Uncovering the Birthplaces of Planets with The

Total Page:16

File Type:pdf, Size:1020Kb

Uncovering the Birthplaces of Planets with The CONTACT ISSUE O6 DECEMBER 2020 FINAL SPRINT BEFORE SKA OBSERVATORY LAUNCH LET’S TALK ABOUT... THE ORIGINS OF LIFE DELIVERING A ‘SOFTWARE TELESCOPE’ CONTENTS 06 09 SKA Global HQ corridors were sadly empty for much of this year due to the pandemic COVID-19 workplace procedures, 12 25 28 risk assessments and controls recently got the stamp of approval from the British Safety Council (BSC). FOREWORD INSIGHT Dear Friends and Colleagues, 03 Prof. Philip Diamond, SKA Director-General 18 Delivering a ‘software telescope’ 21 Trouble in the skies? – An interview on 2020 – what a year! If you cast your mind back, • December 2019 – March 2020: successful satellite mega-constellations IN BRIEF the big news at the beginning of the year was SKA1 critical design review; the Australian bushfires; we all felt for family, • March 2020: successful operations review; friends and colleagues in Australia and didn’t 04 Remembering Nichi D’Amico PATHFINDERS • April 2020: successful, external, cost audit; think things could get much worse. Well, it looks 04 Uncovering the birthplaces of planets with the SKA 24 LOFAR contributes to new solar eruption warning system different now! In January the WHO announced • June 2020: South Africa ratifies; 05 Teams ready for SKA Science Data Challenge 2 that a deadly coronavirus had been detected, I • July 2020: successful business-enabling 24 CHIME detection may resolve mysterious origin of FRBs don’t think any of us (except the epidemiologists review; 05 Towards SKA Regional Centres - the Portuguese case 25 First direct detection of a brown and pandemic experts) understood what that • September 2020: Australia ratifies the 06 CSIRO’s iconic Parkes radio telescope dwarf with a radio telescope meant – we do now. We’re living with the global Convention; given Indigenous name impact of COVID-19 and will be for some time to 26 ASKAP creates ‘Google Map’ of the Universe • September 2020: the SKA Board of Directors come, although it is wonderful to see the rapid 07 Monitoring wildfires in Portugal with endorses the SKA1 Construction Proposal 27 Upgraded GMRT gives new insights development and roll out of vaccines; let us hope SKA-related technology (CP) and the Observatory Establishment and into galaxy evolution 2021 sees a return to a normal world. 07 UK fellowship awarded to expand LOFAR research Delivery Plan (OEDP); The world of politics in 2020 has been fascinating TEAM SKA • December 2020: Italy, Portugal and the UK and worrying, with a hugely visible presidential ratify the Convention; FOCUS ON election in the USA – and significant threats to 28 Prof.Tao An – Head of SKA group at • December 2020: the Council Preparatory democracy, although it is good to see the checks Shanghai Astronomical Observatory Task Force completes its 19th and final 08 Final sprint before SKA Observatory launch and balances working. For those of us in the UK, meeting and passes its final report and 09 The SKA Observatory: our future and our European neighbours, Brexit has been a numerous policies to the SKAO Council for EVENTS show that has been painful to watch. The world approval. woke up, yet again, to the need to fight endemic LET’S TALK ABOUT 32 Workshop: Heritage, History and Indigenous Astronomy racism with the explosion of the Black Lives Achieving all of these milestones is testament to the highly professional team at SKA Organisation 10 The origins of life 32 Workshop: Tackling research accessibility Matter movement; and saw sexism and misogyny tackled but not yet beaten on various fronts. and across our partner institutes; it is an 33 Announcing the 2021 SKA science conference enormous body of work and I congratulate all On a more parochial and much more positive FEATURED IMAGE staff and colleagues, all of whom contributed to NEWS & JOBS note, after an extremely good year for the SKA, this achievement. 12 Goodbye to Arecibo we end it the best possible way with a Note 2021 will see an equally auspicious year for the 34 News Roundup / Partner Publications Verbale from the Foreign, Commonwealth and Development Office informing us that the SKA SKA, with the birth of the SKAO in January, to HQ CORNER 35 SKA Jobs Observatory Convention will officially enter into be celebrated at its first Council meeting. This force on 15 January 2021, marking the start of a will be followed soon thereafter by the formal 14 2 minutes with… Dr Sheila Kanani – Outreach & new era in the SKA history. transition from the SKA Organisation to SKAO Diversity Officer, Royal Astronomical Society (RAS) and then, hopefully, Council approval to begin Previous editions of Contact, and our various SKA construction. I also hope to see more 14 Keeping team spirit alive in the time of COVID-19 news items and press releases have covered countries join the Observatory as Members. 