 ADMINISTRATION . 77 ADMINISTRATION . 77 VERWALTUNG . 77 Appendix I – Summary of Use of Annexe I – Résumé de l’utilisation Anhang I – Zusammenfassung Telescopes by Discipline . 85 des télescopes par discipline . 85 der Teleskopbenutzung nach Appendix II – Publications . 89 Annexe II – Publications . 89 Kategorien . 85 Appendix III – Council and Annexe III – Membres du Conseil Anhang II – Veröffentlichungen . 89 Committee Members in 1999 . .111 et des Comités en 1999 . .111 Anhang III – Rats- und Ausschußmitglieder für 1999 . .111 3 Foreword Préface Vorwort This present Annual Report covers a Le présent Rapport annuel couvre une Der vorliegende Jahresbericht umfaßt crucial year in the history of the Euro- année cruciale dans l’histoire de l’Ob- ein entscheidendes Jahr in der Ge- pean Southern Observatory (ESO). servatoire Européen Austral (ESO). schichte der Europäischen Südstern- warte (ESO). Following a decade of hard work, “First Après une décennie de dur labeur, la Nach einem Jahrzehnt harter Arbeit sah Light” was successfully achieved for « première lumière » a été obtenue avec das erste der vier Teleskope des „Very the first of the four 8.2-m VLT Unit succès au premier des télescopes uni- Large Telescope“ (VLT) auf Paranal er- Telescopes at Paranal. Images of great taire de 8,2 m du VLT, à Paranal. Les folgreich erstes Licht. Bilder von gro- beauty document that this incredibly images d’une grande beauté, montrant ßer Schönheit beeindruckten uns alle complex product of state-of-the-art que ce produit d’une incroyable com- und zeigten, daß sich dieses unglaub- technology is performing according to plexité, à la pointe de la technologie, lich komplexe Produkt nach dem letz- expectations and impressed us all. The fonctionne comme prévu, nous ont tous ten Stand der Technik wie erwartet ver- news about the first results from impressionnés. La nouvelle sur ces pre- hält. Die Meldungen über die ersten Er- Europe’s new front-line research facil- miers résultats provenant du centre de gebnisse von Europas neuer führender ity were well received in all places, in recherche de pointe européen, a été Forschungseinrichtung wurden überall political and administrative circles of partout bien accueillie, dans les mi- gut aufgenommen, sowohl in den Krei- the ESO member states, as well as by lieux politiques et administratifs des sen von Politik und Verwaltung als the scientists, the media and the public. pays membres de l’ESO, ainsi que par auch von Wissenschaftlern, den Me- les scientifiques, les médias et le pu- dien und der Öffentlichkeit. blique. I often think about that memorable Je pense souvent à cette session mémo- Mir kommt oft jene denkwürdige Rats- Council session in December 1987 rable du Conseil de décembre 1987, sitzung vom Dezember 1987 in den when we, as delegates of our respective quand nous, en tant que délégués de nos Sinn, in der wir, die Vertreter unserer countries, gave the green light for the pays respectifs, avons donné le feu vert jeweiligen Staaten, grünes Licht für das VLT project. The decision about a au projet VLT. La décision sur ce défi VLT-Projekt gaben. Es war erwartet multinational endeavour of this scope d’ampleur internationale, d’une telle worden, daß die Entscheidung über ein and size was not expected to be easy, taille et ambition ne fut pas facile. Ce- multinationales Unternehmen dieser but that meeting was carried by a joint pendant, cette réunion a profité d’une Art und Größe nicht leichtfallen würde, feeling of a unique and historical ambiance exceptionnelle, chacun ayant doch diese Sitzung wurde von dem ge- chance. It was a challenge with certain conscience du caractère unique et his- meinsamen Gefühl getragen, daß eine unknowns that, if properly executed, torique du moment. C’était un défi einmalige und historische Gelegenheit would lead to scientific and technolog- avec quelques incertitudes, mais, mené bestand. Es war eine Herausforderung ical benefits of great value for all in- à bien, il pouvait profiter à toutes les mit gewissen Unbekannten, die, falls volved. parties impliquées, tant du point de vue richtig durchgeführt, zu großem wissen- scientifique que technologique. schaftlichen und technologischen Nut- zen für alle Beteiligten führen würde. ESO and its staff carried through this L’ESO et son personnel ont mené à ESO und seine Belegschaft führten die- difficult task in a professional and ded- bien une tâche difficile d’une manière se schwierige Aufgabe auf professio- icated manner. As predicted, this long professionnelle et dédiée. Comme pré- nelle Weise und mit Hingabe aus. Wie process was not entirely without prob- vu, ce long processus n’a pas été sans vorhersehbar war dieser lange Prozeß lems, political and technical, but it was difficultés, aussi bien politiques que nicht ganz ohne Probleme, politisch carried all the way by all partners, in techniques. Mais il a été mené à bien wie technisch, wurde aber immer von the good spirit of mutual respect and par tous les partenaires, dans un esprit allen Partnern im guten Geist gegensei- support.
