Report on the Management of European Astronomy
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European Organisation for Astronomical Research in the Southern Hemisphere ESO
European Organisation for Astronomical Research in the Southern Hemisphere ESO Description The ESO (European Organisation for Astronomical Research in the Southern Hemisphere) is a globally recognised intergovernmental body that builds and operates Earth-based astronomy research facilities and involves the majo- rity of the European States. Currently, the ESO has 14 Member States: Austria, Belgium, the Czech Republic, Den- mark, Finland, France, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United King- dom. It was established in 1962 and its headquarters are in Garching, Germany. The German offices are responsible for managing and carrying out most of the administrative, scientific and tech- nological tasks of the Organisation. Garching has laboratories which are used to develop technologies applied to the 94 sophisticated scientific observation instruments used in the telescopes, as well as integration rooms for them. It is also home to the ESO scientific archive which contains all astronomical observation data obtained at the observa- tories, which can be accessed on the Internet. e (ESO) ESO observation programme: instrumental equipment n Hemispher her The ESO selected Chile to build the first observatory, primarily due to the exceptional atmospheric conditions for astronomy and the possibility of accessing the sky in the Southern Hemisphere. The telescopes are set up in three he Sout locations: La Silla, Cerro Paranal and El Llano de Chajnantor. Although the ESO identifies its operational facilities in h in t Chile as a single observatory for functional purposes, they should be considered separately for description purpo- esearc ses. onomical R tr La Silla or As La Silla, located 600 km north of Santiago de Chile at an altitude of 2,400 m, was the site chosen by the ESO to set up its first facilities. -
Historical & Cultural Astronomy
Historical & Cultural Astronomy Series Editor: WAYNE ORCHISTON, University of Southern Queensland, Australia ([email protected]) MARC ROTHENBERG, Smithsonian Institution (retired), USA ([email protected]) CLIFFORD CUNNINGHAM, University of Southern Queensland, Australia ([email protected]) Editorial Board: JAMES EVANS, University of Puget Sound, USA MILLER GOSS, National Radio Astronomy Observatory, USA DUANE HAMACHER, Monash University, Australia JAMES LEQUEUX, Observatoire de Paris, France SIMON MITTON, St. Edmund’s College Cambridge University, UK CLIVE RUGGLES, University of Leicester, UK VIRGINIA TRIMBLE, University of California Irvine, USA GUDRUN WOLFSCHMIDT, Institute for History of Science and Technology, Germany TRUDY BELL, Sky & Telescope, USA More information about this series at http://www.springer.com/series/15156 Ileana Chinnici • Guy Consolmagno Editors Angelo Secchi and Nineteenth Century Science The Multidisciplinary Contributions of a Pioneer and Innovator Editors Ileana Chinnici Guy Consolmagno INAF Vatican Observatory Osservatorio Astronomico di Palermo Vatican City State, Holy See Palermo, Italy ISSN 2509-310X ISSN 2509-3118 (electronic) Historical & Cultural Astronomy ISBN 978-3-030-58383-5 ISBN 978-3-030-58384-2 (eBook) https://doi.org/10.1007/978-3-030-58384-2 © Springer Nature Switzerland AG 2021 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifcally the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microflms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. -
Legri Operations. Detectors and Detector Stability
