The European Vlbi Network: a Sensitive and State-Of- The-Art Instrument for High-Resolution Science
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Jodrell Bank Observatory
UK Tentative List of Potential Sites for World Heritage Nomination: Application form Please save the application to your computer, fill in and email to: [email protected] The application form should be completed using the boxes provided under each question, and, where possible, within the word limit indicated. Please read the Information Sheets before completing the application form. It is also essential to refer to the accompanying Guidance Note for help with each question, and to the relevant paragraphs of UNESCO’s Operational Guidelines for the Implementation of the World Heritage Convention, (OG) available at: http://whc.unesco.org/en/guidelines Applicants should provide only the information requested at this stage. Further information may be sought in due course. (1) Name of Proposed World Heritage Site Jodrell Bank Observatory (2) Geographical Location Name of country/region United Kingdom Grid reference to centre of site SJ 798708 Please enclose a map preferably A4-size, a plan of the site, and 6 photographs, preferably electronically. page 1 (3) Type of Site Please indicate category: Natural Cultural Mixed Cultural Landscape (4) Description Please provide a brief description of the proposed site, including the physical characteristics. 200 words The Jodrell Bank Observatory, which is part of the University of Manchester’s School of Physics and Astronomy, is dominated by the monumental Lovell Telescope, the first large fully steerable radio telescope in the world - which still operates as the 3rd largest on the planet. The telescope, which is a Grade 1 listed structure, is 76m in diameter and stands 89m high. Despite its age (53 years in 2010), it is now more powerful than ever and remains at the forefront of Astrophysics research, working 24 hours a day, 365 days a year to observe distant galaxies and objects such as Pulsars and Quasars, far out across the Universe. -
RF Interference Monitoring for the Onsala Space Observatory Master of Science Thesis (Communication Engineering)
RF Interference Monitoring for the Onsala Space Observatory Master of Science Thesis (Communication Engineering) SYED AMEER AHMED GILLANI Department of Earth and Space Sciences, Onsala Space Observatory, CHALMERS UNIVERSITY OF TECHNOLOGY, Göteborg, Sweden, 2010. RF INTERFERENCE MONITORING FOR ONSALA SPACE OBSERVATORY SYED AMEER AHMED GILLANI Department of Earth and Space Sciences, Onsala Space Observatory CHALMERS UNIVERSITY OF TECHNOLOGY Göteborg, Sweden 2010 ii ABSTRACT With the continuous and rapid developments in wireless services and allocation of radio frequency spectrum to these services, huge interferences have been observed in the field of radio astronomy. According to the international regulations, parts of the spectra are reserved for radio-astronomical observations. Man-made signals entering the receiver chain of a radio telescope have much higher power compared to natural or passive signals received at the radio telescopes. Passive signals received at radio telescopes are normally 60 dB below the receiver noise level. Active signals generated by man-made wireless services pollute the natural emissions by completely masking them due to high signal strength. The cosmic radiation is determined by the fundamental laws of physics, thus the frequencies are fixed and cannot be changed. So interferences created by active services lead to wrong interpretations of the astronomical data. The present thesis deals with RF interference monitoring system for the Onsala Space Observatory. As part of the thesis, a software application has been developed, which communicates with different type of digital receivers (spectrum analyzers) attached with antenna controlling hardware to control omnidirectional and steerable antennas. A steerable antenna is used to find the direction of interference source by moving the antenna in azimuth and elevation direction. -
Cutting-Edge Engineering for the World's Largest Radio Telescope