Recommended publications
  • Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
    The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al.
    [Show full text]
  • The AAVSO DSLR Observing Manual
    The AAVSO DSLR Observing Manual AAVSO 49 Bay State Road Cambridge, MA 02138 email: [email protected] Version 1.2 Copyright 2014 AAVSO Foreword This manual is a basic introduction and guide to using a DSLR camera to make variable star observations. The target audience is first-time beginner to intermediate level DSLR observers, although many advanced observers may find the content contained herein useful. The AAVSO DSLR Observing Manual was inspired by the great interest in DSLR photometry witnessed during the AAVSO’s Citizen Sky program. Consumer-grade imaging devices are rapidly evolving, so we have elected to write this manual to be as general as possible and move the software and camera-specific topics to the AAVSO DSLR forums. If you find an area where this document could use improvement, please let us know. Please send any feedback or suggestions to [email protected]. Most of the content for these chapters was written during the third Citizen Sky workshop during March 22-24, 2013 at the AAVSO. The persons responsible for creation of most of the content in the chapters are: Chapter 1 (Introduction): Colin Littlefield, Paul Norris, Richard (Doc) Kinne, Matthew Templeton Chapter 2 (Equipment overview): Roger Pieri, Rebecca Jackson, Michael Brewster, Matthew Templeton Chapter 3 (Software overview): Mark Blackford, Heinz-Bernd Eggenstein, Martin Connors, Ian Doktor Chapters 4 & 5 (Image acquisition and processing): Robert Buchheim, Donald Collins, Tim Hager, Bob Manske, Matthew Templeton Chapter 6 (Transformation): Brian Kloppenborg, Arne Henden Chapter 7 (Observing program): Des Loughney, Mike Simonsen, Todd Brown Various figures: Paul Valleli Clear skies, and Good Observing! Arne Henden, Director Rebecca Turner, Operations Director Brian Kloppenborg, Editor Matthew Templeton, Science Director Elizabeth Waagen, Senior Technical Assistant American Association of Variable Star Observers Cambridge, Massachusetts June 2014 i Index 1.