LEGRI OPERATIONS. DETECTORS AND DETECTOR STABILITY V. REGLERO1, F. BALLESTEROS3,P.BLAY1, E. PORRAS2, F. SÁNCHEZ2 and J. SUSO1 1 GACE, Instituto de Ciencias de los Materiales, Universidad de Valencia, P.O. Box 2085, 46071 Valencia, Spain 2 Instituto de Fisica Corpuscular, Spanish Council of Scientific Research - University of Valencia, Edificio de Institutos de Paterna, P.0. Box 2085, E-4 6071 Valencia, Spain 3 Centro de Astrobiología (CAB), Instituto Nacional de Técnica aeorespacial (INTA), Ctra. de Ajalvir Km. 14, Torrejón de Ardoz, Madrid, Spain Abstract. Two years after launch (04.21.97), LEGRI is operating on Minisat-01 in a LEO orbit. The LEGRI detector plane is formed by two type of gamma-ray solid state detectors: HgI2 and CdZnTe. Detectors are embedded in a box containing the FEE and DFE electronics. This box provides an effective detector passive shielding. Detector plane is multiplexed by a Coded Aperture System ◦ ◦ located at 54 cm and a Ta Collimator with a FCFOV of 22 and 2 angular resolution. The aim of this paper is to summarize the detector behaviour in three different time scales: before launch, during the in-orbit check-out period (IOC), and after two years of routine operation in space. Main results can be summarized as follows: A large fraction of the HgI2 detectors presented during LEGRI IOC very high count ratios from their first switch-on (May 1997). Therefore, they induced saturation in the on-board mass memory. After some unsuccessful attempts to reduce the count ratios by setting up different thresholds during LEGRI IOC, all of them were switched off except nine detectors in column 4, with a higher degree of stability. -
Astronomy and Astrophysics in Comunidad De Madrid: Research and Technology
Astronomy and Astrophysics in Comunidad de Madrid: Research and Technology Prepared by the AstroMadrid Steering Committee v 1.0 October 2013 AstroMadrid: Astrophysics and technology development in Comunidad de Madrid is funded by Consejería de Juventud, Educación y Deportes at Comunidad de Madrid, with reference S2009/ESP-1496 INDEX - Introduction - Research groups Universidad Complutense de Madrid. Department of Earth Physics, Astronomy and Astrophysics II. Extragalactic Astrophysics. Universidad Complutense de Madrid. Department of Earth Physics, Astronomy and Astrophysics II. Stellar Astrophysics. Universidad Complutense de Madrid. Department of Earth Physics, Astronomy and Astrophysics II. Instrumentation. Universidad Complutense de Madrid. Department of Atomic, Molecular and Nuclear Physics. Astroparticle Physics. Universidad Complutense de Madrid. Department of Earth Physics, Astronomy and Astrophysics I. Astronomy and Geodesy. AEGORA (Astronomía Espacial y Gestión Óptima de Recursos Astronómicos). Universidad Autónoma de Madrid. Department of Theoretical Physics. Astrophysics Group Universidad de Alcalá. Space Plasmas & Astroparticle Group. Universidad de Alcalá. Space Research Group (SRG-UAH). Universidad Politécnica de Madrid. Faculty of Computing Sciences. Collaborative Learning Group Ciclope. Centro de Astrobiología (CSIC-INTA). Department of Astrophysics. Centro de Astrobiología (CSIC-INTA). Department of Astrophysics. Virtual Observatory. Centro de Astrobiología (CSIC-INTA). Department of Instrumentation. Instituto Nacional -
Report Annexes
International Astronomical Union XXVth General Assembly July 13-26 2003 Sydney, Australia Contents Annex 1 Timeline of Events Annex 2 National Organizing Committee Members Annex 3 Opening Ceremony Annex 4 Student-Volunteer Program Annex 5 Tours Program Annex 6 The Australian Festival of Astronomy Annex 7 Associated Public Events Annex 8 “Astronomy on the Go” Annex 9 Room Allocations Annex 10 Astro Expo Exhibitor listing Annex 11 Industry Day Annex 12 Delegate List Annex 13 The Australian Festival of Astronomy - Marketing Report ANNEX 1 INTERNATIONAL ASTRONOMY UNION 25TH GENERAL ASSEMBLY Timeline of Events 1994 At Don Mathewson’s invitation, IAU Executive Committee members visit Australia Jeremy Mould heads move to bid for 2003 GA in Sydney 1995 Bid for 2003 GA in Sydney submitted to IAU 1997 Aug Sydney awarded 2003 GA during Kyoto GA Jeremy Mould calls for expressions of interest to form LOC (NOC) 1998 Apr John Norris convenes 1st meeting of NOC NOC decide on SCEC for GA venue Convention Centre booked for period July 13-26, 2003? Sep Lawrence Cram takes over Chair for 5th NOC meeting Sep NOC call for tenders for provision of PCO services Dec 7th NOC meeting spent visiting two candidate PCO companies 1999 Mar Raymond Haynes takes over NOC Chair for 8th NOC meeting Jun ICMS chosen as GA PCO at the 9th NOC meeting Jun Use of Sydney Opera House for Opening Ceremony considered Oct Preliminary budget tabled at 11th NOC meeting 2000 May Logo design selected at 14th NOC meeting Aug Sydney GA display and David Malin presentation at Manchester -
