High Resolution Radio Astronomy Using Very Long Baseline Interferometry
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Interferometric Spectrometers
LBNL-40663 UC-410 . ERNEST ORLANDO LAWRENCE BERKELEY NATIONAL LABORATORY Interferometric Spectrometers Anne Thome and Malcolm Howells Accelerator and Fusion Research Division June 1997 To be published as a chapter in Techniques ofVacuum Ultraviolet Physics, J~A-. Samson and D A. Ederer, eds.-, ·..-:~-:.:-':.::;:::;;;;r,;-:·.::~:~~:.::~-~~'*-~~,~~~;.=;t,ffl;.H;~:;;$,'~.~:~~::;;.:~< :.:,:::·.;:~·:..~.,·,;;;~.· l.t..•.-J.' "'"-""···,:·.:·· \ '-· . _ .....::' .~..... .:"~·~-!r.r;.e,.,...;. 17"'JC.(.; .• ,'~..: .••, ..._i;.·;~~(.:j. ... ..,.~1\;i:;.~ ...... J:' Academic Press, ....... ·.. ·... :.: ·..... ~ · ··: ·... · . .. .. .. - • 0 • ···...::; •• 0 ·.. • •• • •• ••• , •• •• •• ••• •••••• , 0 •• 0 .............. -·- " DISCLAIMER. This document was prepared as an account of work sponsored by the United States Government. While this document is believed to contain cmTect information, neither the United States Government nor any agency thereof, nor the Regents of the University of California, nor any of their employees, makes any warranty, express or implied, or assumes any legahesponsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by its trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof, or the -
Multidisciplinary Use of the J Very Long Baseline Array
PE84-16~690 Multidisciplinary Use of the j Very Long Baseline Array Proceedings of a Workshop REPRODUCED BY NATIONAL TECHNICAL NAS INFORMATION SERVICE us DEPAR1MENl OF COMMERCE NAE .. SPRINGFiElD, VA. 22161 10M 50272 ·101 REPORT DOCUMENTATION \1. REPORT NO. PAGE 4. TItle end Subtitle 50 Report Dete Multidisciplinary Use of the Very Long Baseline Array .. Februarv 1984 7. Author(l) L Performln. O...nlutlon Rept. No. 9. Performlna O...nlutlon Neme end Add.... 10. ProJKt/Tuk/Wort! Unit No. National Research Council 11. Contrect(C2 or Gr.nt(G) No. Commission on Physical Sciences, Mathematics, and DMA800-M0366/P Resources ~MDA903-83-M-5896/P i (G)AST-8303119 2101 Constitution Avenue, Washington, DC 20418 ~NA 83AAA02632/P 12. Sponsor1na O..enlutlon Neme end Add_ 11. Type of Report & Period Covered National Science Foundation Final Report. National Aeronautics and Space Administration 11/01/82-3/31/84 Defense Mapping Agency 14. NOAA National Geodetic Survev , Defense Adv. Res. Proj. 15. Supplementer)' Notes . Agency 16. Abltreet (Umlt 200 words) The National Research Council organized a workshop to gather together experts in very long baseline interferometry, astronomy, space navigation, general relativity and the earth sciences,. The purpose of the workshop was to provide a forum for consideration of the various possible multi disciplinary uses of the very long baseline array. Geophysical investigations received major attention. Geodesic uses of the very long baseline array were identified as were uses for fundamental astronomy investigations. Numerous specialized uses were identified. i, Document Anelysll e. Descriptors Very Long Baseline Array, astronomical research, space navigation, general relativity, geophysics, earth sciences, geodetic monitoring. -
HST/WFC3 OBSERVATIONS of an OFF-NUCLEAR SUPERBUBBLE in ARP 220 Kelly E
The Astrophysical Journal, 810:149 (11pp), 2015 September 10 doi:10.1088/0004-637X/810/2/149 © 2015. The American Astronomical Society. All rights reserved. HST/WFC3 OBSERVATIONS OF AN OFF-NUCLEAR SUPERBUBBLE IN ARP 220 Kelly E. Lockhart1, Lisa J. Kewley2, Jessica R. Lu1, Mark G. Allen3, David Rupke4, Daniela Calzetti5, Richard I. Davies6, Michael A. Dopita2, Hauke Engel6, Timothy M. Heckman7, Claus Leitherer8, and David B. Sanders1 1 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 2 Research School of Astronomy and Astrophysics, Australian National University, Cotter Road, Weston Creek ACT 2611, Australia 3 Observatoire de Strasbourg, UMR 7550, Strasbourg, F-67000, France 4 Department of Physics, Rhodes College, Memphis, TN 38112, USA 5 Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA 6 Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany 7 Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA 8 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Received 2015 March 7; accepted 2015 June 8; published 2015 September 9 ABSTRACT We present a high spatial resolution optical and infrared study of the circumnuclear region in Arp 220, a late-stage galaxy merger. Narrowband imaging using Hubble Space Telescope/WFC3 has resolved the previously observed peak in Hα+[N II] emission into a bubble-shaped feature. This feature measures 1″. 6 in diameter, or 600 pc, and is only 1″ northwest of the western nucleus. The bubble is aligned with the western nucleus and the large-scale outflow axis seen in X-rays. -