SKAO Cutting-edge engineering for the world’s largest radio telescope Cutting-edge engineering for the world’s largest radio telescope Approaching a technological challenge on the scale of the SKA is formidable... while building on 60 years of radio- astronomy developments, the huge increase in scale from existing facilities demands a revolutionary break from traditional radio telescope design and radical developments in processing, computer speeds and the supporting technological infrastructure. To answer this challenge the SKA has been broken down into various elements that will form the final SKA telescope. Each element is managed by an international consortium comprising world leading experts in their fields. The SKA Office, staffed with engineering domain experts, systems engineers, scientists and managers, centralises the project management and system design. SKAO The design work was awarded through the SKA Office to these Consortia, made up of over 100 of some of the world’s top research institutions and companies, drawn primarily from the SKA Member countries but also beyond. Following the delivery of a detailed design package in 2016, in 2018 nine consortia are having their Critical Design Reviews (CDR) to deliver the final design documentation to prepare a construction proposal for government approval. The other three consortia are part of the SKA’s Advanced Instrumentation Programme, which develops future instrumention for the SKA. The 2018 SKA CalenDaR aims to recognise the immense work conducted by these hundreds of dedicated engineers and project managers from around the world over the past five years. Without their crucial work, the SKA’s ambitious science programme would not be possible. -
Event Horizon Telescope Observations of the Jet Launching and Collimation in Centaurus A
https://doi.org/10.1038/s41550-021-01417-w Supplementary information Event Horizon Telescope observations of the jet launching and collimation in Centaurus A In the format provided by the authors and unedited Draft version May 26, 2021 Typeset using LATEX preprint style in AASTeX63 Event Horizon Telescope observations of the jet launching and collimation in Centaurus A: Supplementary Information Michael Janssen ,1, 2 Heino Falcke ,2 Matthias Kadler ,3 Eduardo Ros ,1 Maciek Wielgus ,4, 5 Kazunori Akiyama ,6, 7, 4 Mislav Balokovic´ ,8, 9 Lindy Blackburn ,4, 5 Katherine L. Bouman ,4, 5, 10 Andrew Chael ,11, 12 Chi-kwan Chan ,13, 14 Koushik Chatterjee ,15 Jordy Davelaar ,16, 17, 2 Philip G. Edwards ,18 Christian M. Fromm,4, 5, 19 Jose´ L. Gomez´ ,20 Ciriaco Goddi ,2, 21 Sara Issaoun ,2 Michael D. Johnson ,4, 5 Junhan Kim ,13, 10 Jun Yi Koay ,22 Thomas P. Krichbaum ,1 Jun Liu (刘Ê ) ,1 Elisabetta Liuzzo ,23 Sera Markoff ,15, 24 Alex Markowitz,25 Daniel P. Marrone ,13 Yosuke Mizuno ,26, 19 Cornelia Muller¨ ,1, 2 Chunchong Ni ,27, 28 Dominic W. Pesce ,4, 5 Venkatessh Ramakrishnan ,29 Freek Roelofs ,5, 2 Kazi L. J. Rygl ,23 Ilse van Bemmel ,30 Antxon Alberdi ,20 Walter Alef,1 Juan Carlos Algaba ,31 Richard Anantua ,4, 5, 17 Keiichi Asada,22 Rebecca Azulay ,32, 33, 1 Anne-Kathrin Baczko ,1 David Ball,13 John Barrett ,6 Bradford A. Benson ,34, 35 Dan Bintley,36 Raymond Blundell ,5 Wilfred Boland,37 Geoffrey C. Bower ,38 Hope Boyce ,39, 40 Michael Bremer,41 Christiaan D. -
EVN Biennial Report Pages Web
EVN Biennial Report 2015- 2016 Cover Page Credit: Image by Paul Boven ([email protected]). Sateltite Image: Blue marble Next Generation, courtesy of NASA Visible Earth 2 FOREWORD FROM THE EVN CONSORTIUM BOARD OF DIRECTORS CHAIRPERSON 3 THE EVN 6 THE EUROPEAN CONSORTIUM FOR VLBI 6 EVN PROGRAM COMMITTEE 8 EVN PC MEETINGS 9 PROPOSAL STATISTICS 9 REQUESTED SCIENCE RESEARCH AREAS AND OBSERVING BANDS 10 EVN SCHEDULER REPORT 13 TECHNICAL AND OPERATIONS GROUP REPORT 19 EVN OBSERVATORY REPORTS 22 ASTRON - WESTERBORK SYNTHESIS RADIO TELESCOPE 22 HARTEBEESTHOEK RADIO ASTRONOMY OBSERVATORY 24 INSTITUTE OF RADIO ASTRONOMY (INAF), ITALY 25 MEDICINA STATION 25 NOTO STATION 26 SARDINIA RADIO TELESCOPE 27 INSTITUTE OF APPLIED ASTRONOMY - QUASAR VLBI NETWORK 28 IAA CORRELATOR CENTER 29 JODRELL BANK OBSERVATORY 30 MAX-PLANCK-INSTITUT FUER RADIOASTRONOMIE, BONN 32 EFFELSBERG STATION REPORT 33 BONN CORRELATOR REPORT 35 OBSERVATORIO ASTRONOMICO NACIONAL, IGN - YEBES OBSERVATORY 38 ONSALA SPACE OBSERVATORY 42 SHANGHAI ASTRONOMICAL OBSERVATORY 45 THE TIANMA 65M RADIO TELESCOPE 45 THE SESHAN25 TELESCOPE 46 TORUN CENTRE FOR ASTRONOMY 48 ENGINEERING RESEARCH INSTITUTE ‘VENTSPILS INTERNATIONAL RADIO ASTRONOMY CENTRE’ OF VENTSPILS UNIVERSITY COLLEGE (VIRAC) 50 XINJIANG ASTRONOMICAL OBSERVATORY, NANSHAN STATION 53 ARECIBO - NATIONAL ASTRONOMY & IONOSPHERE CENTER, PUERTO RICO 55 GEODETIC OBSERVATORY WETTZELL, GERMANY 56 KOREA ASTRONOMY & SPACE SCIENCE INSTITUTE - KOREAN VLBI NETWORK 58 METSÄHOVI RADIO OBSERVATORY 60 JOINT INSTITUTE FOR VLBI ERIC REPORT 62 INSTITUTE NEWS -
