The VLA Low-band Ionospheric and Transient Experiment (VLITE)
|
|
- Egbert Blankenship
- 5 years ago
- Views:
Transcription
1 The VLA Low-band Ionospheric and Transient Experiment (VLITE) Walter Brisken (NRAO/UMN) Tracy Clarke (NRL) DiFX Workshop November 2014 Bologna, Italy
2 National Radio Astronomy Observatory s Very Large Array 330 MHz dipoles installed on VLA in 1990, and in regular use until MHz dipoles partially deployed in 1991, complete system in use from 1998 to 2009 Both the systems were developed through cooperation between NRAO and NRL code 7213 Systems were decommissioned by the VLA upgrade in 2009 Hicks et al. (2006) 2
3 NRL-Developed Wideband Low Frequency Receivers NRL-developed broadband low frequency receiver. NRL worked with NRAO to develop a new broadband low frequency receiver to replace the old narrow-band system Full system first light was May 2012 and system has been in operation on the VLA since that date In May 2013 Code 7213 proposed to develop a commensal low frequency software correlator backend for nearly continuous monitoring of ionospheric and transient events tapping into the new low frequency receivers VLITE: VLA Low Band Ionosperic and Transient Experiment Hicks et al. (2006) 3
4 VLITE: Overview VLITE is a new commensal backend on the NRAO VLA MHz It74 uses dedicated samplers, fiber transmission, and a dedicated backend software correlator to tap into the low band receivers on 10 VLA antennas VLITE samples a bandwidth of 64 MHz, centered on 352 MHz and provides a temporal resolution of 2s 330 and MHz spectral resolution of 100 khz VLITE will operate on all PI-driven observations at 1 GHz and above and is expected to produce several thousand hours of commensal P band data per year of operation VLASS will cover entire sky > -40d Right: One year of VLA pointings (>3000 hr) shown for the 330 MHz primary beam. This would cover 25% of the VLA sky. Total: >3000 hr 1 hr Hicks et al. (2006) 4 10 hr 100 hr
5 VLITE: Scientific Drivers Ionosphere: high resolution remote sensing of the Earth s ionosphere to 74 MHzcoupling mechanisms of fine, medium and large scale ionospheric study dynamics Transients (slow): searches of large (2.5 ) FoV for transients on time scales of 2s to 1 hour in real-time 330 MHzplus off-line searches for longer term transients Astrophysics: off-line process will provide sensitive simultaneous imaging for spectral studies, source size, extended emission properties etc for nearly all PI-driven science programs VLITE image of a 6 field around 3C286 showing VLITE in red, NVSS in blue and VLSS in green. Note the large number of sources seen well outside the 5 primary beam. This shows the power of VLITE for transient searches. VLITE image of the Tycho SNR made from a PI-driven observation.
6 VLITE: Current Status VLITE has undergone rapid deployment: 74 MHz System Requirements Review November 2013 Preliminary Design Review December 2013 Critical Design Review April 2014 MHzin June 2014 First system deployed on330 the VLA First light fringes: July 17, 2014 Single target field image: July 29, 2014 (5 antennas) Multi-target field image: August 8, 2014 (5 antennas) Full 10 antennas outfitted on the VLA September 1, 2014 Scientific and Technical Commissioning June November 2014 Full operations anticipated at end of commissioning For more information on VLITE contact: Namir Kassim (VLITE PI and transient pipeline) Tracy Clarke (VLITE Commissioning and astrophysics pipeline) Joseph Helmboldt (Ionospheric science) 6. Above: VLITE First Light Fringes on a QSO. VLITE image (red) of Crab nebula with Chandra in blue.
7 . VLITE Images 74 MHz 330 MHz VLITE module in VLA antenna. 3 Degrees Blue circle shows FWHM of VLITE PB. Note the large number of sources imaged well outside the beam. 7 First multi-source image of targets separated by 1.5. VLITE FoV is 2.5.
8 VLITE Technical Details 10 Antennas Dual pol: X/Y (really H/V!) 64 MHz bandwidth (320 to 384 MHz) Pointing / scan definitions based on VLA observing
9 VLITE Design Decisions Send data as UDP packets to correlator but receive them as raw packets Allows other software (e.g., transient search) to get another copy without any userspace interaction libevent is at the core of the vlite-executor application Found to be an excellent base for event-driven (packets, timers, interrupts, file i/o, ) software
10 DiFX changes required for VLITE Raw socket datastream input Vex2difx notation (example): networkport=eth2 # physical ethernet port WindowSize=42 # number of bytes to strip from beginning of each packet (42 for UDP) Datastream processes must run as root! sudo inside mpifxcorr wrapper does this Currently VDIF only X/Y polarization support Just a couple trivial changes needed This is not support for translation to R/L or for correlation of R/L with X/Y. It is just propagation of the labels through the system!
