Stockholm Observatory Annual Report 2006
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JUICE Red Book
ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat. -
Booklet 2008-09.Indd
The Shaw Prize The Shaw Prize is an international award to honour individuals who are currently active in their respective fields and who have achieved distinguished and significant advances, who have made outstanding contributions in culture and the arts, or who in other domains have achieved excellence. The award is dedicated to furthering societal progress, enhancing quality of life, and enriching humanity’s spiritual civilization. Preference will be given to individuals whose significant work was recently achieved. Founder's Biographical Note The Shaw Prize was established under the auspices of Mr Run Run Shaw. Mr Shaw, born in China in 1907, is a native of Ningbo County, Zhejiang Province. He joined his brother’s film company in China in the 1920s. In the 1950s he founded the film company Shaw Brothers (Hong Kong) Limited in Hong Kong. He has been Executive Chairman of Television Broadcasts Limited in Hong Kong since the 1970s. Mr Shaw has also founded two charities, The Sir Run Run Shaw Charitable Trust and The Shaw Foundation Hong Kong, both dedicated to the promotion of education, scientific and technological research, medical and welfare services, and culture and the arts. ~ 1 ~ Message from the Chief Executive I am delighted to congratulate the six distinguished scientists who receive this year’s Shaw Prize. Their accomplishments enrich human knowledge and have a profound impact on the advancement of science. This year, the Shaw Prize recognises remarkable achievements in the areas of astronomy, life science and medicine, and mathematical sciences. The exemplary work and dedication of this year’s recipients vividly demonstrate that constant drive for excellence will eventually bear fruit. -
The Odin Orbital Observatory
A&A 402, L21–L25 (2003) Astronomy DOI: 10.1051/0004-6361:20030334 & c ESO 2003 Astrophysics The Odin orbital observatory H. L. Nordh1,F.vonSch´eele2, U. Frisk2, K. Ahola3,R.S.Booth4,P.J.Encrenaz5, Å. Hjalmarson4, D. Kendall6, E. Kyr¨ol¨a7,S.Kwok8, A. Lecacheux5, G. Leppelmeier7, E. J. Llewellyn9, K. Mattila10,G.M´egie11, D. Murtagh12, M. Rougeron13, and G. Witt14 1 Swedish National Space Board, Box 4006, 171 04 Solna, Sweden Letter to the Editor 2 Swedish Space Corporation, PO Box 4207, 171 04 Solna, Sweden 3 National Technology Agency of Finland (TEKES), Kyllikkiporten 2, PB 69, 00101 Helsinki, Finland 4 Onsala Space Observatory, Chalmers University of Technology, 439 92, Onsala, Sweden 5 Observatoire de Paris, 61 Av. de l’Observatoire, 75014 Paris, France 6 Canadian Space Agency, PO Box 7275, Ottawa, Ontario K1L 8E3, Canada 7 Finnish Meteorological Institute, PO Box 503, 00101 Helsinki, Finland 8 Department of Physics and Astronomy, University of Calgary, Calgary, ABT 2N 1N4, Canada 9 Department of Physics and Engineering Physics, 116 Science Place, University of Saskatchewan, Saskatoon, SK S7N 5E2, Canada 10 Observatory, PO Box 14, University of Helsinki, 00014 Helsinki, Finland 11 Institut Pierre Simon Laplace, CNRS-Universit´e Paris 6, 4 place Jussieu, 75252 Paris Cedex 05, France 12 Global Environmental Measurements Group, Department of Radio and Space Science, Chalmers, 412 96 G¨oteborg, Sweden 13 Centre National d’Etudes´ Spatiales, Centre Spatial de Toulouse, 18 avenue Edouard´ Belin, 31401 Toulouse Cedex 4, France 14 Department of Meteorology, Stockholm University, 106 91 Stockholm, Sweden Received 6 December 2002 / Accepted 17 February 2003 Abstract. -
Science & ROGER PENROSE