Very Long Baseline Interferometry Imaging of the Advancing Ejecta in the first Gamma-Ray Nova V407 Cygni? M
A&A 638, A130 (2020) Astronomy https://doi.org/10.1051/0004-6361/202038142 & c ESO 2020 Astrophysics Very long baseline interferometry imaging of the advancing ejecta in the first gamma-ray nova V407 Cygni? M. Giroletti1, U. Munari2, E. Körding3, A. Mioduszewski4, J. Sokoloski5,6, C. C. Cheung7, S. Corbel8,9, F. Schinzel10;??, K. Sokolovsky11,12,13 , and T. J. O’Brien14 1 INAF Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy e-mail: [email protected] 2 INAF Astronomical Observatory of Padova, 36012 Asiago (VI), Italy 3 Department of Astrophysics/IMAPP, Radboud University Nijmegen, 6500 GL Nijmegen, The Netherlands 4 National Radio Astronomy Observatory, Array Operations Center, 1003 Lopezville Road, Socorro, NM 87801, USA 5 Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA 6 LSST Corproation, 933 North Cherry Avenue, Tucson, AZ 85721, USA 7 Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA 8 Laboratoire AIM (CEA/IRFU – CNRS/INSU – Université Paris Diderot), CEA DSM/IRFU/SAp, 91191 Gif-sur-Yvette, France 9 Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU, USR 704 – Univ. Orléans, OSUC, 18330 Nançay, France 10 National Radio Astronomy Observatory, PO Box O, Socorro, NM 87801, USA 11 Department of Physics and Astronomy, Michigan State University, 567 Wilson Rd, East Lansing, MI 48824, USA 12 Astro Space Center, Lebedev Physical Inst. RAS, Profsoyuznaya 84/32, 117997 Moscow, Russia 13 Sternberg Astronomical Institute, Moscow University, Universitetsky 13, 119991 Moscow, Russia 14 Jodrell Bank Centre for Astrophysics, Alan Turing Building, University of Manchester, Manchester M13 9PL, UK Received 10 April 2020 / Accepted 11 May 2020 ABSTRACT Context. -
High Resolution Radio Astronomy Using Very Long Baseline Interferometry
IOP PUBLISHING REPORTS ON PROGRESS IN PHYSICS Rep. Prog. Phys. 71 (2008) 066901 (32pp) doi:10.1088/0034-4885/71/6/066901 High resolution radio astronomy using very long baseline interferometry Enno Middelberg1 and Uwe Bach2 1 Astronomisches Institut, Universitat¨ Bochum, 44801 Bochum, Germany 2 Max-Planck-Institut fur¨ Radioastronomie, Auf dem Hugel¨ 69, 53121 Bonn, Germany E-mail: [email protected] and [email protected] Received 3 December 2007, in final form 11 March 2008 Published 2 May 2008 Online at stacks.iop.org/RoPP/71/066901 Abstract Very long baseline interferometry, or VLBI, is the observing technique yielding the highest-resolution images today. Whilst a traditionally large fraction of VLBI observations is concentrating on active galactic nuclei, the number of observations concerned with other astronomical objects such as stars and masers, and with astrometric applications, is significant. In the last decade, much progress has been made in all of these fields. We give a brief introduction to the technique of radio interferometry, focusing on the particularities of VLBI observations, and review recent results which would not have been possible without VLBI observations. This article was invited by Professor J Silk. Contents 1. Introduction 1 2.9. The future of VLBI: eVLBI, VLBI in space and 2. The theory of interferometry and aperture the SKA 10 synthesis 2 2.10. VLBI arrays around the world and their 2.1. Fundamentals 2 capabilities 10 2.2. Sources of error in VLBI observations 7 3. Astrophysical applications 11 2.3. The problem of phase calibration: 3.1. Active galactic nuclei and their jets 12 self-calibration 7 2.4. -
Table of Contents - 1 - - 2