    [Show full text]
  • HST Data Handbook for NICMOS
    Version 7.0 April, 2007 HST Data Handbook for NICMOS Space Telescope Science Institute 3700 San Martin Drive Baltimore, Maryland 21218 [email protected] Operated by the Association of Universities for Research in Astronomy, Inc., for the National Aeronautics and Space Administration User Support For prompt answers to any question, please contact the STScI Help Desk. • E-mail: [email protected] • Phone: (410) 338-1082 (800) 544-8125 (U.S., toll free) World Wide Web Information and other resources are available on the Web site: • URL: http://www.stsci.edu. Revision History Version Date Editors 7.0 April 2007 Helene McLaughlin & Tommy Wiklind 6.0 July 2004 Bahram Mobasher & Erin Roye, Editors, NICMOS Data Handbook, Diane Karakla, Chief Editor and Susan Rose, Technical Editor, HST Data Handbook 5.0 January 2002 Mark Dickinson 4.0 December 1999 Mark Dickinson 3.0 October 1997 Daniela Calzetti Contributors STScI NICMOS Group (past & present members), including: Santiago Arribas, Eddie Bergeron, Torsten Boeker, Howard Bushouse, Daniela Calzetti, Luis Colina, Mark Dickinson, Sherie Holfeltz, Lisa Mazzuca, Bahram Mobasher, Keith Noll, Antonella Nota, Erin Roye, Chris Skinner, Al Schultz, Anand Sivaramakrishnan, Megan Sosey, Alex Storrs, Anatoly Suchkov, Chun Xu. ST-ECF: Wolfram Freudling. Send comments or corrections to: Space Telescope Science Institute 3700 San Martin Drive Baltimore, Maryland 21218 E-mail:[email protected] Table of Contents Preface .....................................................................................xi Part I: Introduction to Reducing the HST Data Chapter 1: Getting HST Data............................. 1-1 1.1 Archive Overview ....................................................... 1-2 1.1.1 Archive Registration................................................. 1-3 1.1.2 Archive Documentation and Help ............................ 1-4 1.2 Getting Data with StarView.....................................
    [Show full text]
  • Luminous Blue Variables
    Review Luminous Blue Variables Kerstin Weis 1* and Dominik J. Bomans 1,2,3 1 Astronomical Institute, Faculty for Physics and Astronomy, Ruhr University Bochum, 44801 Bochum, Germany 2 Department Plasmas with Complex Interactions, Ruhr University Bochum, 44801 Bochum, Germany 3 Ruhr Astroparticle and Plasma Physics (RAPP) Center, 44801 Bochum, Germany Received: 29 October 2019; Accepted: 18 February 2020; Published: 29 February 2020 Abstract: Luminous Blue Variables are massive evolved stars, here we introduce this outstanding class of objects. Described are the specific characteristics, the evolutionary state and what they are connected to other phases and types of massive stars. Our current knowledge of LBVs is limited by the fact that in comparison to other stellar classes and phases only a few “true” LBVs are known. This results from the lack of a unique, fast and always reliable identification scheme for LBVs. It literally takes time to get a true classification of a LBV. In addition the short duration of the LBV phase makes it even harder to catch and identify a star as LBV. We summarize here what is known so far, give an overview of the LBV population and the list of LBV host galaxies. LBV are clearly an important and still not fully understood phase in the live of (very) massive stars, especially due to the large and time variable mass loss during the LBV phase. We like to emphasize again the problem how to clearly identify LBV and that there are more than just one type of LBVs: The giant eruption LBVs or h Car analogs and the S Dor cycle LBVs.
    [Show full text]
  • Human Issues Related to Spacecraft Vibration During Ascent
    Human Issues related to Spacecraft Vibration during Ascent Consultant Report to the Constellation Program Standing Review Board Jonathan B. Clark M.D., M.P.H. Suite NA 425 One Baylor Plaza Baylor College of Medicine Houston TX 77030-3498 1731 Sunset Blvd Houston TX 77005 713 859 1381 281 989 8721 [email protected] [email protected] Opinions expressed herein are those of the author and do not reflect the views of the National Space Biomedical Research Institute (NSBRI), Baylor College of Medicine (BCM), the University of Texas Medical Branch (UTMB), or the National Aeronautics and Space Administration (NASA). Human Issues related to Spacecraft Vibration during Ascent Consultant Report to the Constellation Program Standing Review Board Jonathan B. Clark M.D., M.P.H. Opinions expressed herein are those of the author and do not reflect the views of the National Space Biomedical Research Institute (NSBRI), Baylor College of Medicine (BCM), the University of Texas Medical Branch (UTMB), or the National Aeronautics and Space Administration (NASA). Pogo in Liquid Fueled Rocket Motors The pogo phenomenon, or fuel pump inlet pressure fluctuation/ cavitation due to tuning feed line resonant frequencies was a major concern in the early space program. Pump tests showed that as inlet pressures were reduced toward cavitation, the pump started acting as an amplifier, causing large oscillations in the thrust chamber pressure. As the rocket engine thrust develops, liquid propellant is cyclically forced into the turbopump. This fluctuating fluid pressure is converted into an unintended and variable increase in engine thrust, with the net effect being longitudinal axis vibration that could result in spacecraft structural failure.