15 Marking Black History Month the various milestones this year, but it is worth gathering them all in one place, because it is an I wish good health and good cheer to all of you, 15 Nigeria’s first radio astronomer impressive story: the SKA family, as we end 2020, with a bright 16 SKAO procurement preparations ramping up • August 2019: The Netherlands ratifies the light in front of us for 2021. 17 Two years of agile software development at SKA SKA Observatory Convention; Prof. Philip Diamond, SKA Director-General 2 CONTACT | DECEMBER 2020 3 IN BRIEF IN MEMORY OF TEAMS READY FOR SKA NICOLÒ D’AMICO SCIENCE DATA CHALLENGE 2 (1953 – 2020) BY SKAO Registration is complete for the SKA BY ANDREA POSSENTI (INAF) his key role Science Data Challenge 2, with around in the Parkes 30 teams taking part from more than 60 institutions all over the world. The completely unexpected and sudden death of Prof. Nicolò Multibeam surveys (1998- D’Amico (Palermo 1953 – Soleminis 2020), President of the The challenge will see teams analyse a 2004), which Italian National Institute for Astrophysics (INAF), has been an 1 terabyte (TB) simulated SKA HI data doubled the number irreparable loss for the Italian astrophysics community and cube, using their own software tools to of catalogued pulsars beyond, and left a huge void in all the many people who, like identify and determine the properties and led to the discovery me, had the privilege to work with him. During the years of his of galaxies across a distance of four of the still unique double pulsar Presidency, Prof. D’Amico fully exploited his natural aptitude billion light years. to synthesise all the received suggestions into a precise vision PSR J0737−3039. That made him one of the recipients of for the development of astrophysics: to maximise the quality the prestigious “Descartes Prize” for outstanding European An international network of high- scientific collaborations in 2005, among other prizes. Prof. of the research, and to make that a flywheel of growth, while performance computing centres are “The external SRC network will be Feedback from participants and the D’Amico meanwhile obtained a full professorship at the paying special attention to education, outreach activities and a crucial element to the challenge, how the SKA Observatory interacts computing centres will be used to University of Cagliari and became director of the local science communication. He was the voting member for Italy providing access, processing and with our user community, so beginning further inform work on the SRC model. Astronomical Observatory and, later, director of the project in the SKA Board of Directors, and thanks to his remarkable storage for the data. This is similar to put this idea into practice via the SKAO is also encouraging best practice for the construction of the Sardinia Radio Telescope. In managerial capabilities, coupled with an always crystal-clear to how the SKA Observatory will Data Challenge is an important step by working with the UK-based Software autumn 2015, he was nominated President of INAF, and he and sound approach to the world of the institutions, he was disseminate the telescopes’ data in demonstrating how this will work Sustainability Institute to give awards to was confirmed for a second term in December 2019, the first the main actor in securing the long-term Italian funding for the via SKA Regional Centres (SRCs) in effectively as a system,” says SKA teams that demonstrate reproducibility president to be reconfirmed in the history of this prestigious project and in promoting SKA. the future. Science Director Dr Robert Braun. “It (using methods that can be replicated Italian institution. has also strengthened links between by others to achieve the same results). Graduating in Physics in 1977, only four years later Prof. Eight facilities are involved, including these facilities. We’ve had their Reproducibility lies at the heart of the D’Amico, known as “Nichi”, was already “permanent” at two prototype SRCs: IRIS UK (part representatives together in a virtual SKA’s Open Science approach to its the University of Palermo. After beginning with gamma-ray Above: Prof. Nichi D’amico during the second SKA IGO of the UK Science and Technology room discussing provision and access, future operations. Making software astronomy, a visit to CSIRO in Australia re-oriented his studies Negotiations meeting in January 2016 at the Accademia dei Facilities Council), SKA France, which is something we have never had processing techniques open in this way towards radio pulsars, the apex of which was reached with Lincei in Rome. Shanghai proto-SRC, Australia before now.” means they can also be built on for proto-SRC, Italy’s National Institute other, different purposes in the future. for Astrophysics - Information and Through December teams will each be Communications Technologies (ICT), given access to one of the computing UNCOVERING THE Institute for Astrophysics of Andalucía facilities, ready for the challenge to Above: Map of high-performance (IAA) in Spain, ENGAGE-SKA in formally kick off on 15 January.