Table of contents - 1 - - 2 - Table of Contents Foreword 5 1. The European Consortium for VLBI 7 2. Scientific highlights on EVN research 9 3. Network Operations 35 4. VLBI technical developments and EVN operations support at member institutes 47 5. Joint Institute for VLBI in Europe (JIVE) 83 6. EVN meetings 105 7. EVN publications in 2007-2008 109 - 3 - - 4 - Foreword by the Chairman of the Consortium The European VLBI Network (EVN) is the result of a collaboration among most major radio observatories in Europe, China, Puerto Rico and South Africa. The large radio telescopes hosted by these observatories are operated in a coordinated way to perform very high angular observations of cosmic radio sources. The data are then correlated by using the EVN correlator at the Joint Institute for VLBI in Europe (JIVE). The EVN, when operating as a single astronomical instrument, is the most sensitive VLBI array and constitutes one of the major scientific facilities in the world. The EVN also co-observes with the Very Long Baseline Array (VLBA) and other radio telescopes in the U.S., Australia, Japan, Russia, and with stations of the NASA Deep Space Network to form a truly global array. In the past, the EVN also operated jointly with the Japanese space antenna HALCA in the frame of the VLBI Space Observatory Programme (VSOP). The EVN plans now to co-observe with the Japanese space 10-m antenna ASTRO-G, to be launched by 2012, within the frame of the VSOP-2 project. With baselines in excess of 25.000 km, the space VLBI observations provide the highest angular resolution ever achieved in Astronomy. -
Jodrell Bank Discovery Centre Classroom Materials for Schools
Jodrell Bank Discovery Centre Classroom Materials for schools GCSE/BTEC: Inflatable Planetarium Links to resources The resources below are suggested activities your class could complete before or after this workshop. Please note these are recommended activities; it is not compulsory that students complete them. Some of the resources require access to ICT. The University of Manchester cannot be held responsible for the content of external sites. 1. Institute of Physics: Life Cycle of Stars https://www.youtube.com/watch?v=PM9CQDlQI0A Explains how we believe stars are born, live and die and the different ends to different sized stars. Features Professor Tim O’Brien; Associate Director of the Jodrell Bank Observatory. 2. Institute of Physics: How big is the Universe? https://www.youtube.com/watch?v=K_xZuopg4Sk Explains how astronomers have learnt to measure the distance to the stars. How many stars are in the observable universe and is it possible to comprehend the size of it all? 3. Institute of Physics: The Expanding Universe https://www.youtube.com/watch?v=jms_vklUeHA The expansion of the universe, the big bang and dark matter. Astronomers talk us through what we know and don't know about the universe. 4. Institute of Physics: Classroom demonstration: Colour and temperature of stars http://www.youtube.com/watch?v=oZve8FQhLOI Using a variable resistor and a light bulb, it is possible to demonstrate how the colour of a star is related to its temperature. 5. Institute of Physics: Classroom demonstration: H-R diagram https://www.youtube.com/watch?v=bL3tt-fJC1k How to illustrate the life cycle of stars using a Hertzsprung-Russell diagram, a large sheet, and some students. -
A Relativistic Helical Jet in the Gamma-Ray AGN 1156+
Astronomy & Astrophysics manuscriptno.ms3548-hong-final November20,2018 (DOI: will be inserted by hand later) A relativistic helical jet in the γ-ray AGN 1156+295 X. Y. Hong1,2, D. R. Jiang1,2, L. I. Gurvits3, M. A. Garrett3, S. T. Garrington4, R. T. Schilizzi5,6, R. D. Nan2, H. Hirabayashi7, W. H. Wang1,2, and G. D. Nicolson8 1 Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China 2 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China 3 Joint Institute for VLBI in Europe, Postbus 2, 7990 AA Dwingeloo, The Netherlands 4 Jodrell Bank Observatory, University of Manchester, Macclesfield, Cheshire SK11–9DL, UK 5 ASTRON, Postbus 2, 7990 AA Dwingeloo, The Netherlands 6 Leiden Observatory, PO Box 9513, 2300, RA Leiden, The Netherlands 7 Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan 8 Hartebeesthoek Radio Astronomy Observatory, Krugersdorp 1740, South Africa Received 31 January 2003/ accepted 19 November 2003 Abstract. We present the results of a number of high resolution radio observations of the AGN 1156+295. These include multi-epoch and multi-frequency VLBI, VSOP, MERLIN and VLA observations made over a period of ′′ ◦ 50 months. The 5 GHz MERLIN images trace a straight jet extending to ∼ 2 at P.A. ∼ −18 . Extended low brightness emission was detected in the MERLIN observation at 1.6 GHz and the VLA observation at 8.5 GHz ◦ with a bend of ∼ 90 at the end of the 2 arcsecond jet. A region of similar diffuse emission is also seen about 2 arcseconds south of the radio core. -