11 VLITE Correlator quirks Cleanly killing mpifxcorr quickly, cleanly is not reliable: using drastic measures now Sometimes one antenna gets weird patterns in weights (image courtesy Wendy Peters)
12 VLITE DiFX Correlator Overview vlite-difx1 40 Gbps Infiniband network Antenna V0 Each signal is up to 128 MB/s on 10 GbE Antenna V1 Output data: 600 kb/s on 10 GbE vlite-master To post-processor Antenna V8 Antenna V9 vlite-difx5
13 Low-Band Observatory (LOBO) DiFX Correlator The logical conclusion of the VLITE development path RCP LCP Subband 0 RCP Subband 1 LCP Node 0 A pair of 56 Gbps Infiniband networks Node 1 Antenna 1 RCP LCP Antenna 2 Subband 0 RCP Subband 1 LCP Node 2 Output data: 150 MB/s each subband on 10 GbE Node 3 Each signal is up to 512 MB/s on 10 GbE Node 54 (RCP+LCP could share a fiber if needed) Node 55 To post-processor RCP LCP Antenna 27 Subband 0 RCP Subband 1 LCP Node 52 Node 53 VFASTR Processor
An FPGA-Based Back End for Real Time, Multi-Beam Transient Searches Over a Wide Dispersion Measure Range
An FPGA-Based Back End for Real Time, Multi-Beam Transient Searches Over a Wide Dispersion Measure Range Larry D'Addario 1, Nathan Clarke 2, Robert Navarro 1, and Joseph Trinh 1 1 Jet Propulsion Laboratory,
More informationVLA Lowband. Frazer Owen
VLA Lowband Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array What is VLA Lowband? 54-86 MHz + 230-470 MHz: Two uncooled
More informationCasper Instrumentation at Green Bank
Casper Instrumentation at Green Bank John Ford September 28, 2009 The NRAO is operated for the National Science Foundation (NSF) by Associated Universities, Inc. (AUI), under a cooperative agreement. GBT
More informationPlan for Imaging Algorithm Research and Development
Plan for Imaging Algorithm Research and Development S. Bhatnagar July 05, 2009 Abstract Many scientific deliverables of the next generation radio telescopes require wide-field imaging or high dynamic range
More informationFigure 1 Photo of an Upgraded Low Band Receiver
NATIONAL RADIO ASTRONOMY OBSERVATORY SOCORRO, NEW MEXICO EVLA TECHNICAL REPORT #175 LOW BAND RECEIVER PERFORMANCE SEPTMBER 27, 2013 S.DURAND, P.HARDEN Upgraded low band receivers, figure 1, were installed
More informationCorrelator Development at Haystack. Roger Cappallo Haystack-NRAO Technical Mtg
Correlator Development at Haystack Roger Cappallo Haystack-NRAO Technical Mtg. 2006.10.26 History of Correlator Development at Haystack ~1973 Mk I 360 Kb/s x 2 stns. 1981 Mk III 112 Mb/s x 4 stns. 1986
More informationLWA1 Technical and Observational Information
LWA1 Technical and Observational Information Contents April 10, 2012 Edited by Y. Pihlström, UNM 1 Overview 2 1.1 Summary of Specifications.................................... 2 2 Signal Path 3 2.1 Station
More informationGreen Bank Instrumentation circa 2030
Green Bank Instrumentation circa 2030 Dan Werthimer and 800 CASPER Collaborators http://casper.berkeley.edu Upcoming Nobel Prizes with Radio Instrumentation Gravitational Wave Detection (pulsar timing)
More informationCross Correlators. Jayce Dowell/Greg Taylor. University of New Mexico Spring Astronomy 423 at UNM Radio Astronomy
Cross Correlators Jayce Dowell/Greg Taylor University of New Mexico Spring 2017 Astronomy 423 at UNM Radio Astronomy Outline 2 Re-cap of interferometry What is a correlator? The correlation function Simple
More informationN. Pingel, K. Rajwade, D.J. Pisano, D. Lorimer West Virginia University
Brian D. Jeffs, R. Black, J. Diao, M. Ruzindanna, K. Warnick Brigham Young University R. Prestage, J. Ford, S. White, R. Simon, W. Shillue, A. Roshi, V. Van Tonder NRAO: Green Bank Observatory and Central
More informationMWA Antenna Description as Supplied by Reeve
MWA Antenna Description as Supplied by Reeve Basic characteristics: Antennas are shipped broken down and require a few minutes to assemble in the field Each antenna is a dual assembly shaped like a bat