Recommended publications
  • Digital Back End Development and Interference Mitigation Methods for Radio Telescopes with Phased-Array Feeds
    Brigham Young University BYU ScholarsArchive Theses and Dissertations 2014-08-20 Digital Back End Development and Interference Mitigation Methods for Radio Telescopes with Phased-Array Feeds Richard Allen Black Brigham Young University - Provo Follow this and additional works at: https://scholarsarchive.byu.edu/etd Part of the Electrical and Computer Engineering Commons BYU ScholarsArchive Citation Black, Richard Allen, "Digital Back End Development and Interference Mitigation Methods for Radio Telescopes with Phased-Array Feeds" (2014). Theses and Dissertations. 4233. https://scholarsarchive.byu.edu/etd/4233 This Thesis is brought to you for free and open access by BYU ScholarsArchive. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of BYU ScholarsArchive. For more information, please contact [email protected], [email protected]. Digital Back End Development and Interference Mitigation Methods for Radio Telescopes with Phased-Array Feeds Richard Black A thesis submitted to the faculty of Brigham Young University in partial fulfillment of the requirements for the degree of Master of Science Brian D. Jeffs, Chair Karl F. Warnick Neal K. Bangerter Department of Electrical and Computer Engineering Brigham Young University August 2014 Copyright c 2014 Richard Black All Rights Reserved ABSTRACT Digital Back End Development and Interference Mitigation Methods for Radio Telescopes with Phased-Array Feeds Richard Black Department of Electrical and Computer Engineering, BYU Master of Science The Brigham Young University (BYU) Radio Astronomy group, in collaboration with Cornell University, the University of Massachusetts, and the National Radio Astron- omy Observatory (NRAO), have in recent years developed and deployed PAF systems that demonstrated the advantages of PAFs for astronomy.
    [Show full text]
  • ATNF News Issue No
    Galaxy Pair NGC 1512 / NGC 1510 ATNF News Issue No. 67, October 2009 ISSN 1323-6326 Questacon "astronaut" street performer and visitors at the Parkes Open Days 2009. Credit: Shaun Amy, CSIRO. Cover page image Cover Figure: Multi-wavelength color-composite image of the galaxy pair NGC 1512/1510 obtained using the Digitised Sky Survey R-band image (red), the Australia Telescope Compact Array HI distribution (green) and the Galaxy Evolution Explorer NUV -band image (blue). The Spitzer 24µm image was overlaid just in the center of the two galaxies. We note that in the outer disk the UV emission traces the regions of highest HI column density. See article (page 28) for more information. 2 ATNF News, Issue 67, October 2009 Contents From the Director ...................................................................................................................................................................................................4 CSIRO Medal Winners .........................................................................................................................................................................................5 CSIRO Astronomy and Space Science Unit Formed ........................................................................................................................6 ATNF Distinguished Visitors Program ........................................................................................................................................................6 ATNF Graduate Student Program ................................................................................................................................................................7
    [Show full text]
  • CASKAR: a CASPER Concept for the SKA Phase 1 Signal Processing Sub-System
