DOCSLIB.ORG

J Anglo- Australian Telescope 1982/83

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
J Anglo- Australian Telescope 1982/83 J Anglo- Australian Telescope 1982/83 Report of the Anglo-Australian Telescope Board 1 July 1982 to 30 June 1983 Australian Government Publishing Service Canberra 1983 Correspondence to the Board may be addressed to: The Secretary Anglo-Australian Telescope Board Correspondence to the Observatory may be addressed to: The Director Anglo-Australian Observatory P.O. Box 296 Epping,N.S.W.2121 Australia Telephone: (02) 868 1666 Telex: AA23999 (AAOSYD) Frcwt Cover: The Cartwkwl Galaxy. This very unusual galaxy is surrounded by a ring rotating at 250 km/s and expanding at 90 km/s. It is thought to have been formed by a collision with one of the neighbouring small galaxies. Photo by W. D. Pence. © Anglo-Australian Telescope Board 1983 ISSN 0 728-6554 Printed by C. J. THOMPSON, Commonwealth Government Printer, Canberra J The Right Honourable Sir Keith Joseph, M.P. Secretary of State for Education and Science, Government of the United Kingdom of Great Britain and Northern Ireland. The Honourable Barry O. Jones, M.P. Minister for Science and Technology, Government of the Commonwealth of Australia. In accordance with Article 8 of the Agreement between the Australian Government and the Government of the United Kingdom to provide for the establishment and oper- ation of an optical telescope at Siding Spring Mountain in the State of New South Wales, I present herewith a report by the Anglo-Australian Telescope Board for the year from 1 July 1982 to 30 June 1983. The report summarises the operations of the Board for the period under review and includes financial statements and statements of estimated expenditure in accordance with the provisions of the Agreement. Chairman Anglo-Australian Telescope Board November 1983 ANGLO-AUSTRALIAN TELESCOPE BOARD Board Membership for the period 1 July 1982 to 30 June 1983 For the United Kingdom: Sir Harrie Massey, F.R.S. (Chairman) Professor Emeritus, University College London Dr H.H.Atkinson Director, Astronomy, Space and Radio and Nuclear Physics, Science and Engineering Research Council Professor M. S. Longair, F.R.S.E. (from 1 July 1982) Director, Royal Observatory, Edinburgh For Australia: Professor J. H. Carver (Deputy Chairman) Director, Research School of Physical Sciences, Australian National University DrR.H.Frater.F.T.S. Chief, CSIRO Division of Radiophysics Dr W. J. McG. Tegart, F.T.S. Secretary, Department of Science and Technology Director, Anglo-Australian Observatory: Dr D. C. Morton Executive Officer, Anglo-Australian Observatory: MrD.W.Cunliffe Secretary to the Board: Mr J.M. Franklin Secretary designate to the Board 1983-84: Miss K. M. Proust ANGLO-AUSTRALIAN TELESCOPE BOARD ORGANISATION UNITED KINGDOM GOVERNMENT AUSTRALIAN GOVERNMENT Science and Engineering Department of Science Research Council and Technology THE BOARD 3 Members 3 Members appointed by the appointed by United Kingdom Australia AATB Secretariat (Canberra) ANGLO-AUSTRALIAN OBSERVATORY AAO Laboratory Telescope (Epping, NSW) (Siding Spring Director Mountain, NSW) Astronomers Research-Support Administrative Groups Staff Electronic Optical/Mechanical Photographic Programming Telescope Operations RESPONSIBILITIES OF THE BOARD The Anglo-Australian Telescope Board operates under an Agreement between the Governments of the United Kingdom and Australia. The Board is an independent bi-national authority which consists of members appointed from each country and draws its funds in equal shares from each Government. In accordance with its responsibilities under the Agreement, the Board operates and maintains facilities which enable United Kingdom and Australian astronomers to undertake astronomical observations for the advancement of scientific knowledge. The Board's facilities consist of the Anglo-Australian Telescope (AAT) at Siding Spring Mountain, near Coonabarabran, N.S.W., and the associated Laboratory at Epping, N.S.W. Collectively, these fa- cilities are known as the Anglo-Australian Observatory (AAO). A brief history of the AAT proj- ect appears in Appendix D, page 42. NATIONAL AGENCIES DESIGNATED UNDER THE AGREEMENT Under the terms of Article 1 (2) of the Anglo-Australian Telescope Agreement, each Govern- ment acts through an agency designated for that purpose. The designated agencies are the Science and Engineering Research Council of the United Kingdom and the Australian Department of Science and Technology. The agencies are jointly responsible for implementing the Agreement. Contents 1. INTRODUCTION TheYcarPast 