More informationSoftware Spectrometer for an ASTE Multi-beam Receiver. Jongsoo Kim Korea Astronomy and Space Science Institute
Software Spectrometer for an ASTE Multi-beam Receiver Jongsoo Kim Korea Astronomy and Space Science Institute Design Consideration software spectrometer for a near future ASTE multi-beam receiver spectrometer
More informationATA Memo No. 40 Processing Architectures For Complex Gain Tracking. Larry R. D Addario 2001 October 25
ATA Memo No. 40 Processing Architectures For Complex Gain Tracking Larry R. D Addario 2001 October 25 1. Introduction In the baseline design of the IF Processor [1], each beam is provided with separate
More informationPoS(11th EVN Symposium)113
High-order sampling technique for geodetic VLBI and the future National Institute of Information and Communications Technology, 893-1 Hirai, Kashima, Ibaraki 314-8501, Japan E-mail: takefuji@nict.go.jp
More informationRecent progress and future development of Nobeyama 45-m Telescope
Recent progress and future development of Nobeyama 45-m Telescope Masao Saito: Director of Nobeyama Radio Observatory Tetsuhiro Minamidani: Nobeyama Radio Observatory Outline Nobeyama 45-m Telescope Recent
More informationTesting a Prototype Blade Antenna at the LWDA Site
1 Testing a Prototype Blade Antenna at the LWDA Site Nagini Paravastu, William Erickson, Ylva Pihlstrom, Namir Kassim, Brian Hicks August 30, 2005 September 1, 2005 I. INTRODUCTION This report summarizes
More informationRecent progress in EVLA-specific algorithms. EVLA Advisory Committee Meeting, March 19-20, S. Bhatnagar and U. Rau
Recent progress in EVLA-specific algorithms EVLA Advisory Committee Meeting, March 19-20, 2009 S. Bhatnagar and U. Rau Imaging issues Full beam, full bandwidth, full Stokes noise limited imaging Algorithmic
More informationDiFX Correlator at Bonn
DiFX Correlator at Bonn 1 Alessandra Bertarini, IGG University of Bonn & MPIfR Bonn Walter Alef, MPIfR Bonn Arno Müskens, IGG University of Bonn Helge Rottmann, MPIfR Bonn Jan Wagner, MPIfR Bonn DiFX DiFX
More informationPresented by James Aguirre University of Pennsylvania 26 March 2013 SKA1 Low Workshop
Presented by James Aguirre University of Pennsylvania 26 March 2013 SKA1 Low Workshop UVa / NRAO Bradley Carilli Klima Gugliucci Parashare The PAPER Team UC Berkeley Parsons Pober Ali De Boer MacMahon
More informationSmart Antennas in Radio Astronomy
Smart Antennas in Radio Astronomy Wim van Cappellen cappellen@astron.nl Netherlands Institute for Radio Astronomy Our mission is to make radio-astronomical discoveries happen ASTRON is an institute for
More informationThe Jansky Very Large Array. Russ Taylor Ins-tute for Space Imaging Science University of Calgary
The Jansky Very Large Array Russ Taylor Ins-tute for Space Imaging Science University of Calgary The Jansky VLA 27x25m antennas in an upside- down Y, in one of four configura-ons, D (most compact) to A
More informationLow-frequency radio observations at Lustbühel Observatory M. Panchenko(1), H.O. Rucker(2)
Low-frequency radio observations at Lustbühel Observatory M. Panchenko(1), H.O. Rucker(2) (1) Space Research Institute, Graz, Austria (2) Commission for Astronomy, Austrian Academy of Sciences, Graz 1
More informationThe First Station of the Long Wavelength Array
University of New Mexico E-mail: henning@cosmos.phys.unm.edu Steven W. Ellingson Virginia Polytechnic Institute and State University E-mail: ellingson@vt.edu Gregory B. Taylor, Joseph Craig, Ylva Pihlström,
More informationVLBI DATA Acquisition Terminal modernization at the Deep Space Network
VLBI DATA Acquisition Terminal modernization at the Deep Space Network Cristina García Miró Madrid Deep Space Communication Complex NASA/JPL INTA/INSA Summary VLBI at Deep Space Network DSN VLBI Processor
More informationPoS(11th EVN Symposium)078