Science & ROGER PENROSE Live Webinar - hosted by the Center for Consciousness Studies August 3 – 6, 2021 9:00 am – 12:30 pm (MST-Arizona) each day 4 Online Live Sessions DAY 1 Tuesday August 3, 2021 9:00 am to 12:30 pm MST-Arizona Overview / Black Holes SIR ROGER PENROSE (Nobel Laureate) Oxford University, UK Tuesday August 3, 2021 9:00 am – 10:30 am MST-Arizona Roger Penrose was born, August 8, 1931 in Colchester Essex UK. He earned a 1st class mathematics degree at University College London; a PhD at Cambridge UK, and became assistant lecturer, Bedford College London, Research Fellow St John’s College, Cambridge (now Honorary Fellow), a post-doc at King’s College London, NATO Fellow at Princeton, Syracuse, and Cornell Universities, USA. He also served a 1-year appointment at University of Texas, became a Reader then full Professor at Birkbeck College, London, and Rouse Ball Professor of Mathematics, Oxford University (during which he served several 1/2-year periods as Mathematics Professor at Rice University, Houston, Texas). He is now Emeritus Rouse Ball Professor, Fellow, Wadham College, Oxford (now Emeritus Fellow). He has received many awards and honorary degrees, including knighthood, Fellow of the Royal Society and of the US National Academy of Sciences, the De Morgan Medal of London Mathematical Society, the Copley Medal of the Royal Society, the Wolf Prize in mathematics (shared with Stephen Hawking), the Pomeranchuk Prize (Moscow), and one half of the 2020 Nobel Prize in Physics, the other half shared by Reinhard Genzel and Andrea Ghez. -
The Galactic Center: a Laboratory for Fundamental Astrophysics And
The Galactic Center: A Laboratory for Fundamental Astrophysics and Galactic Nuclei An Astro2010 Science White Paper Authors: Andrea Ghez (UCLA; [email protected]), Mark Morris (UCLA), Jessica Lu (Caltech), Nevin Weinberg (UCB), Keith Matthews (Caltech), Tal Alexander (Weizmann Inst.), Phil Armitage (U. of Colorado), Eric Becklin (Ames/UCLA), Warren Brown (CfA), Randy Campbell (Keck) Tuan Do (UCLA), Andrea Eckart (U. of Cologne), Reinhard Genzel (MPE/UCB), Andy Gould (Ohio State), Brad Hansen (UCLA), Luis Ho (Carnegie), Fred Lo (NRAO), Avi Loeb (Harvard), Fulvio Melia (U. of Arizona), David Merritt (RIT), Milos Milosavljevic (U. of Texas), Hagai Perets (Weizmann Inst.), Fred Rasio (Northwestern), Mark Reid (CfA), Samir Salim (NOAO), Rainer Sch¨odel (IAA), Sylvana Yelda (UCLA) Submitted to Science Frontier Panels on (1) The Galactic Neighborhood (GAN) arXiv:0903.0383v1 [astro-ph.GA] 2 Mar 2009 (2) Cosmology and Fundamental Physics (CFP) Supplemental Animations: http://www.astro.ucla.edu/∼ghezgroup/gc/pictures/Future GCorbits.shtml Galactic Center Stellar Dynamics Astro2010 White Paper 1 Abstract As the closest example of a galactic nucleus, the Galactic center presents an exquisite lab- oratory for learning about supermassive black holes (SMBH) and their environs. In this document, we describe how detailed studies of stellar dynamics deep in the potential well of a galaxy offer several exciting directions in the coming decade. First, it will be possible to obtain precision measurements of the Galaxy’s central potential, providing both a unique test of General Relativity (GR) and a detection of the extended dark matter distribution that is predicted to exist around the SMBH. Tests of gravity have not previously been pos- sible on scales larger than our solar system, or in regimes where the gravitational energy of a body is >∼1% of its rest mass energy. -
Messenger-No117.Pdf