    CASKAR: A CASPER concept for the SKA phase 1 Signal Processing Sub-system Francois Kapp, SKA SA Outline • Background • Technical – Architecture – Power • Cost • Schedule • Challenges/Risks • Conclusions Background CASPER Technology MeerKAT Who is CASPER? • Berkeley Wireless Research Center • Nancay Observatory • UC Berkeley Radio Astronomy Lab • Oxford University Astrophysics • UC Berkeley Space Sciences Lab • Metsähovi Radio Observatory, Helsinki University of • Karoo Array Telescope / SKA - SA Technology • NRAO - Green Bank • New Jersey Institute of Technology • NRAO - Socorro • West Virginia University Department of Physics • Allen Telescope Array • University of Iowa Department of Astronomy and • MIT Haystack Observatory Physics • Harvard-Smithsonian Center for Astrophysics • Ohio State University Electroscience Lab • Caltech • Hong Kong University Department of Electrical and Electronic Engineering • Cornell University • Hartebeesthoek Radio Astronomy Observatory • NAIC - Arecibo Observatory • INAF - Istituto di Radioastronomia, Northern Cross • UC Berkeley - Leuschner Observatory Radiotelescope • Giant Metrewave Radio Telescope • University of Manchester, Jodrell Bank Centre for • Institute of Astronomy and Astrophysics, Academia Sinica Astrophysics • National Astronomical Observatories, Chinese Academy of • Submillimeter Array Sciences • NRAO - Tucson / University of Arizona Department of • CSIRO - Australia Telescope National Facility Astronomy • Parkes Observatory • Center for Astrophysics and Supercomputing, Swinburne University
    [Show full text]
  • The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST),
    A&A 468, 353–377 (2007) Astronomy DOI: 10.1051/0004-6361:20065724 & c ESO 2007 Astrophysics The XMM-Newton extended survey of the Taurus molecular cloud Special feature The XMM-Newton extended survey of the Taurus molecular cloud (XEST), M. Güdel1, K. R. Briggs1, K. Arzner1, M. Audard2,, J. Bouvier3, E. D. Feigelson4, E. Franciosini5, A. Glauser1, N. Grosso3, G. Micela5, J.-L. Monin3, T. Montmerle3, D. L. Padgett6, F. Palla7, I. Pillitteri8, L. Rebull6, L. Scelsi8, B. Silva9,10, S. L. Skinner11, B. Stelzer5, and A. Telleschi1 1 Paul Scherrer Institut, Würenlingen and Villigen, 5232 Villigen PSI, Switzerland e-mail: [email protected] 2 Columbia Astrophysics Laboratory, Mail Code 5247, 550 West 120th Street, New York, NY 10027, USA 3 Laboratoire d’Astrophysique de Grenoble, Université Joseph Fourier - CNRS, BP 53, 38041 Grenoble Cedex, France 4 Department of Astronomy & Astrophysics, Penn State University, 525 Davey Lab, University Park, PA 16802, USA 5 INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy 6 Spitzer Science Center, California Institute of Technology, Mail Code 220-6, Pasadena, CA 91125, USA 7 INAF - Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi, 5, 50125 Firenze, Italy 8 Dipartimento di Scienze Fisiche ed Astronomiche, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy 9 Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150 Porto, Portugal 10 Departamento de Matemática Aplicada, Faculdade de Ciêcias da Universidade do Porto, 4169 Porto, Portugal 11 CASA, 389, University of Colorado, Boulder, CO 80309-0389, USA Received 31 May 2006 / Accepted 5 August 2006 ABSTRACT Context.
    [Show full text]
  • Program Plan
    PROGRAM PLAN 1999 NATIONAL RADIO ASTRONOMY OBSERVATORY Cover: A "movie" of the radio emission from the exploding star Supernova 1993J in the galaxy M81. This time-sequence of images was made at a wavelength of 3.6 cm (8.3 Ghz) with a global array of telescopes that included the VLBA and the VIA. The resolution, or clarity of image detail, is 4000 AU (about 20 light-days), hundreds of times finer than can be achieved by optical telescopes on such a distant object. Observers: M. Rupen, N. Bartel, M. Bietenholz, T. Beasley. NATIONAL RADIO ASTRONOMY OBSERVATORY CALENDAR YEAR 1999 PROGRAM PLAN RSI rrao NOVEMBER 1,1998 The National Radio Astronomy Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc. TABLE OF CONTENTS I. INTRODUCTION 1 II. 1999 SCIENTIFIC PROGRAM 2 1. The Very Large Array . 2 .2. The Very Long Baseline Array 8 3. The 12 Meter Telescope 11 4. The 140 Foot Telescope 13 HI. USER FAdLITIES 15 1. The Very Large Array 15 2. The Very Long Baseline Array 18 3. The 12 Meter Telescope 21 4. The 140 Foot Telescope 26 IV. TECHNOLOGY DEVELOPMENT 29 1. Electronics Development Equipment 29 2. Computing 34 V. GREEN BANK TELESCOPE 42 VI. MAJOR INITIATIVES 51 1. The Millimeter Array 51 2. VLA Upgrade 57 3. AIPS++Project 65 VII. NON-NSF RESEARCH 67 1. United States Naval Observatory 67 2. Green Bank Interferometer 67 3. NASA - Green Bank Orbiting VLBI Earth Station 67 VIII. EDUCATION PROGRAM 68 IX. 1999 PRELIMINARY FINANCIAL PLAN 75 APPENDIX A - NRAO SCIENTIFIC STAFF ACTIVITIES 78 1.