First successful VLBI observations in the EVN with VIRAC radio telescope RT-32 1 Engineering Research Institute, Ventspils International Radioastronomy Centre Inženieru Street 101, Ventspils, LV3600, Latvia
More informationThe US Technology Development Project for the SKA. TDP Progress Report. SKA 2010, Manchester
The US Technology Development Project for the SKA TDP Progress Report SKA 2010, Manchester Lynn Baker 22 March 2010 Lynn Baker SKA 2010 1 Reflectors, Feeds, LNA s Several wideband feed concepts moving
More informationMulti-octave radio frequency systems: Developments of antenna technology in radio astronomy and imaging systems
Multi-octave radio frequency systems: Developments of antenna technology in radio astronomy and imaging systems Professor Tony Brown School of Electrical and Electronic Engineering University of Manchester
More informationApplying full polarization A-Projection to very-wide fields of view instruments: An imager for LOFAR Cyril Tasse
Applying full polarization A-Projection to very-wide fields of view instruments: An imager for LOFAR Cyril Tasse ASTRON/Leiden: Joris van Zwieten, Bas van der Tol, Ger van Diepen NRAO: Sanjay Bhatnagar
More informationarxiv: v1 [astro-ph.im] 3 Sep 2010
arxiv:1009.0666v1 [astro-ph.im] 3 Sep 2010 University of New Mexico E-mail: henning@cosmos.phys.unm.edu Steven W. Ellingson Virginia Polytechnic Institute and State University E-mail: ellingson@vt.edu
More informationData Digitization & Transmission Session Moderator: Chris Langley
Data Digitization & Transmission Session Moderator: Chris Langley Atacama Large Millimeter/submillimeter Array Karl G. Jansky Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array
More informationRFI Mitigation Project at Italian Radio Telescopes
Workshop Detection and measurement of RFI in radio astronomy Yebes Observatory (IGN, Spain), June 8-9, 2017 RFI Mitigation Project at Italian Radio Telescopes G. Serra and many other people from Italian
More informationVLBI with IRAM 30m & NOEMA
VLBI with IRAM 30m & NOEMA Bologna 22.01.2015 M.Bremer, R.Garcia, O.Gentaz, A.Grosz, F.Gueth, C.Kramer, V.Pietu, S.Sanchez, K.Schuster IRAM is part of GMVA (2 sessions/yr @ 3mm since 2004) 1 mm experiments
More informationSpecifications for the GBT spectrometer
GBT memo No. 292 Specifications for the GBT spectrometer Authors: D. Anish Roshi 1, Green Bank Scientific Staff, J. Richard Fisher 2, John Ford 1 Affiliation: 1 NRAO, Green Bank, WV 24944. 2 NRAO, Charlottesville,
More informationProcessing Real-Time LOFAR Telescope Data on a Blue Gene/P
Processing Real-Time LOFAR Telescope Data on a Blue Gene/P John W. Romein Stichting ASTRON (Netherlands Institute for Radio Astronomy) Dwingeloo, the Netherlands 1 LOw Frequency ARray radio telescope 10
More informationEVLA Memo 151 EVLA Antenna Polarization at L, S, C, and X Bands
EVLA Memo 11 EVLA Antenna Polarization at L, S, C, and X Bands Rick Perley and Bob Hayward April 28, 211 Abstract The method described in EVLA Memo #131 for determining absolute antenna cross-polarization
More informationARRAY CONFIGURATION AND TOTAL POWER CALIBRATION FOR LEDA
ARRAY CONFIGURATION AND TOTAL POWER CALIBRATION FOR LEDA Frank Schinzel & Joe Craig (UNM) on behalf of the LEDA Collaboration USNC-URSI National Radio Science Meeting 2013 - Boulder, 09.01.2013 What is
More informationThe GMRT : a look at the Past, Present and Future
The GMRT : a look at the Past, Present and Future Yashwant Gupta & Govind Swarup National Centre for Radio Astrophysics Pune India URSI GASS Montreal 2017 The GMRT : a look at the Past, Present and Future
More informationA model for the SKA. Melvyn Wright. Radio Astronomy laboratory, University of California, Berkeley, CA, ABSTRACT
SKA memo 16. 21 March 2002 A model for the SKA Melvyn Wright Radio Astronomy laboratory, University of California, Berkeley, CA, 94720 ABSTRACT This memo reviews the strawman design for the SKA telescope.