    [Show full text]
  • 14476 (Stsci Edit Number: 4, Created: Wednesday, September 7, 2016 4:28:02 PM EST) - Overview
    Proposal 14476 (STScI Edit Number: 4, Created: Wednesday, September 7, 2016 4:28:02 PM EST) - Overview 14476 - A collision reversal in HD 5980 Cycle: 24, Proposal Category: GO (Availability Mode: SUPPORTED) INVESTIGATORS Name Institution E-Mail Dr. Yael Naze (PI) (ESA Member) (Contact) Universite de Liege [email protected] Dr. D. John Hillier (CoI) University of Pittsburgh [email protected] Dr. Gloria Koenigsberger (CoI) (Contact) Universidad Nacional Autonoma de Mexico (UNAM) [email protected] Dr. Julian M. Pittard (CoI) (ESA Member) University of Leeds [email protected] Dr. Michael F. Corcoran (CoI) Universities Space Research Association [email protected] Dr. Gregor Rauw (CoI) (ESA Member) Universite de Liege [email protected] VISITS Visit Targets used in Visit Configurations used in Visit Orbits Used Last Orbit Planner Run OP Current with Visit? 01 (1) HD-5980 STIS/CCD 2 07-Sep-2016 17:28:00.0 yes CCDFLAT STIS/FUV-MAMA 2 Total Orbits Used ABSTRACT HD 5980 provides a unique laboratory for studying the properties of wind-wind collisions. It contains one of only two binary systems having a WR- star in orbit with a LBV. The latter star has been observed to undergo major changes in its wind structure over the past 35 years, implying changes in the geometry and emitting conditions of the wind-wind collision region. Ten years ago, when the LBV wind was very strong, XMM observations revealed X-ray emission consistent with the shock cone wrapping around the WR component. Since then, the wind strength has significantly declined, implying that the collision shock cone may be inverting its orientation.
    [Show full text]
  • Galaxy Cluster's Rotation
    Mon. Not. R. Astron. Soc. 000, 000{000 (0000) Printed 14 June 2018 (MN LATEX style file v2.2) Galaxy cluster's rotation M. Manolopoulou1;2?, M. Plionis2;3 1 Institute for Astronomy, The University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK. 2 Section of Astrophysics, Astronomy and Mechanics, Department of Physics, Aristotle University of Thessaloniki, 54 124, Thessaloniki, Greece. 3 Instituto Nacional de Astrof´ısica Optica y Electr´onica, AP 51 y 216, 72000, Puebla, M´exico. 14 June 2018 ABSTRACT We study the possible rotation of cluster galaxies, developing, testing and applying a novel algorithm which identifies rotation, if such does exist, as well as its rotational centre, its axis orientation, rotational velocity amplitude and, finally, the clockwise or counterclockwise direction of rotation on the plane of the sky. To validate our algo- rithms we construct realistic Monte Carlo mock rotating clusters and confirm that our method provides robust indications of rotation. We then apply our methodology on a sample of Abell clusters with z . 0:1 with member galaxies selected from the Sloan Digital Sky Survey (SDSS) DR10 spectroscopic data base. After excluding a number of substructured clusters, which could provide erroneous indications of rotation, and taking into account the expected fraction of misidentified coherent substructure ve- locities for rotation, provided by our Monte-Carlo simulation analysis, we find that ∼ 23% of our clusters are rotating under a set of strict criteria. Loosening the strict- ness of the criteria, on the expense of introducing spurious rotation indications, we find this fraction increasing to ∼ 28%.