List of Acronyms
List of Acronyms List of Acronyms AAS American Astronomical Society AC (IVS) Analysis Center ACF AutoCorrelation Function ACU Antenna Control Unit ADC Analog to Digital Converter AES Advanced Engineering Services Co., Ltd (Japan) AGILE Astro-rivelatore Gamma ad Immagini LEggero satellite (Italy) AGN Active Galactic Nuclei AIPS Astronomical Image Processing System AIUB Astronomical Institute, University of Bern (Switzerland) AO Astronomical Object APSG Asia-Pacific Space Geodynamics program APT Asia Pacific Telescope ARIES Astronomical Radio Interferometric Earth Surveying program ASD Allan Standard Deviation ASI Agenzia Spaziale Italiana (Italy) ATA Allen Telescope Array (USA) ATCA Australia Telescope Compact Array (Australia) ATM Asynchronous Transfer Mode ATNF Australia Telescope National Facility (Australia) AUT Auckland University of Technology (New Zealand) A-WVR Advanced Water Vapor Radiometer BBC Base Band Converter BdRAO Badary Radio Astronomical Observatory (Russia) BIPM Bureau Internacional de Poids et Mesures (France) BKG Bundesamt f¨ur Kartographie und Geod¨asie (Germany) BMC Basic Module of Correlator BOSSNET BOSton South NETwork BVID Bordeaux VLBI Image Database BWG Beam WaveGuide CARAVAN Compact Antenna of Radio Astronomy for VLBI Adapted Network (Japan) CAS Chinese Academy of Sciences (China) CASPER Center for Astronomy Signal Processing and Electronics Research (USA) CAY Centro Astron´omico de Yebes (Spain) CC (IVS) Coordinating Center CDDIS Crustal Dynamics Data Information System (USA) CDP Crustal Dynamics Project CE -
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 Methods and Experiments of Shape Measurement for Off-Axis
materials Article The Methods and Experiments of Shape Measurement for Off-Axis Conic Aspheric Surface Shijie Li 1,2,*, Jin Zhang 1,2, Weiguo Liu 1,2, Haifeng Liang 1,2, Yi Xie 3 and Xiaoqin Li 4 1 Shaanxi Province Key Laboratory of Thin Film Technology and Optical Test, Xi’an Technological University, Xi’an 710021, China; [email protected] (J.Z.); [email protected] (W.L.); hfl[email protected] (H.L.) 2 School of Optoelectronic Engineering, Xi’an Technological University, Xi’an 710021, China 3 Display Technology Department, Luoyang Institute of Electro-optical Equipment, AVIC, Luoyang 471009, China; [email protected] 4 Library of Xi’an Technological University, Xi’an Technological University, Xi’an 710021, China; [email protected] * Correspondence: [email protected] Received: 26 March 2020; Accepted: 27 April 2020; Published: 1 May 2020 Abstract: The off-axis conic aspheric surface is widely used as a component in modern optical systems. It is critical for this kind of surface to obtain the real accuracy of the shape during optical processing. As is widely known, the null test is an effective method to measure the shape accuracy with high precision. Therefore, three shape measurement methods of null test including auto-collimation, single computer-generated hologram (CGH), and hybrid compensation are presented in detail in this research. Although the various methods have their own advantages and disadvantages, all methods need a special auxiliary component to accomplish the measurement. In the paper, an off-axis paraboloid (OAP) was chosen to be measured using the three methods along with auxiliary components of their own and it was shown that the experimental results involved in peak-to-valley (PV), root-mean-square (RMS), and shape distribution from three methods were consistent. -
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 -
Optical Low-Coherence Interferometry for Selected Technical Applications
BULLETIN OF THE POLISH ACADEMY OF SCIENCES TECHNICAL SCIENCES Vol. 56, No. 2, 2008 Optical low-coherence interferometry for selected technical applications J. PLUCIŃSKI∗, R. HYPSZER, P. WIERZBA, M. STRĄKOWSKI, M. JĘDRZEJEWSKA-SZCZERSKA, M. MACIEJEWSKI, and B.B. KOSMOWSKI Faculty of Electronics, Telecommunications and Informatics, Gdańsk University of Technology, 11/12 Narutowicza St., 80-952 Gdańsk, Poland Abstract. Optical low-coherence interferometry is one of the most rapidly advancing measurement techniques. This technique is capable of performing non-contact and non-destructive measurement and can be used not only to measure several quantities, such as temperature, pressure, refractive index, but also for investigation of inner structure of a broad range of technical materials. We present theoretical description of low-coherence interferometry and discuss its unique properties. We describe an OCT system developed in our Department for investigation of the structure of technical materials. In order to provide a better insight into the structure of investigated objects, our system was enhanced to include polarization state analysis capability. Measurement results of highly scattering materials e.g. PLZT ceramics and polymer composites are presented. Moreover, we present measurement setups for temperature, displacement and refractive index measurement using low coherence interferometry. Finally, some advanced detection setups, providing unique benefits, such as noise reduction or extended measurement range, are discussed. Key words: low-coherence interferometry (LCI), optical coherence tomography (OCT), polarization-sensitive OCT (PS-OCT). 