More informationLOFAR: Special Issues
Netherlands Institute for Radio Astronomy LOFAR: Special Issues John McKean (ASTRON) ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) 1 Preamble http://www.astron.nl/~mckean/eris-2011-2.pdf
More informationResults from LWA1 Commissioning: Sensitivity, Beam Characteristics, & Calibration
Results from LWA1 Commissioning: Sensitivity, Beam Characteristics, & Calibration Steve Ellingson (Virginia Tech) LWA1 Radio Observatory URSI NRSM Jan 4, 2012 LWA1 Title 10-88 MHz usable, Galactic noise-dominated
More informationHow to SPAM the 150 MHz sky
How to SPAM the 150 MHz sky Huib Intema Leiden Observatory 26/04/2016 Main collaborators: Preshanth Jagannathan (UCT/NRAO) Kunal Mooley (Oxford) Dale Frail (NRAO) Talk outline The need for a low-frequency
More informationNRC Herzberg Astronomy & Astrophysics
NRC Herzberg Astronomy & Astrophysics SKA Pre-Construction Update Séverin Gaudet, Canadian Astronomy Data Centre David Loop, Director Astronomy Technology June 2016 update SKA Pre-Construction NRC Involvement
More informationComponents of Imaging at Low Frequencies: Status & Challenges
Components of Imaging at Low Frequencies: Status & Challenges Dec. 12th 2013 S. Bhatnagar NRAO Collaborators: T.J. Cornwell, R. Nityananda, K. Golap, U. Rau J. Uson, R. Perley, F. Owen Telescope sensitivity
More informationBRAND EVN EVN) Joint Research Activity in RadioNet4 Gino Tuccari & Walter Alef plus partners
BRAND EVN (BRoad-bAND EVN) Joint Research Activity in RadioNet4 Gino Tuccari & Walter Alef plus partners EVN Observing Bands < 22GHz Today in the EVN separate receivers cover: 18 cm - L band 13 cm - S
More information2-PAD: An Introduction. The 2-PAD Team
2-PAD: An Introduction The 2-PAD Team Workshop, Jodrell Bank, 10 Presented th November 2009 by 2-PAD: Dr An Georgina Introduction Harris Georgina Harris for the 2-PAD Team 1 2-PAD Objectives Demonstrate
More informationTHE ARO 1.3mm IMAGE-SEPARATING MIXER RECEIVER SYSTEM. Revision 1.0
THE ARO 1.3mm IMAGE-SEPARATING MIXER RECEIVER SYSTEM Revision 1.0 September, 2006 Table of Contents 1 System Overview... 3 1.1 Front-End Block Diagram... 5 1.2 IF System... 6 2 OPERATING PROCEDURES...
More informationLWA Station Design. S. Ellingson, Virginia Tech N. Kassim, U.S. Naval Research Laboratory. URSI General Assembly Chicago Aug 11, 2008 JPL
LWA Station Design S. Ellingson, Virginia Tech N. Kassim, U.S. Naval Research Laboratory URSI General Assembly Chicago Aug 11, 2008 JPL Long Wavelength Array (LWA) An LWA Station State of New Mexico, USA
More informationAllen Telescope Array & Radio Frequency Interference. Geoffrey C. Bower UC Berkeley
Allen Telescope Array & Radio Frequency Interference Geoffrey C. Bower UC Berkeley Allen Telescope Array Large N design 350 x 6.1m antennas Sensitivity of the VLA Unprecedented imaging capabilities Continuous
More informationPlanning (VLA) observations
Planning () observations 14 th Synthesis Imaging Workshop (May 2014) Loránt Sjouwerman National Radio Astronomy Observatory (Socorro, NM) Atacama Large Millimeter/submillimeter Array Karl G. Jansky Very
More informationEVLA Memo #166 Comparison of the Performance of the 3-bit and 8-bit Samplers at C (4 8 GHz), X (8 12 GHz) and Ku (12 18 GHz) Bands
EVLA Memo #166 Comparison of the Performance of the 3-bit and 8-bit Samplers at C (4 8 GHz), X (8 12 GHz) and Ku (12 18 GHz) Bands E. Momjian and R. Perley NRAO March 27, 2013 Abstract We present sensitivity
