Jodrell Bank Observatory Relevant Sections of This Evaluation Report
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
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. -
Square Kilometre Array Computational Challenges
Square Kilometre Array Computational Challenges Paul Alexander Paul Alexander SKA Computational Challenges What is the Square Kilometre Array (SKA) • Next Generation radio telescope – compared to best current instruments it is ... E-MERLIN • ~100 times sensitivity • ~ 106 times faster imaging the sky • More than 5 square km of collecting area on sizes 3000km eVLA 27 27m dishes Longest baseline 30km GMRT 30 45m dishes Longest baseline 35 km Paul Alexander SKA Computational Challenges What is the Square Kilometre Array (SKA) • Next Generation radio telescope – compared to best current instruments it is ... • ~100 times sensitivity • ~ 106 times faster imaging the sky • More than 5 square km of collecting area on sizes 3000km • Will address some of the key problems of astrophysics and cosmology (and physics) • Builds on techniques developed in Cambridge • It is an interferometer • Uses innovative technologies... • Major ICT project • Need performance at low unit cost Paul Alexander SKA Computational Challenges Dishes Paul Alexander SKA Computational Challenges Phased Aperture array Paul Alexander SKA Computational Challenges also a Continental sized Radio Telescope • Need a radio-quiet site • Very low population density • Large amount of space • Possible sites (decision 2012) • Western Australia • Karoo Desert RSA Paul Alexander SKA Computational Challenges Sensitivity comparison 12,000 Sensitivity Comparison 10,000 1 - K 2 8,000 SKA2 6,000 SKA2 SKA1 MeerKAT LOFAR ASKAP 4,000 Sensitivity: Aeff/Tsys m Sensitivity:Aeff/Tsys eVLA SKA1 2,000 -
Introduction to Radio Astronomy
Introduction to Radio Astronomy Greg Hallenbeck 2016 UAT Workshop @ Green Bank Outline Sources of Radio Emission Continuum Sources versus Spectral Lines The HI Line Details of the HI Line What is our data like? What can we learn from each source? The Radio Telescope How do we actually detect this stuff? How do we get from the sky to the data? I. Radio Emission Sources The Electromagnetic Spectrum Radio ← Optical Light → A Galaxy Spectrum (Apologies to the radio astronomers) Continuum Emission Radiation at a wide range of wavelengths ❖ Thermal Emission ❖ Bremsstrahlung (aka free-free) ❖ Synchrotron ❖ Inverse Compton Scattering Spectral Line Radiation at a wide range of wavelengths ❖ The HI Line Categories of Emission Continuum Emission — “The Background” Radiation at a wide range of wavelengths ❖ Thermal Emission ❖ Synchrotron ❖ Bremsstrahlung (aka free-free) ❖ Inverse Compton Scattering Spectral Lines — “The Spikes” Radiation at specific wavelengths ❖ The HI Line ❖ Pretty much any element or molecule has lines. Thermal Emission Hot Things Glow Emit radiation at all wavelengths The peak of emission depends on T Higher T → shorter wavelength Regulus (12,000 K) The Sun (6,000 K) Jupiter (100 K) Peak is 250 nm Peak is 500 nm Peak is 30 µm Thermal Emission How cold corresponds to a radio peak? A 3 K source has peak at 1 mm. Not getting any colder than that. Synchrotron Radiation Magnetic Fields Make charged particles move in circles. Accelerating charges radiate. Synchrotron Ingredients Strong magnetic fields High energies, ionized particles. Found in jets: ❖ Active galactic nuclei ❖ Quasars ❖ Protoplanetary disks Synchrotron Radiation Jets from a Protostar At right: an optical image. -
50 Years of the Lovell Telescope Transcript
50 years of the Lovell telescope Transcript Date: Wednesday, 5 December 2007 - 12:00AM 50 YEARS OF THE LOVELL TELESCOPE Professor Ian Morison The Early days at Jodrell Bank In late 1945 Dr Bernard Lovell (as he then was) returned to Manchester University after working on the development of radar during the war years. His aim was to continue his researches into cosmic rays - highly energetic particles that enter the Earth's atmosphere from outer space. He had the idea that sporadic echoes sometimes received by military radars might be the result of cosmic rays entering the atmosphere and thus radar observations might provide a new way to continue his researches. Radar observations were not practical in the centre of Manchester so he took his ex-army radar system out to the University's Botanical Grounds at Jodrell Bank, some 20 miles to the south. By the middle of December 1945, the system was operating and his team was soon able to prove that the echoes were coming not from cosmic rays but from ionized meteor trails left behind when small particles, released from comets, are burnt up in the upper atmosphere of the Earth. Radar Antenna in the Botany Grounds. The Jodrell Bank Experimental Station. The observations continued and, to house the expanding staff and equipment, the Jodrell Bank Experimental Station was built in the field next to the Botanic Grounds. Lovell realised that a much more sensitive radio telescope would be required to detect cosmic rays and so, in 1947, the researchers built a large parabolic reflector, 66-m across, pointing upwards to observe the sky passing overhead. -