ESO WELCOMES FINLANDINLAND AS ELEVENTH MEMBER STAATE CATHERINE CESARSKY, ESO DIRECTOR GENERAL n early July, Finland joined ESO as Education and Science, and exchanged which started in June 2002, and were con- the eleventh member state, following preliminary information. I was then invit- ducted satisfactorily through 2003, mak- II the completion of the formal acces- ed to Helsinki and, with Massimo ing possible a visit to Garching on 9 sion procedure. Before this event, howev- Tarenghi, we presented ESO and its scien- February 2004 by the Finnish Minister of er, Finland and ESO had been in contact tific and technological programmes and Education and Science, Ms. Tuula for a long time. Under an agreement with had a meeting with Finnish authorities, Haatainen, to sign the membership agree- Sweden, Finnish astronomers had for setting up the process towards formal ment together with myself. quite a while enjoyed access to the SEST membership. In March 2000, an interna- Before that, in early November 2003, at La Silla. Finland had also been a very tional evaluation panel, established by the ESO participated in the Helsinki Space active participant in ESO’s educational Academy of Finland, recommended Exhibition at the Kaapelitehdas Cultural activities since they began in 1993. It Finland to join ESO “anticipating further Centre with approx. 24,000 visitors. became clear, that science and technology, increase in the world-standing of ESO warmly welcomes the new mem- as well as education, were priority areas Astronomy in Finland”. In February 2002, ber country and its scientific community for the Finnish government. we were invited to hold an information that is renowned for its expertise in many Meanwhile, the optical astronomers in seminar on ESO in Helsinki as a prelude frontline areas. -
Long-Term Monitoring of Jupiter's Stratospheric H2O Abundance with the Odin Space Telescope
EPSC Abstracts Vol. 13, EPSC-DPS2019-484-2, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Long-term monitoring of Jupiter's stratospheric H2O abundance with the Odin Space Telescope T. Cavalié1,2, B. Benmahi1, N. Biver2, M. Dobrijevic1, K. Bermudez-Diaz3, E. Lellouch2, P. Hartogh4, Aa. Sandqvist5, A. Lecacheux2, Å. Hjalmarson6, U. Frisk7, M. Olberg8, and The Odin Team. (1) LAB – CNRS – Univ. Bordeaux, Pessac, France ([email protected]), (2) LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cité, France (3) Université Paris Diderot, France, (4) Max Planck Institute for Solar System Research, Göttingen, Germany, (5) Stockholm Observatory, Sweden, (6) Onsala Space Observatory, Sweden, (7) Omnisys Instruments, Gothenburg, Sweden, (8) Chalmers University, Gothenburg, Sweden. Abstract References Water vapor and CO2 have been detected in the Burgdorf et al. 2006. Icarus 184, 634–637. stratospheres of the giant planets and Titan Cavalié et al. 2013. Astron. Astrophys. 553, A21. (Feuchtgruber et al. 1997, Coustenis et al. 1998, Coustenis et al. 1998. Astron. Astrophys. 336, L85– Burgdorf et al. 2006). The presence of the atmospheric L89. cold trap implies an external origin for H2O, and the Feuchtgruber et al. 1997. Nature 389, 159–162. possible sources are: interplanetary dust particles Lellouch et al. 1995. Nature 373, 592–595. (IDP), icy rings and/or satellites, and large comet Nordh et al. 2003. Astron. Astrophys. 402, L21-L25. impacts. In July 1994, the Shoemaker-Levy 9 comet (SL9) spectacularly impacted Jupiter near 44°S. On the long term, Jupiter was left with a variety of new species in its stratosphere, including CO, HCN, CS, etc (Lellouch et al. -
Works of Love
reader.ad section 9/21/05 12:38 PM Page 2 AMAZING LIGHT: Visions for Discovery AN INTERNATIONAL SYMPOSIUM IN HONOR OF THE 90TH BIRTHDAY YEAR OF CHARLES TOWNES October 6-8, 2005 — University of California, Berkeley Amazing Light Symposium and Gala Celebration c/o Metanexus Institute 3624 Market Street, Suite 301, Philadelphia, PA 19104 215.789.2200, [email protected] www.foundationalquestions.net/townes Saturday, October 8, 2005 We explore. What path to explore is important, as well as what we notice along the path. And there are always unturned stones along even well-trod paths. Discovery awaits those who spot and take the trouble to turn the stones. -- Charles H. Townes Table of Contents Table of Contents.............................................................................................................. 