More informationASKAP Phased Array Feed Digital Beamformer Design Overview and Performance Characteristics
ASKAP Phased Array Feed Digital Beamformer Design Overview and Performance Characteristics John Tuthill, Tim Bateman, Grant Hampson, John Bunton, Andrew Brown, Daniel George, Mia Baquiran August 2016 CASS
More informationMay AA Communications. Portugal
SKA Top-level description A large radio telescope for transformational science Up to 1 million m 2 collecting area Operating from 70 MHz to 10 GHz (4m-3cm) Two or more detector technologies Connected to
More informationComparing MMA and VLA Capabilities in the GHz Band. Socorro, NM Abstract
Comparing MMA and VLA Capabilities in the 36-50 GHz Band M.A. Holdaway National Radio Astronomy Observatory Socorro, NM 87801 September 29, 1995 Abstract I explore the capabilities of the MMA and the VLA,
More informationBRAND EVN (BRoad-bAND EVN) Joint Research Activity in RadioNet4 Gino Tuccari & Walter Alef plus partners
BRAND EVN (BRoad-bAND EVN) Joint Research Activity in RadioNet4 Gino Tuccari & Walter Alef plus partners digital VLBI-receiver: ~1.5-15.5 GHz for the EVN and other telescopes Prototype for prime focus
More informationResults from the Yebes RAEGE telescope
Results from the Yebes RAEGE telescope P. de Vicente Observatorio de Yebes - CDT (IGN) The telescope Designed by Mt-Mechatronics Mechanics built by Asturfeito Telescope finished by end of 2013 Diameter:
More informationEVLA System Commissioning Results
EVLA System Commissioning Results EVLA Advisory Committee Meeting, March 19-20, 2009 Rick Perley EVLA Project Scientist t 1 Project Requirements EVLA Project Book, Chapter 2, contains the EVLA Project
More informationMore Radio Astronomy
More Radio Astronomy Radio Telescopes - Basic Design A radio telescope is composed of: - a radio reflector (the dish) - an antenna referred to as the feed on to which the radiation is focused - a radio
More informationTask Progress Milestone Summary. Page 1
1 ANTENNA RETROFITS 11/4/08 8/9/10 3 21 antennas retrofitted 4/13/09 4/13/09 4 24 antennas retrofitted 11/5/09 11/5/09 5 Last antenna retrofitted 8/9/10 8/9/10 6 WIDE-BAND RECEIVERS 2/4/08 10/15/12 7 L-Band
More informationEVLA Scientific Commissioning and Antenna Performance Test Check List
EVLA Scientific Commissioning and Antenna Performance Test Check List C. J. Chandler, C. L. Carilli, R. Perley, October 17, 2005 The following requirements come from Chapter 2 of the EVLA Project Book.
More informationThe Future: Ultra Wide Band Feeds and Focal Plane Arrays
The Future: Ultra Wide Band Feeds and Focal Plane Arrays Germán Cortés-Medellín NAIC Cornell University 1-1 Overview Chalmers Feed Characterization of Chalmers Feed at Arecibo Focal Plane Arrays for Arecibo
More informationTowards SKA Multi-beam concepts and technology
Towards SKA Multi-beam concepts and technology SKA meeting Meudon Observatory, 16 June 2009 Philippe Picard Station de Radioastronomie de Nançay philippe.picard@obs-nancay.fr 1 Square Kilometre Array:
More informationBeamformer and Calibration Performance for the Focal-plane L-band Array feed for the Green Bank Telescope (FLAG)
Beamformer and Calibration Performance for the Focal-plane L-band Array feed for the Green Bank Telescope (FLAG) B. D. Jeffs 1, K. F. Warnick 1, R. A. Black 1, M. Ruzindanna 1, M. Burnett 1 1 Brigham Young
More informationReal-time RFI Mitigation for the Upgraded GMRT
