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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. -
THE 1000 BRIGHTEST HIPASS GALAXIES: H I PROPERTIES B
The Astronomical Journal, 128:16–46, 2004 July A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 1000 BRIGHTEST HIPASS GALAXIES: H i PROPERTIES B. S. Koribalski,1 L. Staveley-Smith,1 V. A. Kilborn,1, 2 S. D. Ryder,3 R. C. Kraan-Korteweg,4 E. V. Ryan-Weber,1, 5 R. D. Ekers,1 H. Jerjen,6 P. A. Henning,7 M. E. Putman,8 M. A. Zwaan,5, 9 W. J. G. de Blok,1,10 M. R. Calabretta,1 M. J. Disney,10 R. F. Minchin,10 R. Bhathal,11 P. J. Boyce,10 M. J. Drinkwater,12 K. C. Freeman,6 B. K. Gibson,2 A. J. Green,13 R. F. Haynes,1 S. Juraszek,13 M. J. Kesteven,1 P. M. Knezek,14 S. Mader,1 M. Marquarding,1 M. Meyer,5 J. R. Mould,15 T. Oosterloo,16 J. O’Brien,1,6 R. M. Price,7 E. M. Sadler,13 A. Schro¨der,17 I. M. Stewart,17 F. Stootman,11 M. Waugh,1, 5 B. E. Warren,1, 6 R. L. Webster,5 and A. E. Wright1 Received 2002 October 30; accepted 2004 April 7 ABSTRACT We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 H i brightest galaxies in the southern sky as obtained from the H i Parkes All-Sky Survey (HIPASS). The selection of the brightest sources is basedontheirHi peak flux density (Speak k116 mJy) as measured from the spatially integrated HIPASS spectrum. 7 ; 10 The derived H i masses range from 10 to 4 10 M . -
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 -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate 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 is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it 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 of course 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. The longitud inal angle is called the right ascension (RA for short). -
Structure, Properties and Formation Histories of S0 Galaxies
Structure, Properties and Formation Histories of S0 Galaxies by Kaustubh Vaghmare Thesis Supervisor Prof. Ajit K. Kembhavi A thesis presented for the degree of Doctor of Philosophy to IUCAA & Jawaharlal Nehru University India July, 2015 Structure, Properties and Formation Histories of S0 Galaxies by Kaustubh Vaghmare c 2015 All rights reserved. Certificate This is to certify that the thesis entitled Structure, Properties and Formation Histories of S0 Galaxies submitted by Mr. Kaustubh Vaghmare for the award of the degree of Doctor of Philosophy to Jawaharlal Nehru University, New Delhi is his original work. This has not been published or submitted to any other University for any other Degree or Diploma. Pune July 30th, 2015 Prof. Ajit K. Kembhavi (Thesis Advisor & Director, IUCAA) Declaration I hereby declare that the work reported in this thesis is entirely original. This thesis is composed independently by me at the Inter-University Centre for Astronomy and Astrophysics, Pune under the supervision of Prof. Ajit K. Kembhavi. I further declare that the subject matter presented in the thesis has not previously formed the basis for the award of any degree, diploma, associateship, fellowship or any other similar title of any University or Institution. Pune July 30th, 2015 Prof. Ajit K. Kembhavi Mr. Kaustubh Vaghmare (Thesis Advisor) (Ph.D. Candidate) 3 Dedicated to ... Prathama & Prakash (my parents, my Gods) Rahul (my brother, whose ever presence with my parents and unquestioning support allowed me to work in peace) & Sneha (my beloved) 5 Acknowledgements For all students and regular visitors, it is clear that Prof. Ajit Kembhavi is one of the busiest people with frequent meetings, visits abroad, directorial duties and several other responsibilities. -