    [Show full text]
  • Fundamental Parameters of Wolf-Rayet Stars VI
    Astron. Astrophys. 320, 500–524 (1997) ASTRONOMY AND ASTROPHYSICS Fundamental parameters of Wolf-Rayet stars VI. Large Magellanic Cloud WNL stars? P.A.Crowther and L.J. Smith Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK Received 5 February 1996 / Accepted 26 June 1996 Abstract. We present a detailed, quantitative study of late WN Key words: stars: Wolf-Rayet;mass-loss; evolution; fundamen- (WNL) stars in the LMC, based on new optical spectroscopy tal parameters – galaxies: Magellanic Clouds (AAT, MSO) and the Hillier (1990) atmospheric model. In a pre- vious paper (Crowther et al. 1995a), we showed that 4 out of the 10 known LMC Ofpe/WN9 stars should be re-classified WN9– 10. We now present observations of the remaining stars (except the LBV R127), and show that they are also WNL (WN9–11) 1. Introduction stars, with the exception of R99. Our total sample consists of 17 stars, and represents all but one of the single LMC WN6– Quantitative studies of hot luminous stars in galaxies are im- 11 population and allows a direct comparison with the stellar portant for a number of reasons. First, and probably foremost, parameters and chemical abundances of Galactic WNL stars is the information they provide on the effect of the environment (Crowther et al. 1995b; Hamann et al. 1995a). Previously un- on such fundamental properties as the mass-loss rate and stellar published ultraviolet (HST-FOS, IUE-HIRES) spectroscopy are evolution. In the standard picture (e.g. Maeder & Meynet 1987) presented for a subset of our programme stars.
    [Show full text]
  • Appendix A: Scientific Notation
    Appendix A: Scientific Notation Since in astronomy we often have to deal with large numbers, writing a lot of zeros is not only cumbersome, but also inefficient and difficult to count. Scientists use the system of scientific notation, where the number of zeros is short handed to a superscript. For example, 10 has one zero and is written as 101 in scientific notation. Similarly, 100 is 102, 100 is 103. So we have: 103 equals a thousand, 106 equals a million, 109 is called a billion (U.S. usage), and 1012 a trillion. Now the U.S. federal government budget is in the trillions of dollars, ordinary people really cannot grasp the magnitude of the number. In the metric system, the prefix kilo- stands for 1,000, e.g., a kilogram. For a million, the prefix mega- is used, e.g. megaton (1,000,000 or 106 ton). A billion hertz (a unit of frequency) is gigahertz, although I have not heard of the use of a giga-meter. More rarely still is the use of tera (1012). For small numbers, the practice is similar. 0.1 is 10À1, 0.01 is 10À2, and 0.001 is 10À3. The prefix of milli- refers to 10À3, e.g. as in millimeter, whereas a micro- second is 10À6 ¼ 0.000001 s. It is now trendy to talk about nano-technology, which refers to solid-state device with sizes on the scale of 10À9 m, or about 10 times the size of an atom. With this kind of shorthand convenience, one can really go overboard.
    [Show full text]
  • Astrometry and Optics During the Past 2000 Years
    1 Astrometry and optics during the past 2000 years Erik Høg Niels Bohr Institute, Copenhagen, Denmark 2011.05.03: Collection of reports from November 2008 ABSTRACT: The satellite missions Hipparcos and Gaia by the European Space Agency will together bring a decrease of astrometric errors by a factor 10000, four orders of magnitude, more than was achieved during the preceding 500 years. This modern development of astrometry was at first obtained by photoelectric astrometry. An experiment with this technique in 1925 led to the Hipparcos satellite mission in the years 1989-93 as described in the following reports Nos. 1 and 10. The report No. 11 is about the subsequent period of space astrometry with CCDs in a scanning satellite. This period began in 1992 with my proposal of a mission called Roemer, which led to the Gaia mission due for launch in 2013. My contributions to the history of astrometry and optics are based on 50 years of work in the field of astrometry but the reports cover spans of time within the past 2000 years, e.g., 400 years of astrometry, 650 years of optics, and the “miraculous” approval of the Hipparcos satellite mission during a few months of 1980. 2011.05.03: Collection of reports from November 2008. The following contains overview with summary and link to the reports Nos. 1-9 from 2008 and Nos. 10-13 from 2011. The reports are collected in two big file, see details on p.8. CONTENTS of Nos. 1-9 from 2008 No. Title Overview with links to all reports 2 1 Bengt Strömgren and modern astrometry: 5 Development of photoelectric astrometry including the Hipparcos mission 1A Bengt Strömgren and modern astrometry ..