Real-time RFI Mitigation for the Upgraded GMRT Kaushal D. Buch Digital Backend Group, Giant Metrewave Radio Telescope, NCRA-TIFR, Pune, India kdbuch@gmrt.ncra.tifr.res.in The (Upgraded) GMRT Giant Metrewave
More informationActive Impedance Matched Dual-Polarization Phased Array Feed for the GBT
Active Impedance Matched Dual-Polarization Phased Array Feed for the GBT Karl F. Warnick, David Carter, Taylor Webb, Brian D. Jeffs Department of Electrical and Computer Engineering Brigham Young University,
More informationmodel 802C HF Wideband Direction Finding System 802C
model 802C HF Wideband Direction Finding System 802C Complete HF COMINT platform that provides direction finding and signal collection capabilities in a single integrated solution Wideband signal detection,
More informationTo: Deuterium Array Group From: Alan E.E. Rogers, K.A. Dudevoir and B.J. Fanous Subject: Low Cost Array for the 327 MHz Deuterium Line
DEUTERIUM ARRAY MEMO #068 MASSACHUSETTS INSTITUTE OF TECHNOLOGY HAYSTACK OBSERVATORY WESTFORD, MASSACHUSETTS 01886 August 2, 2007 Telephone: 978-692-4764 Fax: 781-981-0590 To: Deuterium Array Group From:
More informationNew Trends on Receivers Development" May 30, 2005, Medicina. RECEIVING SYSTEMs for the ANTENNAS OPERATED by the INSTITUTE of RADIOASTRONOMY in ITALY
New Trends on Receivers Development" May 30, 2005, Medicina RECEIVING SYSTEMs for the ANTENNAS OPERATED by the INSTITUTE of RADIOASTRONOMY in ITALY Alessandro Orfei IRA-INAF, Medicina station (Italy) RADIONET
More informationngvla Technical Overview
ngvla Technical Overview Mark McKinnon, Socorro, NM Outline ngvla Nominal Technical Parameters Technical Issues to Consider in Science Use Cases Programmatics Additional Information Pointed or Survey Telescope?
More informationBRAND EVN AND EVN) (BRoad-bAND Joint Research Activity in RadioNet4 Gino Tuccari & Walter Alef plus partners
BRAND EVN (BRoad-b AND EVN) (BRoad-bAND Joint Research Activity in RadioNet4 Gino Tuccari & Walter Alef plus partners digital VLBI-receiver: ~1.5-15.5 GHz for the EVN and other telescopes Prototype for
More informationPhased Array Feeds for the SKA. WP2.2.3 PAFSKA Consortium CSIRO ASTRON DRAO NRAO BYU OdP Nancay Cornell U Manchester
Phased Array Feeds for the SKA WP2.2.3 PAFSKA Consortium CSIRO ASTRON DRAO NRAO BYU OdP Nancay Cornell U Manchester Dish Array Hierarchy Dish Array L5 Elements PAF Dish Single Pixel Feeds L4 Sub systems
More informationVery Long Baseline Interferometry
Very Long Baseline Interferometry Cormac Reynolds, JIVE European Radio Interferometry School, Bonn 12 Sept. 2007 VLBI Arrays EVN (Europe, China, South Africa, Arecibo) VLBA (USA) EVN + VLBA coordinate
More informationStatus of LOFAR. Ronald Nijboer (ASTRON) On behalf of the LOFAR team
Status of LOFAR Ronald Nijboer (ASTRON) On behalf of the LOFAR team ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) -1- LOFAR: LOw Frequency ARray LBA: 10/30 80 MHz; HBA: 120
More informationarxiv: v1 [astro-ph.im] 5 Jan 2011
DiFX2: A more flexible, efficient, robust and powerful software correlator A.T. Deller 1,2, W.F. Brisken 1, C.J. Phillips 3, J. Morgan 4, W. Alef 5, R. Cappallo 6, E. Middelberg 7, J. Romney 1, H. Rottmann
More informationLBA Operations. Cormac Reynolds, Chris Phillips, Phil Edwards + LBA Team 19 November 2015 CSIRO ASTRONOMY & SPACE SCIENCE
LBA Operations Cormac Reynolds, Chris Phillips, Phil Edwards + LBA Team 19 November 2015 CSIRO ASTRONOMY & SPACE SCIENCE Hartebeesthoek 8000 km Real-time e-vlbi LBA 6 ant 1700km 40 ujy/beam (Ceduna) +Auscope
More information2. SYSTEM DESCRIPTION...