Cosmic Times Teachers' Guide Table of Contents
Cosmic Times Teachers’ Guide Table of Contents Cosmic Times Teachers’ Guide ....................................................................................... 1 1919 Cosmic Times ........................................................................................................... 3 Summary of the 1919 Articles...................................................................................................4 Sun’s Gravity Bends Starlight .................................................................................................4 Sidebar: Why a Total Eclipse?.................................................................................................4 Mount Wilson Astronomer Estimates Milky Way Ten Times Bigger Than Thought ............4 Expanding or Contracting? ......................................................................................................4 In Their Own Words................................................................................................................4 Notes on the 1919 Articles .........................................................................................................5 Sun's Gravity Bends Starlight..................................................................................................5 Sidebar: Why a Total Eclipse?.................................................................................................7 Mount Wilson Astronomer Estimates Milky Way Ten Times Bigger Than Thought ............7 Expanding or Contracting? ......................................................................................................8 -
2020 the Pathfinder View of the Sky LEGEND Canadian Hydrogen Intensity Mapping European VLBI Experiment (CHIME) - Network (EVN) - Canada Europe
Calendar 2020 The Pathfinder View of the Sky LEGEND Canadian Hydrogen Intensity Mapping European VLBI Experiment (CHIME) - Network (EVN) - Canada Europe enhanced Multi Element Remotely NenuFAR - France Linked Interferometer Network (e-MERLIN) - United Kingdom Low Frequency Array (LOFAR) - the MeerKAT Radio Netherlands Telescope - South Africa Five-hundred-meter Aperture Spherical Australian SKA Telescope (FAST) - Pathfinder (ASKAP) - China Australia (CHIME) Giant Metrewave Murchison Widefield Radio Telescope Array (MWA) - (GMRT) - India Australia VLBI Exploration of Effelsberg 100m Members of the SKA Organisation African Partner Countries Radio Astrometry Radio Telescope - Host Countries: Australia, South Africa, United Kingdom (VERA) - Japan Germany In the lead up to the SKA, many new groundbreaking radio elusive Fast Radio Bursts. They’re also allowing engineers The 2020 SKA calendar, called The Pathfinder View of the astronomy facilities have sprung up around the world in to develop new technical solutions like aperture arrays or Sky and featuring a small selection of the results already the past 10 years. These facilities are part of a global Phased Array Feeds. In so doing, they are paving the way coming out of 12 of these telescopes, is our tribute to effort to design and build ever-more sensitive instruments for the world’s largest radio telescope, the SKA. the pathfinder family as a whole, the people who have built to detect some of the faintest signals in the universe them and the people who are using them. The knowledge These facilities are now open to the community or going and grow new scientific and technical communities while and experience they’ve accumulated will guide us through through commissioning, and already they are providing benefiting society through cutting-edge R&D.