    [Show full text]
  • Binocular Double Star Logbook
    Astronomical League Binocular Double Star Club Logbook 1 Table of Contents Alpha Cassiopeiae 3 14 Canis Minoris Sh 251 (Oph) Psi 1 Piscium* F Hydrae Psi 1 & 2 Draconis* 37 Ceti Iota Cancri* 10 Σ2273 (Dra) Phi Cassiopeiae 27 Hydrae 40 & 41 Draconis* 93 (Rho) & 94 Piscium Tau 1 Hydrae 67 Ophiuchi 17 Chi Ceti 35 & 36 (Zeta) Leonis 39 Draconis 56 Andromedae 4 42 Leonis Minoris Epsilon 1 & 2 Lyrae* (U) 14 Arietis Σ1474 (Hya) Zeta 1 & 2 Lyrae* 59 Andromedae Alpha Ursae Majoris 11 Beta Lyrae* 15 Trianguli Delta Leonis Delta 1 & 2 Lyrae 33 Arietis 83 Leonis Theta Serpentis* 18 19 Tauri Tau Leonis 15 Aquilae 21 & 22 Tauri 5 93 Leonis OΣΣ178 (Aql) Eta Tauri 65 Ursae Majoris 28 Aquilae Phi Tauri 67 Ursae Majoris 12 6 (Alpha) & 8 Vul 62 Tauri 12 Comae Berenices Beta Cygni* Kappa 1 & 2 Tauri 17 Comae Berenices Epsilon Sagittae 19 Theta 1 & 2 Tauri 5 (Kappa) & 6 Draconis 54 Sagittarii 57 Persei 6 32 Camelopardalis* 16 Cygni 88 Tauri Σ1740 (Vir) 57 Aquilae Sigma 1 & 2 Tauri 79 (Zeta) & 80 Ursae Maj* 13 15 Sagittae Tau Tauri 70 Virginis Theta Sagittae 62 Eridani Iota Bootis* O1 (30 & 31) Cyg* 20 Beta Camelopardalis Σ1850 (Boo) 29 Cygni 11 & 12 Camelopardalis 7 Alpha Librae* Alpha 1 & 2 Capricorni* Delta Orionis* Delta Bootis* Beta 1 & 2 Capricorni* 42 & 45 Orionis Mu 1 & 2 Bootis* 14 75 Draconis Theta 2 Orionis* Omega 1 & 2 Scorpii Rho Capricorni Gamma Leporis* Kappa Herculis Omicron Capricorni 21 35 Camelopardalis ?? Nu Scorpii S 752 (Delphinus) 5 Lyncis 8 Nu 1 & 2 Coronae Borealis 48 Cygni Nu Geminorum Rho Ophiuchi 61 Cygni* 20 Geminorum 16 & 17 Draconis* 15 5 (Gamma) & 6 Equulei Zeta Geminorum 36 & 37 Herculis 79 Cygni h 3945 (CMa) Mu 1 & 2 Scorpii Mu Cygni 22 19 Lyncis* Zeta 1 & 2 Scorpii Epsilon Pegasi* Eta Canis Majoris 9 Σ133 (Her) Pi 1 & 2 Pegasi Δ 47 (CMa) 36 Ophiuchi* 33 Pegasi 64 & 65 Geminorum Nu 1 & 2 Draconis* 16 35 Pegasi Knt 4 (Pup) 53 Ophiuchi Delta Cephei* (U) The 28 stars with asterisks are also required for the regular AL Double Star Club.