1. Introduction 2. Analysis of two-beam interference Low-coherence interferometry (LCI), also known as white- 2.1. Two-beam interference – time domain description. light interferometry (WLI), is an attractive measurement Let us consider interference of two beams emitted from method offering high measurement resolution, high sensi- a quasi-monochromatic light source located at a point P, i.e. -
A Study of Giant Radio Galaxies at Ratan-600 173
Bull. Spec. Astrophys. Obs., 2011, 66, 171–182 c Special Astrophysical Observatory of the Russian AS, 2018 A Study of Giant Radio Galaxies at RATAN-600 M.L. Khabibullinaa, O.V. Verkhodanova, M. Singhb, A. Piryab, S. Nandib, N.V. Verkhodanovaa a Special Astrophysical Observatory of the Russian AS, Nizhnij Arkhyz 369167, Russia; b Aryabhatta Research Institute of Observational Sciences, Manora Park, Nainital 263 129, India Received July 28, 2010; accepted September 15, 2010. We report the results of flux density measurements in the extended components of thirteen giant radio galaxies, made with the RATAN-600 in the centimeter range. Supplementing them with the WENSS, NVSS and GB6 survey data we constructed the spectra of the studied galaxy components. We computed the spectral indices in the studied frequency range and demonstrate the need for a detailed account of the integral contribution of such objects into the background radiation. Key words: Radio lines: galaxies—techniques: radar astronomy 1. INTRODUCTION than the one, expected from the evolutional models. As noted in [8], such radio galaxies may affect the According to the generally accepted definition, gi- processes of galaxy formation, since the pressure of ant radio galaxies (GRGs) are the radio sources with gas, outflowing from the radio source, may compress linear sizes greater than 1 Mpc, i.e. the largest ra- the cold gas clouds thus initiating the development dio sources in the Universe. They mostly belong to of stars on the one hand, and stop the formation of the morphological type FR II [1] and are identified galaxies on the other hand. -
Adventures in Radio Astronomy Instrumentation and Signal Processing
Adventures in Radio Astronomy Instrumentation and Signal Processing by Peter Leonard McMahon Submitted to the Department of Electrical Engineering in partial fulfillment of the requirements for the degree of Master of Science in Electrical Engineering at the University of Cape Town July 2008 Supervisor: Professor Michael Inggs Co-supervisors: Dr Dan Werthimer, CASPER1, University of California, Berkeley Dr Alan Langman, Karoo Array Telescope arXiv:1109.0416v1 [astro-ph.IM] 2 Sep 2011 1Center for Astronomy Signal Processing and Electronics Research Abstract This thesis describes the design and implementation of several instruments for digi- tizing and processing analogue astronomical signals collected using radio telescopes. Modern radio telescopes have significant digital signal processing demands that are typically best met using custom processing engines implemented in Field Pro- grammable Gate Arrays. These demands essentially stem from the ever-larger ana- logue bandwidths that astronomers wish to observe, resulting in large data volumes that need to be processed in real time. We focused on the development of spectrometers for enabling improved pulsar2 sci- ence on the Allen Telescope Array, the Hartebeesthoek Radio Observatory telescope, the Nan¸cay Radio Telescope, and the Parkes Radio Telescope. We also present work that we conducted on the development of real-time pulsar timing instrumentation. All the work described in this thesis was carried out using generic astronomy pro- cessing tools and hardware developed by the Center for Astronomy Signal Processing and Electronics Research (CASPER) at the University of California, Berkeley. We successfully deployed to several telescopes instruments that were built solely with CASPER technology, which has helped to validate the approach to developing radio astronomy instruments that CASPER advocates.