3 Welcome Letter................................................................................................................. 5 Conference Supporters and Organizers ............................................................................ 7 Sponsors.......................................................................................................................... 13 Program Agenda ............................................................................................................. 29 Amazing Light Young Scholars Competition................................................................. 37 Amazing Light Laser Challenge Website Competition.................................................. 41 Foundational -
Reversed out (White) Reversed
Berkeley rev.( white) Berkeley rev.( FALL 2014 reversed out (white) reversed IN THIS ISSUE Berkeley’s Space Sciences Laboratory Tabletop Physics Bringing More Women into Physics ALUMNI NEWS AND MORE! Cover: The MAVEN satellite mission uses instrumentation developed at UC Berkeley's Space Sciences Laboratory to explore the physics behind the loss of the Martian atmosphere. It’s a continuation of Berkeley astrophysicist Robert Lin’s pioneering work in solar physics. See p 7. photo credit: Lockheed Martin Physics at Berkeley 2014 Published annually by the Department of Physics Steven Boggs: Chair Anil More: Director of Administration Maria Hjelm: Director of Development, College of Letters and Science Devi Mathieu: Editor, Principal Writer Meg Coughlin: Design Additional assistance provided by Sarah Wittmer, Sylvie Mehner and Susan Houghton Department of Physics 366 LeConte Hall #7300 University of California, Berkeley Berkeley, CA 94720-7300 Copyright 2014 by The Regents of the University of California FEATURES 4 12 18 Berkeley’s Space Tabletop Physics Bringing More Women Sciences Laboratory BERKELEY THEORISTS INVENT into Physics NEW WAYS TO SEARCH FOR GOING ON SIX DECADES UC BERKELEY HOSTS THE 2014 NEW PHYSICS OF EDUCATION AND SPACE WEST COAST CONFERENCE EXPLORATION Berkeley theoretical physicists Ashvin FOR UNDERGRADUATE WOMEN Vishwanath and Surjeet Rajendran IN PHYSICS Since the Space Lab’s inception are developing new, small-scale in 1959, Berkeley physicists have Women physics students from low-energy approaches to questions played important roles in many California, Oregon, Washington, usually associated with large-scale of the nation’s space-based scientific Alaska, and Hawaii gathered on high-energy particle experiments. -
The Two-Colour EMCCD Instrument for the Danish 1.54 M Telescope and SONG?
A&A 574, A54 (2015) Astronomy DOI: 10.1051/0004-6361/201425260 & c ESO 2015 Astrophysics The two-colour EMCCD instrument for the Danish 1.54 m telescope and SONG? J. Skottfelt1;2, D. M. Bramich3, M. Hundertmark1, U. G. Jørgensen1;2, N. Michaelsen1, P. Kjærgaard1, J. Southworth4, A. N. Sørensen1, M. F. Andersen5, M. I. Andersen1, J. Christensen-Dalsgaard5, S. Frandsen5, F. Grundahl5, K. B. W. Harpsøe1;2, H. Kjeldsen5, and P. L. Pallé6;7 1 Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 København Ø, Denmark e-mail: [email protected] 2 Centre for Star and Planet Formation, Natural History Museum, University of Copenhagen, Østervoldgade 5–7, 1350 København K, Denmark 3 Qatar Environment and Energy Research Institute, Qatar Foundation, PO Box 5825, Doha, Qatar 4 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK 5 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark 6 Instituto de Astrofísica de Canarias (IAC), 38200 La Laguna, Tenerife, Spain 7 Dept. Astrofísica, Universidad de La Laguna (ULL), 38206 Tenerife, Spain Received 1 November 2014 / Accepted 27 November 2014 ABSTRACT We report on the implemented design of a two-colour instrument based on electron-multiplying CCD (EMCCD) detectors. This instrument is currently installed at the Danish 1.54 m telescope at ESO’s La Silla Observatory in Chile, and will be available at the SONG (Stellar Observations Network Group) 1m telescope node at Tenerife and at other SONG nodes as well. We present the software system for controlling the two-colour instrument and calibrating the high frame-rate imaging data delivered by the EMCCD cameras. -