Unified View of Stellar Winds in Massive X-Ray Binaries
Unified View of Stellar Winds in Massive X-ray Binaries Team Leader: S. Mart´ınez Nu´ nez,˜ University of Alicante, Spain. Abstract We propose to bring together specialists for winds from massive stars and observers of High-Mass X-ray Binary (HMXB) systems for two meetings at ISSI in order to review the state-of-the-art in observations and modeling and to develop a unified view on the physics of the stellar winds in these systems. The aim of the meetings is to define a general strategy on what can be learned from each other and also to explicitly advance towards a unified picture of massive star outflows in single stars and X-ray binaries. 1 Scientific rationale, goals and timeliness of the project The birth, life, and death of massive stars (Minitial > 10 M ) are deeply interwoven with the evolution ⊙ of star clusters and galaxies. Massive stars generate most of the ultraviolet radiation of galaxies – the whole Universe was re-ionized with the help of the first (super)massive stars – and power their infrared luminosities. Massive star winds and final explosions as supernovae provide a significant input of me- chanical and radiative energy into the interstellar medium, and play a crucial role in the evolution of star clusters and galaxies (Kudritzki 2002). Thus, massive stars are among the most important cosmic en- gines: they trigger the star formation and, together with low-mass stars, enrich the interstellar medium with the heavy elements but on short time scales, ultimately leading to formation of Earth-like plan- ets and development of life. -
The EM Imaging Reconstruction Method in C-Ray Astronomy
Nuclear Instruments and Methods in Physics Research B 145 (1998) 469±481 The EM imaging reconstruction method in c-ray astronomy Fernando Jesus Ballesteros Rosello a,*, Filomeno Sanchez Martõnez a, Võctor Reglero Velasco b a Instituto de Fõsica Corpuscular, University of Valencia ± CSIC, Dr. Moliner 50, E-46100 Burjassot, Valencia, Spain b Department of Astronomy and Astrophysics, University of Valencia, Dr. Moliner 50, E-46100 Burjassot, Valencia, Spain Received 11 May 1998; received in revised form 14 July 1998 Abstract The simpler imaging reconstruction methods used for c-ray coded mask telescopes are based on correlation methods, very fast and simple-to-use but with limitations in the reconstructed image. To improve these results, other recon- struction methods have been developed, such as the maximum entropy methods or the Iterative Removal Of Sources (IROS). However, such kind of methods are slower and can be impracticable for very complex telescopes. In this paper we present an alternative image reconstruction method, based on an iterative maximum likelihood algorithm called the EM algorithm, easy to implement and that can be successfully used for not very complex coded mask systems, as is the case of the LEGRI telescope. This is the ®rst time this algorithm has been applied in c-ray astronomy. Ó 1998 Elsevier Science B.V. All rights reserved. 1. Introduction incidence angles with regard to the arriving pho- tons, bigger than the critical angle of the re¯ecting When trying to obtain an image of a celestial surface material, de¯ecting the radiation towards a source emitting X or c radiation, classical tele- focus where the detecting surface is. -
Recent Space Weather Advances by Research Community in Italy
ISWI Workshop 2019 ICTP Trieste, Italy Recent Space Weather Advances by Research Community in Italy Y. Migoya-Orué 1, C. Plainaki 2, V. Romano 3,, U. Villante 4 1 ICTP, Trieste, Italy, [email protected], ISWI National co-coordinator 2 ASI – Agenzia Spaziale Italiana, [email protected] Coordinator of ASI Space Weather Working Group 3 INGV, Italy, [email protected] , ISWI National co-coordinator 4 University of L’Aquila, Dept. Physical and Chemical Sciences, L’Aquila, Italy, [email protected], President of SWICO (Italian Space Weather Community) Outline Space weather-related thematic areas • Italian strategic Initiatives • Research and Technology Development in the fields of: o Solar Physics o Interplanetary