1 Scientific Highlights 2 Co-operation with Other Institutions 2 Changes in Board Membership 3 Meetings of the Board 3 Symposia and Publications 3 Advisory Committee on Instrumentation 3 Freedom of Information Act 4 2. OPERATIONS OF THE OBSERVATORY Observatory Staff 5 Building and Accommodation Programme 5 Allocation of Observing Time 5 Visiting Scientists 6 Photography 6 Public Relations 6 3. RESEARCH Overview 7 Gas Motions in Barred Galaxies 9 A Collapsing Supercluster 10 An Infrared Nucleus in Ml04 11 Asymmetric Supernova Explosion 11 Infrared Views of Jupiter 12 NGC 4696—A Centre of Activity 14 Do Supernovae Liberate Dust? 14 4. INSTRUMENTATION Introduction 16 Available Equipment 16 Computing Facilities 17 Development of Instrumentation 19 Image Photon Counting System (IPCS) 19 Spcctropolarimetcr 19 Hatfield Infrared-Optical Polarimeter 19 Faint Object Red Spectrograph (FORS) 19 Optical Fibres 20 5. FINANCIAL STATEMENTS A. Audited Accounts 1982-83 21 Report of the Auditor-General 21 Statement of Fixed Assets 21 Statement of Receipts and Payments 22 B. Disposal of Assets in 1982-83 23 C. Expenditure Forecast 1983-84 to 1987-88 23 Vll APPENDIXES A. Research Papers 25 Published Scientific Papers based on AAT data (1 July 1982 to 30 June 1983) 25 Papers delivered at AAO Research Symposia 30 B. Telescope Allocation 33 PATT Allocations 33 ATAC Allocations 34 Summary of Observing Programmes 35 C. Staff of the Anglo-Australian Observatory 41 D. History of the AAT Project 42 via 1 Introduction The Year Past In this eighth year of full scientific operation the Anglo-Australian Telescope continues to hold its place as one of the foremost scientific instruments of its kind world-wide. The introduction of new devices for making astronomical observations, particularly long-baseline radio telescopes and satellites designed to detect radiation which cannot be satisfactorily observed at ground level, increases the demand for complementary ob- servations at optical wavelengths using the most far-seeing and accurate telescopes. The list of scientists of many nationalities who, against considerable competition, have won observing time on the AAT and the ever-growing list of scientific achievements based on these observations are the proper testimony to the value of the Telescope. The excellence of the original design and engineering of the Telescope and its lo- cation in the Southern Hemisphere laid firm foundations on which to build a repu- tation. It has been through two other elements—the technical developments which have maximised the quality of the observational data obtained from the Telescope and the high standard of service to visiting observers—that the Observatory has become a major international focus for observational astronomy. The Board acknowledges with great appreciation that this reputation is due to the efforts of the observers, the Direc- tor of the Observatory and his staff, and the members of associated institutions in the United Kingdom and Australia who contribute to the development of instrumentation for the Telescope. The Board has again given close attention during the year to the efficient manage- ment of the funds provided by the two contributing Governments. The economy measures which have been imposed generally on public authorities in both countries have not yet made a noticeable impact on the Board's operations. Some protection from cuts in funding may have been derived from the agreed programme of instrumentation and building development established by the 1979 report on future funding of the AAT, referred to in the last two annual reports. The end of this five-year programme is now approaching, and the Board is examining the essential and desirable needs of observers with respect to new detector and spectroscopic instrumentation and augmented com- puting resources. It is to be hoped that the level of funding for the Board will remain ad- equate to maintain the Observatory's standard of facilities and services. On 1 April 1983, the Board concluded an occupancy agreement with CSIRO for the continued use and enjoyment of the Epping site for as long as the Anglo-Australian Telescope Agreement remains in force. Early in the 1983-84 year, the Board's Secretariat will be re-located from Canberra to Sydney, where it will be accommodated at the Anglo-Australian Observatory's Lab- oratory at Epping. The Board's Secretary will continue to have responsibility for vari- ous functions, relating particularly to the Board's bi-national and statutory status, independently of the Director of the Observatory. The Board's new secretary will be Miss Katrina