The E-MERLIN Notebook
The e-MERLIN Notebook IRIS Collaboration F2F Meeting - 4 April 2019 Dr. Rachael Ainsworth Jodrell Bank Centre for Astrophysics University of Manchester @rachaelevelyn Overview ● Motivation ● Brief intro to e-MERLIN ● Pieces of the puzzle: ○ e-MERLIN CASA Pipeline ○ Data Archive ○ Open Notebooks ● Putting everything together: ○ e-MERLIN @ IRIS Motivation (Whitaker 2018, https://doi.org/10.6084/m9.figshare.7140050.v2 ) “Computational science has led to exciting new developments, but the nature of the work has exposed limitations in our ability to evaluate published findings. Reproducibility has the potential to serve as a minimum standard for judging scientific claims when full independent replication of a study is not possible.” (Peng 2011; https://doi.org/10.1126/science.1213847) e-MERLIN (e)MERLIN ● enhanced Multi Element Remotely Linked Interferometer Network ● An array of 7 radio telescopes spanning 217 km across the UK ● Connected by a superfast optical fibre network to its headquarters at Jodrell Bank Observatory. ● Has a unique position in the world with an angular resolution comparable to that of the Hubble Space Telescope and carrying out centimetre wavelength radio astronomy with micro-Jansky sensitivities. http://www.e-merlin.ac.uk/ (e)MERLIN ● Does not have a publicly accessible data archive. http://www.e-merlin.ac.uk/ Radio Astronomy Software: CASA ● The CASA infrastructure consists of a set of C++ tools bundled together under an iPython interface as data reduction tasks. ● This structure provides flexibility to process the data via task interface or as a python script. ● https://casa.nrao.edu/ Pieces of the puzzle e-MERLIN CASA Pipeline ● Developed openly on GitHub (Moldon, et al.) ● Python package composed of different modules that can be run together sequentially to produce calibration tables, calibrated data, assessment plots and a summary weblog. -
The Merlin - Phase 2
Radio Interferometry: Theory, Techniques and Applications, 381 IAU Coll. 131, ASP Conference Series, Vol. 19, 1991, T.J. Comwell and R.A. Perley (eds.) THE MERLIN - PHASE 2 P.N. WILKINSON University of Manchester, Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire, SKll 9DL, United Kingdom ABSTRACT The Jodrell Bank MERLIN is currently being upgraded to produce higher sensitivity and higher resolving power. The major capital item has been a new 32m telescope located at MRAO Cambridge which will operate to at least 50 GHz. A brief outline of the upgraded MERLIN and its performance is given. INTRODUCTION The MERLIN (Multi-Element Radio-Linked Interferometer Network), based at Jodrell Bank, was conceived in the mid-1970s and first became operational in 1980. It was a bold concept; no one had made a real-time long-baseline interferometer array with phase-stable local oscillator links before. Six remotely operated telescopes, controlled via telephone lines, are linked to a control computer at Jodrell Bank. The rf signals are transmitted to Jodrell via commercial multi-hop microwave links operating at 7.5 GHz. The local oscillators are coherently slaved to a master oscillator via go-and- return links operating at L-band, the change in the link path-length being taken out in software. This single-frequency L-band link can transfer phase to the equivalent of < 1 picosec (< 0.3 mm of path length) on timescales longer than a few seconds. A detailed description of the MERLIN system has been given by Thomasson (1986). The MERLIN has provided the UK with a unique astronomical facility, one which has made important contributions to extragalactic radio source and OH maser studies. -
The Lovell Telescope … Through Its Surfaces Simon Garrington, JBO/University of Manchester