Space and Solar-Terrestrial Physics o Geomagnetism o Upper Atmosphere Physics ISWI Workshop 2019 ICTP Trieste, Italy Italian Space Weather strategic initiatives Italy at UN – Office for Outer Space Affairs Istituto Nazionale di Geofisica e Vulcanologia INGV and ASI are the Italian representatives at the Space Weather Expert Group of COPUOS (Committee on the Peaceful Uses of Outer Space) Italy at ISWI INGV and ICTP are the Italian co-coordinators in ISWI (International Space Weather Initiative). Italy at SCAR – Scientific Committee for Antarctic Research Italy leads the SCAR expert group called GRAPE (GNSS Research and Application for Polar Environment). GRAPE is a joint GeoSciences and Physical Sciences Expert Group lasting from 2012 to 2020 13 countries are involved (new members are welcome!). Main Objectives -
The Modular X- and Gamma-Ray Sensor (MXGS) of the ASIM Payload on the International Space Station
Space Sci Rev (2019) 215:23 https://doi.org/10.1007/s11214-018-0573-7 The Modular X- and Gamma-Ray Sensor (MXGS) of the ASIM Payload on the International Space Station Nikolai Østgaard1 · Jan E. Balling2 · Thomas Bjørnsen1 · Peter Brauer2 · Carl Budtz-Jørgensen2 · Waldemar Bujwan3 · Brant Carlson1 · Freddy Christiansen2 · Paul Connell4 · Chris Eyles4 · Dominik Fehlker1 · Georgi Genov1 · Pawel Grudzinski´ 3 · Pavlo Kochkin1 · Anja Kohfeldt1 · Irfan Kuvvetli2 · Per Lundahl Thomsen2 · Søren Møller Pedersen2 · Javier Navarro-Gonzalez4 · Torsten Neubert2 · Kåre Njøten1 · Piotr Orleanski3 · Bilal Hasan Qureshi1 · Linga Reddy Cenkeramaddi1 · Victor Reglero4 · Manuel Reina5 · Juan Manuel Rodrigo4 · Maja Rostad1 · Maria D. Sabau5 · Steen Savstrup Kristensen2 · Yngve Skogseide1 · Arne Solberg1 · Johan Stadsnes1 · Kjetil Ullaland1 · Shiming Yang1 Received: 31 August 2018 / Accepted: 18 December 2018 © The Author(s) 2019 Abstract The Modular X- and Gamma-ray Sensor (MXGS) is an imaging and spectral X- and Gamma-ray instrument mounted on the starboard side of the Columbus module on the International Space Station. Together with the Modular Multi-Spectral Imaging Assembly (MMIA) (Chanrion et al. this issue) MXGS constitutes the instruments of the Atmosphere-Space Interactions Monitor (ASIM) (Neubert et al. this issue). The main ob- jectives of MXGS are to image and measure the spectrum of X- and γ -rays from lightning discharges, known as Terrestrial Gamma-ray Flashes (TGFs), and for MMIA to image and perform high speed photometry of Transient Luminous Events (TLEs) and lightning dis- charges. With these two instruments specifically designed to explore the relation between electrical discharges, TLEs and TGFs, ASIM is the first mission of its kind. With an imag- ing system and a large detector area MXGS will, for the first time, allow estimation of the location of the source region and characterization of the energy spectrum of individual events. -
100 Conceptos Básicos De Astronomía
100 Conceptos básicos de Astronomía 100 Conceptos básicos de Astronomía Coordinado por: Julia Alfonso Garzón LAEX, CAB (INTA/CSIC) David Galadí Enríquez Centro Astronómico Hispano-Alemán (Observatorio de Calar Alto) Carmen Morales Durán LAEX, CAB (INTA/CSIC) Instituto Nacional de Técnica Aeroespacial «Esteban Terradas» 1 2 3 4 5 8 6 7 1. Galaxia M51 tomada por el instrumento OSIRIS en el GTC. Créditos: Daniel López (Instituto de Astrofísica de Canarias). 2. Eclipse de Luna en noviembre de 2003. Créditos: Fernando Comerón (Observatorio Europeo Austral). 3. Imagen infrarroja que muestra en falso color la huella dejada por un reciente impacto, posiblemente cometario, en la atmósfera de Júpiter. En azul se ven las regiones más altas: el propio impacto, la Gran Mancha Roja y las nieblas polares. Créditos: Santiago Pérez Hoyos (Universidad del País Vasco). 4. Antena DSS63 de la estación de Robledo de Chavela. Créditos: F. Rojo (MDSCC), Juan Ángel Vaquerizo (Centro de Astrobiología). 5. Nebulosa N44 en la Gran Nube de Magallanes. Créditos: Fernando Comerón (Observatorio Europeo Austral). 6. Nebulosa planetaria NGC 6309. Créditos: Martín A. Guerrero (Instituto de Astrofísica de Andalucía). 7. Trazas de estrellas y telescopio 3,5m del Observatorio de Calar Alto. Créditos: Felix Hormuth (Observatorio de Calar Alto). 8. Ilustración de las instalaciones del Centro Europeo de Astronomía Espacial (ESAC) en Villafranca del Castillo (Madrid). Créditos: Manuel Morales. 100 Conceptos básicos de Astronomía Emilio Alfaro Navarro Mariana Lanzara Julia Alfonso Garzón (coord.) Javier Licandro Goldaracena David Barrado Navascués Javier López Santiago Amelia Bayo Arán Mercedes Mollá Lorente Javier Bussons Gordo Benjamín Montesinos Comino José Antonio Caballero Hernández Carmen Morales Durán (coord.) José R. -