    [Show full text]
  • Publications of the Astronomical Society of Australia Volume 18, 2001 © Astronomical Society of Australia 2001
    Publishing Publications of the Astronomical Society of Australia Volume 18, 2001 © Astronomical Society of Australia 2001 An international journal of astronomy and astrophysics For editorial enquiries and manuscripts, please contact: The Editor, PASA, ATNF, CSIRO, PO Box 76, Epping, NSW 1710, Australia Telephone: +61 2 9372 4590 Fax: +61 2 9372 4310 Email: [email protected] For general enquiries and subscriptions, please contact: CSIRO Publishing PO Box 1139 (150 Oxford St) Collingwood, Vic. 3066, Australia Telephone: +61 3 9662 7666 Fax: +61 3 9662 7555 Email: [email protected] Published by CSIRO Publishing for the Astronomical Society of Australia www.publish.csiro.au/journals/pasa Publ. Astron. Soc. Aust., 2001, 18, 287–310 On Eagle’s Wings: The Parkes Observatory’s Support of the Apollo 11 Mission John M. Sarkissian CSIRO ATNF Parkes Observatory, PO Box 276, Parkes NSW, 2870, Australia [email protected] Received 2001 February 1, accepted 2001 July 1 Abstract: At 12:56 p.m., on Monday 21 July 1969 (AEST), six hundred million people witnessed Neil Armstrong’s historic first steps on the Moon through television pictures transmitted to Earth from the lunar module, Eagle. Three tracking stations were receiving the signals simultaneously. They were the CSIRO’s Parkes Radio Telescope, the Honeysuckle Creek tracking station near Canberra, and NASA’s Goldstone station in California. During the first nine minutes of the broadcast, NASA alternated between the signals being received by the three stations. When they switched to the Parkes pictures, they were of such superior quality that NASA remained with them for the rest of the 2½-hour moonwalk.
    [Show full text]
  • Symposium on Telescope Science
    Proceedings for the 26th Annual Conference of the Society for Astronomical Sciences Symposium on Telescope Science Editors: Brian D. Warner Jerry Foote David A. Kenyon Dale Mais May 22-24, 2007 Northwoods Resort, Big Bear Lake, CA Reprints of Papers Distribution of reprints of papers by any author of a given paper, either before or after the publication of the proceedings is allowed under the following guidelines. 1. The copyright remains with the author(s). 2. Under no circumstances may anyone other than the author(s) of a paper distribute a reprint without the express written permission of all author(s) of the paper. 3. Limited excerpts may be used in a review of the reprint as long as the inclusion of the excerpts is NOT used to make or imply an endorsement by the Society for Astronomical Sciences of any product or service. Notice The preceding “Reprint of Papers” supersedes the one that appeared in the original print version Disclaimer The acceptance of a paper for the SAS proceedings can not be used to imply or infer an endorsement by the Society for Astronomical Sciences of any product, service, or method mentioned in the paper. Published by the Society for Astronomical Sciences, Inc. First printed: May 2007 ISBN: 0-9714693-6-9 Table of Contents Table of Contents PREFACE 7 CONFERENCE SPONSORS 9 Submitted Papers THE OLIN EGGEN PROJECT ARNE HENDEN 13 AMATEUR AND PROFESSIONAL ASTRONOMER COLLABORATION EXOPLANET RESEARCH PROGRAMS AND TECHNIQUES RON BISSINGER 17 EXOPLANET OBSERVING TIPS BRUCE L. GARY 23 STUDY OF CEPHEID VARIABLES AS A JOINT SPECTROSCOPY PROJECT THOMAS C.
    [Show full text]
  • U.S. Naval Observatory Washington, DC 20392-5420 This Report Covers the Period July 2001 Through June Dynamical Astronomy in Order to Meet Future Needs
    1 U.S. Naval Observatory Washington, DC 20392-5420 This report covers the period July 2001 through June dynamical astronomy in order to meet future needs. J. 2002. Bangert continued to serve as Department head. I. PERSONNEL A. Civilian Personnel A. Almanacs and Other Publications Marie R. Lukac retired from the Astronomical Appli- cations Department. The Nautical Almanac Office ͑NAO͒, a division of the Scott G. Crane, Lisa Nelson Moreau, Steven E. Peil, and Astronomical Applications Department ͑AA͒, is responsible Alan L. Smith joined the Time Service ͑TS͒ Department. for the printed publications of the Department. S. Howard is Phyllis Cook and Phu Mai departed. Chief of the NAO. The NAO collaborates with Her Majes- Brian Luzum and head James R. Ray left the Earth Ori- ty’s Nautical Almanac Office ͑HMNAO͒ of the United King- entation ͑EO͒ Department. dom to produce The Astronomical Almanac, The Astronomi- Ralph A. Gaume became head of the Astrometry Depart- cal Almanac Online, The Nautical Almanac, The Air ment ͑AD͒ in June 2002. Added to the staff were Trudy Almanac, and Astronomical Phenomena. The two almanac Tillman, Stephanie Potter, and Charles Crawford. In the In- offices meet twice yearly to discuss and agree upon policy, strument Shop, Tie Siemers, formerly a contractor, was hired science, and technical changes to the almanacs, especially to fulltime. Ellis R. Holdenried retired. Also departing were The Astronomical Almanac. Charles Crawford and Brian Pohl. Each almanac edition contains data for 1 year. These pub- William Ketzeback and John Horne left the Flagstaff Sta- lications are now on a well-established production schedule.