Proust, B.A., LL.B. The Sec- retariat's new address, the same as that for the Observatory, is shown on p.ii. These changes will take effect from 4 July 1983. Since 197S, an officer of the Australian designated agency, which is currently the Department of Science and Technology, has been made available to serve full-time as 1 the Board's Secretary, on a cost recovery basis. This arrangement, coinciding with the first operational years of the Observatory, has been very beneficial to the Board, as a major task in this period has been to establish and implement administrative procedures suitable to Australian governmental practices within the framework of which the Board largely operates. The employment of suitable personnel and the provision of access to the Department's resources for the Secretariat have also assisted the Board. The Board is very appreciative of this support from the Australian Government. It recognizes that the current limitations on departmental resources necessitates ter- mination of the arrangement. Scientific Highlights Some of the scientific highlights from research programmes conducted during the year are described briefly below.
Load more

Recommended publications
  • Exploration of the Moon
    Exploration of the Moon The physical exploration of the Moon began when Luna 2, a space probe launched by the Soviet Union, made an impact on the surface of the Moon on September 14, 1959. Prior to that the only available means of exploration had been observation from Earth. The invention of the optical telescope brought about the first leap in the quality of lunar observations. Galileo Galilei is generally credited as the first person to use a telescope for astronomical purposes; having made his own telescope in 1609, the mountains and craters on the lunar surface were among his first observations using it. NASA's Apollo program was the first, and to date only, mission to successfully land humans on the Moon, which it did six times. The first landing took place in 1969, when astronauts placed scientific instruments and returnedlunar samples to Earth. Apollo 12 Lunar Module Intrepid prepares to descend towards the surface of the Moon. NASA photo. Contents Early history Space race Recent exploration Plans Past and future lunar missions See also References External links Early history The ancient Greek philosopher Anaxagoras (d. 428 BC) reasoned that the Sun and Moon were both giant spherical rocks, and that the latter reflected the light of the former. His non-religious view of the heavens was one cause for his imprisonment and eventual exile.[1] In his little book On the Face in the Moon's Orb, Plutarch suggested that the Moon had deep recesses in which the light of the Sun did not reach and that the spots are nothing but the shadows of rivers or deep chasms.
    [Show full text]
  • AGN Jet Kinematics on Parsec-Scales: the MOJAVE Program
    galaxies Article AGN Jet Kinematics on Parsec-Scales: The MOJAVE Program Matthew Lister and the MOJAVE Collaboration Department of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USA; [email protected] Academic Editors: Jose L. Gómez, Alan P. Marscher and Svetlana G. Jorstad Received: 20 July 2016; Accepted: 2 September 2016; Published: 9 September 2016 Abstract: Very long baseline interferometry offers the best means of investigating the complex dynamics of relativistic jets powered by active galactic nuclei, via multi-epoch, sub-milliarcsecond, full-polarization imaging at radio wavelengths. Although targeted studies have yielded important information on the structures of individual AGN jets, the strong selection effects associated with relativistically beaming imply that general aspects of the flows can only be determined via large statistical studies. In this review I discuss major results from the Monitoring of Jets in Active Galactic Nuclei With VLBA Experiments (MOJAVE) program, which has gathered multi-epoch Very Long Baseline Array (VLBA) data at 15 GHz on over 400 AGN jets over the course of two decades. The sample is large enough to encompass a range of AGN optical class, radio luminosity and synchrotron peak frequency, and has been used to show that within a particular jet, individual bright features have a spread of apparent speed and velocity vector position angle about a characteristic value. We have found that in some cases there is a secular evolution of launch angle direction over time, indicative of evolving narrow energized channels within a wider outflow. The majority of the jet features are superluminal and accelerating, with changes in speed more common than changes in direction.