The Lovell Telescope … through its surfaces Simon Garrington, JBO/University of Manchester • Original design & redesign: 1950-1957 • Radical modification & new surface: 1971 • Replacement of surface: 2001 • Replacement of original Picture A. Holloway surface: 2018 • Other consequences: foundations O1 Original MkI proposal and changes • Concept & proposals: 1950-1 • Lovell-Husband Sep 1949 • Radio Astronomy Cttee 1950 • rail track; towers, cradle, 4-inch mesh • 2-inch mesh/5-in profile by 20 Mar 1951 submission • Design changes • 21cm line discovered (Ewen 25 Mar 1951) • Inner 100’ mesh 1x2-in ‘at no cost’ ? Sep 1952 • Interest from Air Ministry: 10cm radar • March 1954: 3/4-in mesh -> stronger cradle … but Air Ministry step back O2 Original MkI proposal and changes • Concept & proposals: 1950-1 • Lovell-Husband Sep 1949 • Radio Astronomy Cttee 1950 • rail track; towers, cradle, 4-inch mesh • 2-inch mesh/5-in profile by 20 Mar 1951 submission • Design changes • 21cm line discovered (Ewen 25 Mar 1951) • Inner 100’ mesh 1x2-in ‘at no cost’ ? Sep 1952 • Interest from Air Ministry: 10cm radar • March 1954: 3/4-in mesh -> stronger cradle … but Air Ministry step back O3 Original MkI proposal and changes • Concept & proposals: 1950-1 • Lovell-Husband Sep 1949 • Radio Astronomy Cttee 1950 • rail track; towers, cradle, 4-inch mesh • 2-inch mesh/5-in profile by 20 Mar 1951 submission • Design changes • 21cm line discovered (Ewen 25 Mar 1951) • Inner 100’ mesh 1x2-in ‘at no cost’ ? Sep 1952 • Interest from Air Ministry: 10cm radar • March 1954: 3/4-in -
Jod Bank 1.Indd 56 23/10/2019 08:11 Feature
Feature Radio Eye on the Sky (Part I) Dr Bruce Taylor HB9ANY Dr Bruce Taylor HB9ANY relates how chance, [email protected] skill, tenacity and the enthusiasm of a botanist n July 7th 2019 Jodrell Bank radio amateur created a technical masterpiece. Observatory, the home of what is surely the most iconic radio antenna in the world, was de- Oclared a World Heritage Site in the same cultural category as the Great Wall of China and the Pyramid Fields from Giza to Dahshur. It was recognised by UNESCO as “a masterpiece of human creative genius” because of its scientifi c achievements in advancing our understanding of the uni- verse. But as the champagne fl owed in cel- ebration of this magnifi cent accolade, few remembered that 62 years earlier its found- er, Bernard Lovell, endured immense per- sonal hardship and narrowly escaped incar- ceration during the technical, Political and fi nancial drama surrounding its creation. In 1939, 25 year-old Lovell was one of many talented university teachers and re- searchers who abandoned their Peaceful studies to join the war effort. They teamed uP with hundreds of radio amateurs and professional electronics experts who con- tributed their technical skills to the defence of the United Kingdom. Lovell was just about to set out from Manchester for the Pyrenees, in a small van loaded with equip- 1 ment for cosmic ray research, when he re- ceived a call to rePort to the Chain Home at which available thermionic valves could (CH) laboratories at Bawdsey Manor on generate signifi cant power was about the east coast of England. -
Detection Statistics of the Radioastron AGN Survey
Available online at www.sciencedirect.com ScienceDirect Advances in Space Research 65 (2020) 705–711 www.elsevier.com/locate/asr Detection statistics of the RadioAstron AGN survey Y.Y. Kovalev a,b,c,⇑, N.S. Kardashev a,†, K.V. Sokolovsky a,d,e, P.A. Voitsik a,T.Anf, J.M. Anderson g,h, A.S. Andrianov a, V.Yu. Avdeev a, N. Bartel i, H.E. Bignall j, M.S. Burgin a, P.G. Edwards k, S.P. Ellingsen l, S. Frey m, C. Garcı´a-Miro´ n, M.P. Gawron´ski o, F.D. Ghigo p, T. Ghosh p,q, G. Giovannini r,s, I.A. Girin a, M. Giroletti r, L.I. Gurvits t,u, D.L. Jauncey k,v, S. Horiuchi w, D.V. Ivanov x, M.A. Kharinov x, J.Y. Koay y, V.I. Kostenko a, A.V. Kovalenko aa, Yu.A. Kovalev a, E.V. Kravchenko r,a, M. Kunert-Bajraszewska o, A.M. Kutkin a,z, S.F. Likhachev a, M.M. Lisakov c,a, I.D. Litovchenko a, J.N. McCallum l, A. Melis ab, A.E. Melnikov x, C. Migoni ab, D.G. Nair t, I.N. Pashchenko a, C.J. Phillips k, A. Polatidis z, A.B. Pushkarev a,ad, J.F.H. Quick ae, I.A. Rakhimov x, C. Reynolds j, J.R. Rizzo af, A.G. Rudnitskiy a, T. Savolainen ag,ah,c, N.N. Shakhvorostova a, M.V. Shatskaya a, Z.-Q. Shen f,ac, M.A. Shchurov a, R.C. Vermeulen z, P. de Vicente ai, P. -
Dynamics of the Arecibo Radio Telescope