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. -
Where Are Compton-Thick Radio Galaxies? a Hard X-Ray View of Three Candidates
MNRAS 000, 000–000 (0000) Preprint 11 September 2018 Compiled using MNRAS LATEX style file v3.0 Where are Compton-thick radio galaxies? A hard X-ray view of three candidates F. Ursini,1 ? L. Bassani,1 F. Panessa,2 A. Bazzano,2 A. J. Bird,3 A. Malizia,1 and P. Ubertini2 1 INAF-IASF Bologna, Via Gobetti 101, I-40129 Bologna, Italy. 2 INAF/Istituto di Astrofisica e Planetologia Spaziali, via Fosso del Cavaliere, 00133 Roma, Italy. 3 School of Physics and Astronomy, University of Southampton, SO17 1BJ, UK. Released Xxxx Xxxxx XX ABSTRACT We present a broad-band X-ray spectral analysis of the radio-loud active galactic nuclei NGC 612, 4C 73.08 and 3C 452, exploiting archival data from NuSTAR, XMM-Newton, Swift and INTEGRAL. These Compton-thick candidates are the most absorbed sources among the hard X-ray selected radio galaxies studied in Panessa et al.(2016). We find an X-ray absorbing column density in every case below 1:5 × 1024 cm−2, and no evidence for a strong reflection continuum or iron K α line. Therefore, none of these sources is properly Compton-thick. We review other Compton-thick radio galaxies reported in the literature, arguing that we currently lack strong evidences for heavily absorbed radio-loud AGNs. Key words: galaxies: active – galaxies: Seyfert – X-rays: galaxies – X-rays: individual: NGC 612, 4C 73.08, 3C 452 1 INTRODUCTION 2000). A number of local CT AGNs have been detected thanks to recent hard X-ray surveys with INTEGRAL (Sazonov et al. 2008; A significant fraction of active galactic nuclei (AGNs) are known Malizia et al. -
Dwarf Galaxies
Europeon South.rn Ob.ervotory• ESO ML.2B~/~1 ~~t.· MAIN LIBRAKY ESO Libraries ,::;,q'-:;' ..-",("• .:: 114 ML l •I ~ -." "." I_I The First ESO/ESA Workshop on the Need for Coordinated Space and Ground-based Observations - DWARF GALAXIES Geneva, 12-13 May 1980 Report Edited by M. Tarenghi and K. Kjar - iii - INTRODUCTION The Space Telescope as a joint undertaking between NASA and ESA will provide the European community of astronomers with the opportunity to be active partners in a venture that, properly planned and performed, will mean a great leap forward in the science of astronomy and cosmology in our understanding of the universe. The European share, however,.of at least 15% of the observing time with this instrumentation, if spread over all the European astrono mers, does not give a large amount of observing time to each individual scientist. Also, only well-planned co ordinated ground-based observations can guarantee success in interpreting the data and, indeed, in obtaining observ ing time on the Space Telescope. For these reasons, care ful planning and cooperation between different European groups in preparing Space Telescope observing proposals would be very essential. For these reasons, ESO and ESA have initiated a series of workshops on "The Need for Coordinated Space and Ground based Observations", each of which will be centred on a specific subject. The present workshop is the first in this series and the subject we have chosen is "Dwarf Galaxies". It was our belief that the dwarf galaxies would be objects eminently suited for exploration with the Space Telescope, and I think this is amply confirmed in these proceedings of the workshop. -
Secular Evolution and the Formation of Pseudobulges in Disk Galaxies