    [Show full text]
  • Eyes Skies Full En.Pdf
    1 00:00:05,240 --> 00:00:08,800 By taking our sense of sight far beyond the realm of our forebears' 2 00:00:08,880 --> 00:00:13,200 imagination, these wonderful instruments, the telescopes, open the way to 3 00:00:13,280 --> 00:00:17,240 a deeper and more perfect understanding of nature. - René Descartes, 1637 4 00:00:17,720 --> 00:00:22,520 For millennia mankind gazed out into the mesmerising night sky 5 00:00:22,600 --> 00:00:28,320 without recognising the stars of our own Milky Way Galaxy as other suns 6 00:00:28,400 --> 00:00:33,400 or the billions of sister galaxies making up the rest of our Universe 7 00:00:35,440 --> 00:00:38,760 or that we are merely punctuation in the Universe’s 8 00:00:38,840 --> 00:00:42,480 13.7 billion year-long story. 9 00:00:42,560 --> 00:00:46,080 With only our eyes as observing tools we had no means of 10 00:00:46,160 --> 00:00:50,120 finding solar systems around other stars, or of determining 11 00:00:50,200 --> 00:00:55,000 whether life exists elsewhere in the Universe. 12 00:00:58,080 --> 00:01:00,320 Today we are well on our way to unravelling many of the 13 00:01:00,400 --> 00:01:03,520 mysteries of the Universe, living in what may be the most remarkable 14 00:01:03,600 --> 00:01:05,920 age of astronomical discovery.
    [Show full text]
  • Australian Sky & Telescope
    TRANSIT MYSTERY Strange sights BINOCULAR TOUR Dive deep into SHOOT THE MOON Take amazing as Mercury crosses the Sun p28 Virgo’s endless pool of galaxies p56 lunar images with your smartphone p38 TEST REPORT Meade’s 25-cm LX600-ACF P62 THE ESSENTIAL MAGAZINE OF ASTRONOMY Lasers and advanced optics are transforming astronomy p20 HOW TO BUY THE RIGHT ASTRO CAMERA p32 p14 ISSUE 93 MAPPING THE BIG BANG’S COSMIC ECHOES $9.50 NZ$9.50 INC GST LPI-GLPI-G LUNAR,LUNAR, PLANETARYPLANETARY IMAGERIMAGER ANDAND GUIDERGUIDER ASTROPHOTOGRAPHY MADE EASY. Let the LPI-G unleash the inner astrophotographer in you. With our solar, lunar and planetary guide camera, experience the universe on a whole new level. 0Image Sensor:'+(* C O LOR 0 Pixel Size / &#*('+ 0Frames per second/Resolution• / • / 0 Image Format: #,+$)!&))'!,# .# 0 Shutter%,*('#(%%#'!"-,,* 0Interface: 0Driver: ASCOM compatible 0GuiderPort: 0Color or Monochrome Models (&#'!-,-&' FEATURED DEALERS: MeadeTelescopes Adelaide Optical Centre | www.adelaideoptical.com.au MeadeInstrument The Binocular and Telescope Shop | www.bintel.com.au MeadeInstruments www.meade.com Sirius Optics | www.sirius-optics.com.au The device to free you from your handbox. With the Stella adapter, you can wirelessly control your GoTo Meade telescope at a distance without being limited by cord length. Paired with our new planetarium app, *StellaAccess, astronomers now have a graphical interface for navigating the night sky. STELLA WI-FI ADAPTER / $#)'$!!+#!+ #$#)'#)$##)$#'&*' / (!-')-$*')!($%)$$+' "!!$#$)(,#%',).( StellaAccess app. Available for use on both phones and tablets. /'$+((()$!'%!#)'*")($'!$)##!'##"$'$*) stars, planets, celestial bodies and more /$,'-),',### -' ($),' /,,,$"$')*!!!()$$"%)!)!($%( STELLA is controlled with Meade’s planetarium app, StellaAccess. Available for purchase for both iOS S and Android systems.
    [Show full text]
  • 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.