    [Show full text]
  • Observations of Radio Magnetars with the Deep Space Network
    Hindawi Advances in Astronomy Volume 2019, Article ID 6325183, 12 pages https://doi.org/10.1155/2019/6325183 Research Article Observations of Radio Magnetars with the Deep Space Network Aaron B. Pearlman ,1 Walid A. Majid,1,2 and Thomas A. Prince1,2 1 Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA Correspondence should be addressed to Aaron B. Pearlman; [email protected] Received 5 October 2018; Revised 11 December 2018; Accepted 27 January 2019; Published 2 June 2019 Guest Editor: Ersin G¨o˘g¨us¸ Copyright © 2019 Aaron B. Pearlman et al. Tis is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Te Deep Space Network (DSN) is a worldwide array of radio telescopes which supports NASA’sinterplanetary spacecraf missions. When the DSN antennas are not communicating with spacecraf, they provide a valuable resource for performing observations of radio magnetars, searches for new pulsars at the Galactic Center, and additional pulsar-related studies. We describe the DSN’s capabilities for carrying out these types of observations. We also present results from observations of three radio magnetars, PSR J1745–2900, PSR J1622–4950, and XTE J1810–197, and the transitional magnetar candidate, PSR J1119–6127, using the DSN radio telescopes near Canberra, Australia. 1. Introduction Figure 2). A detailed list of properties associated with known magnetars can be found in the McGill Magnetar Catalog (see Magnetars are young neutron stars with very strong magnetic ∼ 13 15 http://www.physics.mcgill.ca/ pulsar/magnetar/main.html) felds (�≈10–10 G).
    [Show full text]
  • Astronomical Coordinate Systems
    Appendix 1 Astronomical Coordinate Systems A basic requirement for studying the heavens is being able to determine where in the sky things are located. To specify sky positions, astronomers have developed several coordinate systems. Each sys- tem uses a coordinate grid projected on the celestial sphere, which is similar to the geographic coor- dinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth’s equator). Each coordinate system is named for its choice of fundamental plane. The Equatorial Coordinate System The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the most closely related to the geographic coordinate system because they use the same funda- mental plane and poles. The projection of the Earth’s equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles onto the celestial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate sys- tems: the geographic system is fixed to the Earth and rotates as the Earth does. The Equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but it’s really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec. for short). It measures the angle of an object above or below the celestial equator.
    [Show full text]
  • The Great Attractor-A Cosmic String? *
    Aust. J. Phys., 1990, 43, 167-77 The Great Attractor-A Cosmic String? * D. S. Mathewson Mount Stromlo and Siding Spring Observatories, Australian National University, Private Bag, Woden, A.C.T. 2606, Australia. Abstract A brief review is made of the observational work on large-scale streaming motions in the Local Universe. There is considerable controversy as to whether the Great Attractor model of these streaming motions is correct. Preliminary results are presented of a southern sky survey of spiral galaxies to measure their peculiar velocities using the Tully-Fisher relationship. The region of strong peculiar motions has an elongated shape some 80° in angular extent centred roughly on the Great Attractor enclosing the brightest parts of the supergalactic plane. The peculiar velocities reverse in sign at a distance of 4000 km S-i which is conclusive evidence that such a dominant attracting region exists at that distance. However, there is little evidence of galaxies associated with this attracting mass and most galaxies appear to be participating in the streaming motions. The conclusion is that the attractor is largely invisible. It is proposed that a large moving loop of cosmic string is responsible for the peculiar velocities of the galaxies. 1. Introduction The story of the Great Attractor starts in 1976 when Vera Rubin and her colleagues found anisotropy of the Hubble flow on surprisingly large scales from observations of spiral galaxies (Rubin et al. 1976). Shortly after, the cosmic microwave background dipole was discovered (Smoot and Lubin 1979) 0 and interpreted as motion of our Local Group of 600 km S-1 towards 1= 269 , b = 28° (R.A.
    [Show full text]