Long-Term X-Ray Variability of Active Galactic Nuclei and X-Ray Binaries
Long-term X-ray variability of Active Galactic Nuclei and X-ray Binaries Dissertation zur Erlangung des Grades eines Doktors der Naturwissenschaften der Fakultät für Mathematik und Physik der Eberhard-Karls-Universität Tübingen vorgelegt von Sara Benlloch García aus Madrid 2004 Selbstverlegt von: S. Benlloch García Tag der mündlichen Prüfung: 28. Oktober 2003 Dekan: Prof. Dr. H. Müther 1. Berichterstatter: Prof. Dr. K. Werner 2. Berichterstatter: PD. Dr. J. Wilms Erweiterte deutsche Zusammenfassung Sara Benlloch García Langzeitvariabilität im Röntgenbereich von Aktiven Galaxienkernen und Röntgendoppelsternen In dieser Dissertation beschäftige ich mich mit der Langzeitvariabilität von zwei Klassen von Röntgenobjekten: Aktiven Galaxiekernen (engl. Active Galac- tic Nuclei, AGN) und Röntgendoppelsternen (engl. X-ray Binaries, XRBs). Variabilität im Röntgenbereich ist ein allgemeines Phänomen in vielen astrono- mischen Quellen. Variabilität ist eine lange bekannte Eigenschaft von AGN, die in allen Wellenlängen und auf Zeitskalen (von Dekaden zu Tagen/Stunden) auf- tritt. Die Veränderungen scheinen aperiodisch zu sein und variable Amplituden zu haben. Es gib einige Berichte über das periodische Verhalten auf Zeitskalen von einigen Kilosekunden in Form sogenannter quasiperiodischer Oszillationen (QPO). Die Bestätigung einiger dieser Modulationen ist jedoch noch unklar (z.B. Priedhorsky & Holt, 1987; Schwarzenberg-Czerny, 1992; Wijers & Pringle, 1999; Ogilvie & Dubus, 2001). In einer kleinen aber wachsenden Zahl von hellen XRBs ist eine dritte (oder “superorbitale”) Periode zusätzlich zu den üblichen Periodizi- täten zu beobachten. Solche langfristigen Veränderungen helfen, Fragen über die Struktur der Akretionsscheiben von Röntgendoppelsternen, das Vorhandenseinei- nes dritten Objektes in solchen Systemen, die intrinsische Variationen aufgrund von Änderung der Massenakretionsrate oder der Opazität im nahe gelegenen be- deckenden Material und über die Natur der nicht immer beobachtbaren transien- ten Quellen zu beantworten (Smale & Lochner, 1992). -
Lower Atmosphere and Pressure Evolution on Pluto from Ground-Based Stellar Occultations, 1988–2016 E
A&A 625, A42 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834281 & © E. Meza et al. 2019 Astrophysics Lower atmosphere and pressure evolution on Pluto from ground-based stellar occultations, 1988–2016 E. Meza1,?, B. Sicardy1, M. Assafin2,3, J. L. Ortiz4, T. Bertrand5, E. Lellouch1, J. Desmars1, F. Forget6, D. Bérard1, A. Doressoundiram1, J. Lecacheux1, J. Marques Oliveira1, F. Roques1, T. Widemann1, F. Colas7, F. Vachier7, S. Renner7,8, R. Leiva9, F. Braga-Ribas1,3,10, G. Benedetti-Rossi3, J. I. B. Camargo3, A. Dias-Oliveira3, B. Morgado3, A. R. Gomes-Júnior3, R. Vieira-Martins3, R. Behrend11, A. Castro Tirado4, R. Duffard4, N. Morales4, P. Santos-Sanz4, M. Jelínek12, R. Cunniffe13, R. Querel14, M. Harnisch15,16, R. Jansen15,16, A. Pennell15,16, S. Todd15,16, V. D. Ivanov17, C. Opitom17, M. Gillon18, E. Jehin18, J. Manfroid18, J. Pollock19, D. E. Reichart20, J. B. Haislip20, K. M. Ivarsen20, A. P. LaCluyze21, A. Maury22, R. Gil-Hutton23, V. Dhillon24,25, S. Littlefair24, T. Marsh26, C. Veillet27, K.-L. Bath28,29, W. Beisker28,29, H.-J. Bode28,29,†, M. Kretlow28,29, D. Herald15,30,31, 15,32,33 15,34 30 29, 29 35 35 36 D. Gault , S. Kerr , H. Pavlov , O. Faragó y, O. Klös , E. Frappa , M. Lavayssière , A. A. Cole , 36 36, 36 9 9 9 9 A. B. Giles , J. G. Greenhill y, K. M. Hill , M. W. Buie , C. B. Olkin , E. F. Young , L. A. Young , L. H. Wasserman37, M. Devogèle37, R. G. French38, F. B. Bianco39,40,41,42, F. Marchis1,43, N.