Herschel Space Observatory-An ESA Facility for Far-Infrared And
Astronomy & Astrophysics manuscript no. 14759glp c ESO 2018 October 22, 2018 Letter to the Editor Herschel Space Observatory? An ESA facility for far-infrared and submillimetre astronomy G.L. Pilbratt1;??, J.R. Riedinger2;???, T. Passvogel3, G. Crone3, D. Doyle3, U. Gageur3, A.M. Heras1, C. Jewell3, L. Metcalfe4, S. Ott2, and M. Schmidt5 1 ESA Research and Scientific Support Department, ESTEC/SRE-SA, Keplerlaan 1, NL-2201 AZ Noordwijk, The Netherlands e-mail: [email protected] 2 ESA Science Operations Department, ESTEC/SRE-OA, Keplerlaan 1, NL-2201 AZ Noordwijk, The Netherlands 3 ESA Scientific Projects Department, ESTEC/SRE-P, Keplerlaan 1, NL-2201 AZ Noordwijk, The Netherlands 4 ESA Science Operations Department, ESAC/SRE-OA, P.O. Box 78, E-28691 Villanueva de la Canada,˜ Madrid, Spain 5 ESA Mission Operations Department, ESOC/OPS-OAH, Robert-Bosch-Strasse 5, D-64293 Darmstadt, Germany Received 9 April 2010; accepted 10 May 2010 ABSTRACT Herschel was launched on 14 May 2009, and is now an operational ESA space observatory offering unprecedented observational capabilities in the far-infrared and submillimetre spectral range 55−671 µm. Herschel carries a 3.5 metre diameter passively cooled Cassegrain telescope, which is the largest of its kind and utilises a novel silicon carbide technology. The science payload comprises three instruments: two direct detection cameras/medium resolution spectrometers, PACS and SPIRE, and a very high-resolution heterodyne spectrometer, HIFI, whose focal plane units are housed inside a superfluid helium cryostat. Herschel is an observatory facility operated in partnership among ESA, the instrument consortia, and NASA. The mission lifetime is determined by the cryostat hold time. -
On the Hunt for Excited States
INTERNATIONAL JOURNAL OF HIGH-ENERGY PHYSICS CERN COURIER VOLUME 45 NUMBER 10 DECEMBER 2005 On the hunt for excited states HOMESTAKE DARK MATTER SNOWMASS Future assured for Galactic gamma rays US workshop gets underground lab p5 may hold the key p 17 ready for the ILC p24 www.vectorfields.comi Music to your ears 2D & 3D electromagnetic modellinj If you're aiming for design excellence, demanding models. As a result millions you'll be pleased to hear that OPERA, of elements can be solved in minutes, the industry standard for electromagnetic leaving you to focus on creating modelling, gives you the most powerful outstanding designs. Electron trajectories through a TEM tools for engineering and scientific focussing stack analysis. Fast, accurate model analysis • Actuators and sensors - including Designed for parameterisation and position and NDT customisation, OPERA is incredibly easy • Magnets - ppm accuracy using TOSCA to use and has an extensive toolset, making • Electron devices - space charge analysis it ideal for a wide range of applications. including emission models What's more, its high performance analysis • RF Cavities - eigen modes and single modules work at exceptional levels of speed, frequency response accuracy and stability, even with the most • Motors - dynamic analysis including motion Don't take our word for it - order your free trial and check out OPERA yourself. B-field in a PMDC motor Vector Fields Ltd Culham Science Centre, Abingdon, Oxon, 0X14 3ED, U.K. Tel: +44 (0)1865 370151 Fax: +44 (0)1865 370277 Email: [email protected] Vector Fields Inc 1700 North Famsworth Avenue, Aurora, IL, 60505.