5 Aug 2004 22:35 AR AR222-AA42-15.tex AR222-AA42-15.sgm LaTeX2e(2002/01/18) P1: IKH 10.1146/annurev.astro.42.053102.134024 Annu. Rev. Astron. Astrophys. 2004. 42:603–83 doi: 10.1146/annurev.astro.42.053102.134024 Copyright c 2004 by Annual Reviews. All rights reserved First published! online as a Review in Advance on June 2, 2004 SECULAR EVOLUTION AND THE FORMATION OF PSEUDOBULGES IN DISK GALAXIES John Kormendy Department of Astronomy, University of Texas, Austin, Texas 78712; email: [email protected] Robert C. Kennicutt, Jr. Department of Astronomy, Steward Observatory, University of Arizona, Tucson, Arizona 85721; email: [email protected] KeyWords galaxy dynamics, galaxy structure, galaxy evolution I Abstract The Universe is in transition. At early times, galactic evolution was dominated by hierarchical clustering and merging, processes that are violent and rapid. In the far future, evolution will mostly be secular—the slow rearrangement of energy and mass that results from interactions involving collective phenomena such as bars, oval disks, spiral structure, and triaxial dark halos. Both processes are important now. This review discusses internal secular evolution, concentrating on one important con- sequence, the buildup of dense central components in disk galaxies that look like classical, merger-built bulges but that were made slowly out of disk gas. We call these pseudobulges. We begin with an “existence proof”—a review of how bars rearrange disk gas into outer rings, inner rings, and stuff dumped onto the center. The results of numerical sim- ulations correspond closely to the morphology of barred galaxies. -
Sample Program of Study
Sample Program of Study - Nurse Anesthetist Program 126 Credits* (Specialty coursework in BOLD) Year One – Preclinical Year Summer Cr Fall Cr Spring Cr NAN 543 Principles of Anesthesia I 3 NAN 718 Prof Aspects NA I 1 NAN 544 Principles of Anes II 2 NGC 501 Conceptual Foundations 3 NGC 527 Eval and Gen Evidence for HC II 3 NAN 544L Principles of Anes II Lab 1 NGC 518 Health Promotion 3 NGC 527L Eval and Gen Evidence II Lab 1 NAN 672 Pharm Anesth/Adj Drugs 3 NGC 520 Scientific Communications 2 NGC 634 Organizational Leadership 3 NAN 719 Prof Aspects NA II 1 NGC 625 Pathophysiology for APN I 3 NGC 575 Adv Helth Assessmnt (CRNA) 2 NGC 502 Informatics 3 NGC 612 Pharmacotherapeutics 4 NGC 509 Ethics* 3 NGC 626 Pathophysiology for APN II 3 NGC 526 Eval and Gen Evidence for HC I 4 Total Credits 14 Total Credits 17 Total Credits 17 Year Two – Clinical Year I Summer Fall Spring NAN 598 Intro to NA Clin Prac (1 d/wk) 2 NAN 545 Principles of Anes III 3 NAN 546 Principles of Anes IV 3 NAN 601 NA Clin Pract I (3 d/wk) 6 NAN 602 NA Clin Pract II (4 d/wk) 8 NAN 603 NA Clin Pract III (4 d/wk) 8 NGC 632 Interpreting HC Policy 3 NAN 711 Current Top Anes 1 NAN 712 Current Top Anes II 1 NGC 692 Grantsmanship 1 NGC 701 State of the Science 3 NAN 721 Anes Crisis Res Mgt I 1 NGC 638 Program Evaluation 3 Total Credits 12 Total Credits 15 Total Credits 16 Year Three – Clinical Year II Summer Fall Spring NAN 604 NA Clin Pract IV (4 d/wk) 6 NAN 605 NA Clin Pract V (4 d/wk) 6 NAN 547 Principles of Anes V 3 NGC 725 DNP Advanced Clinical Prac I 2 NAN 713 Current Top Anes III 1 NAN 606 NA Clin Pract VI (4 d/wk) 8 NGC 798 DNP Capstone Course I 1 NAN 722 Anes Crisis Res Mgt II 1 NAN 714 Current Top Anes IV 1 NGC 533 Teaching in Nursing 3 NGC 726 DNP Advanced Clinical Prac II 2 NGC 799 DNP Capstone Course II 1 Total Credits 9 Total Credits 14 Total Credits 12 *Effective for all students matriculating Spring 2015 and thereafter, N509 is not a required course and the total credits will be 123. -
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. -
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).