    [Show full text]
  • Curriculum Vitae John P
    Curriculum Vitae John P. Blakeslee National Research Council of Canada Phone: 1-250-363-8103 Herzberg Astronomy & Astrophysics Programs Fax: 1-250-363-0045 5071 West Saanich Road Cell: 1-250-858-1357 Victoria, B.C. V9E 2E7 Email: [email protected] Canada Citizenship: USA Education 1997 Ph.D., Physics, Massachusetts Institute of Technology (supervisor: Prof. John Tonry) 1991 B. A., Physics, University of Chicago (Honors; supervisor: Prof. Donald York) Employment History 2007 – present Astronomer, Senior Research Officer NRC Herzberg Institute of Astrophysics 2008 – present Adjunct Associate Professor Department of Physics, University of Victoria 2008 – 2013 Adjunct Professor Washington State University 2005 – 2007 Assistant Professor of Physics Washington State University 2004 – 2005 Research Scientist Johns Hopkins University 2000 – 2004 Associate Research Scientist Johns Hopkins University 1999 – 2000 Postdoctoral Research Associate University of Durham, U.K. 1996 – 1999 Fairchild Postdoctoral Scholar California Institute of Technology Fellowships and Awards 2004 Ernest F. Fullam Award for Innovative Research in Astronomy, Dudley Observatory 2003 NASA Certificate for contributions to the success of HST Servicing Mission 3B 1996 – 1999 Sherman M. Fairchild Postdoctoral Fellowship in Astronomy, Caltech Professional Service 2016 – present Canadian Large Synoptic Survey Telescope (LSST) Consortium, Co-PI 2014 – present Chair, NOAO Time Allocation Committee (TAC) Extragalactic Panel 2008 – present National Representative, Gemini International
    [Show full text]
  • Overview of GX Launch Services by GALEX Koji Sato∗, Yoshirou Kondou
    Acta Astronautica 59 (2006) 381–391 www.elsevier.com/locate/actaastro Overview of GX launch services by GALEX Koji Sato∗, Yoshirou Kondou Galaxy Express Corporation, Tokyo, Japan Available online 19 May 2006 Abstract Galaxy Express Corporation (GALEX) is a launch service company in Japan to develop a medium size rocket, GX rocket and to provide commercial launch services for medium/small low Earth orbit (LEO) and Sun synchronous orbit (SSO) payloads with a future potential for small geo-stationary transfer orbit (GTO). It is GALEX’s view that small/medium LEO/SSO payloads compose of medium scaled but stable launch market due to the nature of the missions. GX rocket is a two-stage rocket of well flight proven liquid oxygen (LOX)/kerosene booster and LOX/liquid natural gas (LNG) upper stage. This LOX/LNG propulsion under development by Japan’s Aerospace Exploration Agency (JAXA), is robust with comparable performance as other propulsions and have future potential for wider application such as exploration programs. GX rocket is being developed through a joint work between the industries and GX rocket is applying a business oriented approach in order to realize competitive launch services for which well flight proven hardware and necessary new technology are to be introduced as much as possible. It is GALEX’s goal to offer “Easy Access to Space”, a highly reliable and user-friendly launch services with a competitive price. GX commercial launch will start in Japanese fiscal year (JFY) 2007–2008. © 2006 Elsevier Ltd. All rights reserved. 1. Background of GX rocket (R&D) budget was filed to the Ministry of Finance (MOF) to start the R&D as “Advance Technology The origin of GX rocket can be traced back to Demonstration Rocket Program” from JFY1998.
    [Show full text]