    [Show full text]
  • Vireo Manual.Pdf
    VIREO: The Virtual Educational Observatory 1 VIREO: THE VIRTUAL EDUCATIONAL OBSERVATORY Software Reference Guide A Manual to Accompany Software Document SM 20: Circ.Version 1.0 Department of Physics Gettysburg College Gettysburg, PA 17325 Telephone: (717) 337-6028 email: [email protected] Software, and Manuals prepared by: Contemporary Laboratory Glenn Snyder and Laurence Marschall (CLEA PROJECT, Gettysburg College) Experiences in Astronomy VIREO: The Virtual Educational Observatory 2 Contents Introduction To Vireo: The Virtual Educational Observatory .................................................................................. 3 Starting Vireo ................................................................................................................................................................ 4 The Virtual Observatory Control Screen ..................................................................................................................... 4 Using an Optical Telescope ........................................................................................................................................... 5 Using the Photometer .................................................................................................................................................... 8 Using the Spectrometer ............................................................................................................................................... 11 Using the Multi-Channel Spectrometer .....................................................................................................................
    [Show full text]
  • RAPID Tev GAMMA-RAY FLARING of BL LACERTAE
    The Astrophysical Journal, 762:92 (13pp), 2013 January 10 doi:10.1088/0004-637X/762/2/92 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. RAPID TeV GAMMA-RAY FLARING OF BL LACERTAE T. Arlen1, T. Aune2, M. Beilicke3, W. Benbow4, A. Bouvier2, J. H. Buckley3, V. Bugaev3, A. Cesarini5,L.Ciupik6, M. P. Connolly5, W. Cui7, R. Dickherber3,J.Dumm8, M. Errando9, A. Falcone10, S. Federici11,12, Q. Feng7,J.P.Finley7, G. Finnegan13, L. Fortson8, A. Furniss2, N. Galante4, D. Gall14,S.Griffin15,J.Grube6,G.Gyuk6,D.Hanna15, J. Holder16, T. B. Humensky17, P. Kaaret14, N. Karlsson8, M. Kertzman18, Y. Khassen19, D. Kieda13, H. Krawczynski3, F. Krennrich20, G. Maier11, P. Moriarty21, R. Mukherjee9, T. Nelson8, A. O’Faolain´ de Bhroithe´ 19,R.A.Ong1, M. Orr20, N. Park22, J. S. Perkins23,24,A.Pichel25, M. Pohl11,12, H. Prokoph11, J. Quinn19, K. Ragan15, L. C. Reyes26, P. T. Reynolds27, E. Roache4, D. B. Saxon16, M. Schroedter4, G. H. Sembroski7, D. Staszak15, I. Telezhinsky11,12, G. Tesiˇ c´15, M. Theiling7, K. Tsurusaki14, A. Varlotta7,S.Vincent11, S. P. Wakely22, T. C. Weekes4, A. Weinstein20, R. Welsing11, D. A. Williams2, and B. Zitzer28 (The VERITAS Collaboration), and S. G. Jorstad29,30, N. R. MacDonald29, A. P. Marscher29,P.S.Smith31, R. C. Walker32, T. Hovatta33, J. Richards7, W. Max-Moerbeck33, A. Readhead33,M.L.Lister7, Y. Y. Kovalev34,35, A. B. Pushkarev36,37,M.A.Gurwell38, A. Lahteenm¨ aki¨ 39, E. Nieppola39, M. Tornikoski39, and E. Jarvel¨ a¨ 39 1 Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA 2 Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA 3 Department of Physics, Washington University, St.
    [Show full text]
  • Astronomy Alphabet
    Astronomy Alphabet Educational video for children Teacher https://vimeo.com/77309599 & Learner Guide This guide gives background information about the astronomy topics mentioned in the video, provides questions and answers children may be curious about, and suggests topics for discussion. Alhazen A Alhazen, called the Father of Optics, performed NASA/Goddard/Lunar Reconnaissance Orbiter, Apollo 17 experiments over a thousand years ago Can you find Alhazen crater when you look at the Moon? to learn about how light travels and Why does the Moon look bigger near the behaves. He also studied astronomy, horizon? separated light into colors, and sought to Believe it or not, scientists still don’t know for sure why explain why the Moon looks bigger near we perceive the Moon to be larger when it lies near to the the horizon. horizon. Though photos of the Moon at different points in the sky show it to be the same size, we humans think we I’ve never heard of Abu Ali al-Hasan ibn al- see something quite different. Try this experiment yourself Hasan ibn al-Hatham (Alhazen). sometime! One possibility is that objects we see next to the Tell me more about him. Moon when it’s near to them give us the illusion that it’s We don’t know that much about Alhazen be- bigger, because of a sense of scale and reference. cause he lived so long ago, but we do know that he was born in Persia in 965. He wrote hundreds How many craters does the Moon have, and what of books on math and science and pioneered the are their names? scientific method of experimentation.