DYNAMICS OF THE ARECIBO RADIO TELESCOPE Ramy Rashad 110030106 Department of Mechanical Engineering McGill University Montreal, Quebec, Canada February 2005 Under the supervision of Professor Meyer Nahon Abstract The following thesis presents a computer and mathematical model of the dynamics of the tethered subsystem of the Arecibo Radio Telescope. The computer and mathematical model for this part of the Arecibo Radio Telescope involves the study of the dynamic equations governing the motion of the system. It is developed in its various components; the cables, towers, and platform are each modeled in succession. The cable, wind, and numerical integration models stem from an earlier version of a dynamics model created for a different radio telescope; the Large Adaptive Reflector (LAR) system. The study begins by converting the cable model of the LAR system to the configuration required for the Arecibo Radio Telescope. The cable model uses a lumped mass approach in which the cables are discretized into a number of cable elements. The tower motion is modeled by evaluating the combined effective stiffness of the towers and their supporting backstay cables. A drag model of the triangular truss platform is then introduced and the rotational equations of motion of the platform as a rigid body are considered. The translational and rotational governing equations of motion, once developed, present a set of coupled non-linear differential equations of motion which are integrated numerically using a fourth-order Runge-Kutta integration scheme. In this manner, the motion of the system is observed over time. A set of performance metrics of the Arecibo Radio Telescope is defined and these metrics are evaluated under a variety of wind speeds, directions, and turbulent conditions. -
Fact Sheet Fact Sheet
FactFact sheet sheet What is the SKA? The Square Kilometre Array (SKA) is a next-generation radio telescope that will be vastly more sensitive than the best present-day instruments. It will give astronomers remarkable insights into the formation of the early Universe, including the emergence of the first stars, galaxies and other structures. This will shed light on the birth, and eventual death, of the cosmos. The SKA will require new technology and progress in Why build the SKA? fundamental engineering in fields such as information and communication technology, high performance computing In order to answer some fundamental questions about the and production manufacturing techniques. It will comprise origin and evolution of the Universe, a more sensitive radio a vast array of antennas, arranged in clusters to be spread telescope is needed that can detect the very weak signals over 3000 kilometres or more. The antennas will be linked coming from the edge of the cosmos. A telescope such as the electronically to form one enormous telescope. The SKA will be able to “see” distant objects in the very young combination of unprecedented collecting area, versatility Universe and provide answers to questions such as the and sensitivity will make the SKA the world’s premier imaging emergence of the first stars, galaxies and other structures. and survey telescope over a wide range of radio frequencies, Because the speed of light is finite and the size of the Universe producing the sharpest pictures of the sky of any telescope. is so large, telescopes are effectively time machines, enabling astronomers to look into the past and study the Universe as it The SKA will: was billions of years ago. -
The Meerkat Radio Telescope Rhodes University SKA South Africa E-Mail: a B Pos(Meerkat2016)001 Justin L
The MeerKAT Radio Telescope PoS(MeerKAT2016)001 Justin L. Jonas∗ab and the MeerKAT Teamb aRhodes University bSKA South Africa E-mail: [email protected] This paper is a high-level description of the development, implementation and initial testing of the MeerKAT radio telescope and its subsystems. The rationale for the design and technology choices is presented in the context of the requirements of the MeerKAT Large-scale Survey Projects. A technical overview is provided for each of the major telescope elements, and key specifications for these components and the overall system are introduced. The results of selected receptor qual- ification tests are presented to illustrate that the MeerKAT receptor exceeds the original design goals by a significant margin. MeerKAT Science: On the Pathway to the SKA, 25-27 May, 2016, Stellenbosch, South Africa ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). http://pos.sissa.it/ MeerKAT Justin L. Jonas 1. Introduction The MeerKAT radio telescope is a precursor for the Square Kilometre Array (SKA) mid- frequency telescope, located in the arid Karoo region of the Northern Cape Province in South Africa. It will be the most sensitive decimetre-wavelength radio interferometer array in the world before the advent of SKA1-mid. The telescope and its associated infrastructure is funded by the government of South Africa through the National Research Foundation (NRF), an agency of the Department of Science and Technology (DST). Construction and commissioning of the telescope has been the responsibility of the SKA South Africa Project Office, which is a business unit of the PoS(MeerKAT2016)001 NRF.