    [Show full text]
  • Star-Birth Myth 'Busted' (W/ Podcast) 25 August 2009
    Star-birth myth 'busted' (w/ Podcast) 25 August 2009 The different numbers of stars of different masses at birth is called the ‘initial mass function’ (IMF). Most of the light we see from galaxies comes from the highest mass stars, while the total mass in stars is dominated by the lower mass stars. By measuring the amount of light from a population of stars, and making some corrections for the stars’ ages, astronomers can use the IMF to False-colour images of two galaxies, NGC 1566 (left) estimate the total mass of that population of stars. and NGC 6902 (right), showing their different proportions of very massive stars. Regions with massive O stars Results for different galaxies can be compared only show up as white or pink, while less massive B stars if the IMF is the same everywhere, but Dr Meurer’s appear in blue. NGC 1566 is much richer in O stars than team has shown that this ratio of high-mass to low- is NGC 6902. The images combine observations of UV mass newborn stars differs between galaxies. emission by NASA's Galaxy Evolution Explorer spacecraft and H-alpha observations made with the For instance, small 'dwarf' galaxies form many Cerro Tololo Inter-American Observatory (CTIO) telescope in Chile. NGC 1566 is 68 million light years more low-mass stars than expected. away in the southern constellation of Dorado. NGC 6902 is about 33 million light years away in the constellation To arrive at this finding, Dr Meurer’s team used Sagittarius. Photo by: NASA/JPL-Caltech/JHU galaxies from the HIPASS Survey (HI Parkes All Sky Survey) done with CSIRO’s Parkes radio telescope.
    [Show full text]
  • Science Programs for a 2-M Class Telescope at Dome C, Antarctica: PILOT, the Pathfinder for an International Large Optical Telescope
    CSIRO PUBLISHING www.publish.csiro.au/journals/pasa Publications of the Astronomical Society of Australia, 2005, 22, 199–235 Science Programs for a 2-m Class Telescope at Dome C, Antarctica: PILOT, the Pathfinder for an International Large Optical Telescope M. G. BurtonA,M, J. S. LawrenceA, M. C. B. AshleyA, J. A. BaileyB,C, C. BlakeA, T. R. BeddingD, J. Bland-HawthornB, I. A. BondE, K. GlazebrookF, M. G. HidasA, G. LewisD, S. N. LongmoreA, S. T. MaddisonG, S. MattilaH, V. MinierI, S. D. RyderB, R. SharpB, C. H. SmithJ, J. W. V. StoreyA, C. G. TinneyB, P. TuthillD, A. J. WalshA, W. WalshA, M. WhitingA, T. WongA,K, D. WoodsA, and P. C. M. YockL A School of Physics, University of New South Wales, Sydney NSW 2052, Australia B Anglo Australian Observatory, Epping NSW 1710, Australia C Centre for Astrobiology, Macquarie University, Sydney NSW 2109, Australia D University of Sydney, Sydney NSW 2006, Australia E Massey University, Auckland, New Zealand F John Hopkins University, Baltimore, MD 21218, USA G Swinburne University, Melbourne VIC 3122, Australia H Stockholm Observatory, Stockholm, Sweden I CEA Centre d’Etudes de Saclay, Paris, France J Electro Optics Systems, Queanbeyan NSW 2620, Australia K CSIRO Australia Telescope National Facility, Epping NSW 1710, Australia L University of Auckland, Auckland, New Zealand M Corresponding author. E-mail: [email protected] Received 2004 November 12, accepted 2005 April 12 Abstract: The cold, dry, and stable air above the summits of the Antarctic plateau provides the best ground- based observing conditions from optical to sub-millimetre wavelengths to be found on the Earth.
    [Show full text]
  • The Swift Ultra-Violet/Optical Telescope
    The Swift Ultra-Violet/Optical Telescope Peter W. A. Roming*a, Thomas E. Kennedyb, Keith O. Masonb, John A. Nouseka, Lindy Ahrc, Richard E. Binghamd, Patrick S. Broosa, Mary J. Carterb, Barry K. Hancockb, Howard E. Huckleb, S. D. Hunsbergera, Hajime Kawakamib, Ronnie Killoughc, T. Scott Kocha, Michael K. McLellandc, Kelly Smithc, Philip J. Smithb, Juan Carlos Soto†e, Patricia T. Boydf, Alice A. Breeveldb, Stephen T. Hollandf, Mariya Ivanushkinaa, Michael S. Pryzbyg, Martin D. Stillf, Joseph Stockg aDepartment of Astronomy & Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA bMullard Space Sciences Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK cSouthwest Research Institute, 6220 Culebra Rd, San Antonio, TX 78228, USA dOptical Science Laboratory, University College London, Gower St, London WC1E 6BT, UK eStarsys Research Corporation, 4909 Nautilus Court N., Boulder, CO 80301, USA fNASA/Goddard Space Flight Center, Code 660.1, Greenbelt, MD 20771, USA gSwales Aerospace, 5050 Powder Mill Rd, Beltsville, MD 20705, USA ABSTRACT The UV/Optical Telescope (UVOT) is one of three instruments flying aboard the Swift Gamma-ray Observatory. It is designed to capture the early (~1 minute) UV and optical photons from the afterglow of gamma-ray bursts in the 170-600 nm band as well as long term observations of these afterglows. This is accomplished through the use of UV and optical broadband filters and grisms. The UVOT has a modified Ritchey-Chrétien design with micro-channel plate intensified charged-coupled device detectors that record the arrival time of individual photons and provide sub- arcsecond positioning of sources.
    [Show full text]
  • BL Lacertae Flaring Activity 2019-2020
    BL Lacertae flaring activity 2019-2020 Dijana Dominis Prester, University of Rijeka, Department of Physics & G. Bonnolli, E. Lindfords, D. Morcuende, J. Strišković, S. Ventura CMC Meeting, Zagreb, 22 September 2020 CMC Meeting, Zagreb, 22.9.2020 BL Lac Flaring Activity, D. Dominis Prester 1 Outline • BL Lacertae • MAGIC paper on BL Lac flare in 2015 • BL Lac flare in May 2019 • BL Lac flares from July 2019 up to Sept 2020 • Potential alternative modeling of MAGIC BL Lac data CMC Meeting, Zagreb, 22.9.2020 BL Lac Flaring Activity, D. Dominis Prester 2 BL Lacertae • RA: 22h 02m 43.3s , dec: +42° 16ʹ 40ʺ (2000) in Constellation Lacerta (lizard) • Redshift: z=0.069 • Discovered by C. Hoffmeister (1929) and misinterpreted as variable star • Strong radio emission detection (J. Schmitt, 1968), host galaxy identified • Detected in VHE by MAGIC I mono (Albert et al, Astrophys.J.666:L17- L20,2007) CMC Meeting, Zagreb, 22.9.2020 BL Lac Flaring Activity, D. Dominis Prester 3 BL Lacertae objects • Blazars of extreme nature • Named after “The Prototype” BL Lacertae • Typically in centers of luminous elliptical galaxies • Rapid and large-amplitude flux variability • Significant optical polarization • Spectra dominated by a relatively featureless non-thermal emission continuum over the entire electromagnetic range • No strong emission lines, contrary to quasars • Core dominated radio sources • Subclasses depending on the broadband spectral shape (HBL, IBL, LBL, XBL, RBL) CMC Meeting, Zagreb, 22.9.2020 BL Lac Flaring Activity, D. Dominis Prester 4 MAGIC paper on BL Lac flare in 2015 MAGIC Collaboration et al.: BL Lac in 2015 γ γ ] VHE -ray flare.
    [Show full text]