Implementation of a Digital Signal Processing Subsystem for a Long Wavelength Array Station Melissa Soriano, Robert Navarro, Larry D Addario, Elliott Sigman, Douglas Wang Jet Propulsion Laboratory California
More informationEVLA Technical Performance
EVLA Technical Performance With much essential help from Barry Clark, Ken Sowinski, Vivek Dhawan, Walter Brisken, George Moellenbrock, Bob Hayward, Dan Mertely, and many others. 1 Performance Requirements
More informationA Multi-Fielding SKA Covering the Range 100 MHz 22 GHz. Peter Hall and Aaron Chippendale, CSIRO ATNF 24 November 2003
A Multi-Fielding SKA Covering the Range 100 MHz 22 GHz Peter Hall and Aaron Chippendale, CSIRO ATNF 24 November 2003 1. Background Various analyses, including the recent IEMT report [1], have noted that
More informationLOFAR update: long baselines and other random topics
LOFAR update: long baselines and other random topics AIfA/MPIfR lunch colloquium Olaf Wucknitz wucknitz@astro.uni-bonn.de Bonn, 6th April 20 LOFAR update: long baselines and other random topics LOFAR previous
More informationPhased Array Feeds for Parkes. Robert Braun Science with 50 Years Young
Phased Array Feeds for Parkes Robert Braun Science with Parkes @ 50 Years Young Outline PAFs in the SKA context PAFSKA activities Apertif, BYU, NRAO, NAIC, DRAO, ASKAP ASKAP PAF MkI ASKAP PAF MkII Parkes:
More informationReceivers for. FFRF Tutorial by Tom Clark, NASA/GSFC & NVI Wettzell, March 19, 2009
Receivers for VLBI2010 FFRF Tutorial by Tom Clark, NASA/GSFC & NVI Wettzell, March 19, 2009 There is no fundamental difference between the receivers for PRIME FOCUS & CASSEGRAIN Except for: the beamwidth
More informationLow Frequency Radio Astronomy from the Lunar Surface
Low Frequency Radio Astronomy from the Lunar Surface R. J. MacDowall (1), T. J. Lazio (2), J. Burns (3) (1) NASA/GSFC, Greenbelt, MD, USA (2) JPL/Caltech, Pasadena, CA, USA (3) U. Colorado, Boulder, CO,
More informationPoS(11th EVN Symposium)073
Gino Tuccari, Salvo Buttaccio INAF Istituto di Radioastronomia, Contrada Renna Bassa, I-96017 Noto, Italy E-mail: g.tuccari@ira.inaf.it, Michael Wunderlich, David A. Graham, Alessandra Bertarini, Alan
More informationTechnical Considerations: Nuts and Bolts Project Planning and Technical Justification
Technical Considerations: Nuts and Bolts Project Planning and Technical Justification Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long
More informationHigh Fidelity Imaging of Extended Sources. Rick Perley NRAO Socorro, NM
High Fidelity Imaging of Extended Sources Rick Perley NRAO Socorro, NM A Brief History of Calibration (VLA) An Amazing Fact: The VLA was proposed, and funded, without any real concept of how to calibrate
More informationLonger baselines and how it impacts the ALMA Central LO
Longer baselines and how it impacts the ALMA Central LO 1 C. Jacques - NRAO October 3-4-5 2017 ALMA LBW Quick overview of current system Getting the data back is not the problem (digital transmission),
More informationAtacama Large Millimeter Array Project Status. M. Tarenghi ALMA Director
Atacama Large Millimeter Array Project Status M. Tarenghi ALMA Director Atacama Large Millimeter Array Specifications Partners: US (NSF)+Canada (NRC) - ESO+Spain - Chile 64 12-m antennas, at 5000 m altitude
More informationVLBI Developments in Australia Cormac Reynolds, Chris Phillips + LBA & Parkes Teams 14 November 2018 CSIRO ASTRONOMY & SPACE SCIENCE
VLBI Developments in Australia Cormac Reynolds, Chris Phillips + LBA & Parkes Teams 14 November 2018 CSIRO ASTRONOMY & SPACE SCIENCE LBA LBA VLBI array operated by CSIRO UTAS, AUT and SARAO (Hart) Parkes
More informationMarch Phased Array Technology. Andrew Faulkner
Aperture Arrays Michael Kramer Sparse Type of AA selection 1000 Sparse AA-low Sky Brightness Temperature (K) 100 10 T sky A eff Fully sampled AA-mid Becoming sparse Aeff / T sys (m 2 / K) Dense A eff /T
More informationCorrelator electronics. Alejandro Saez
Correlator electronics Alejandro Saez List of hardware elements to be discussed Correlator Interface Cards (CI) Correlator Cards (CC) Long Term Accumulator (LTA) Final Adder (FA) Data Port Interface (DPI)
More informationUseful Definitions. The two books are:
RESOURCES LIBRARY NEWS ARTICLES PAPERS & DOCUMENTS TECHNICAL DOCUMENTS PACIFIC ISLAND REGIONAL MAPS LINKS TO PAGES OF INTEREST Useful Definitions The following are some definitions of terms from two books
More informationDetrimental Interference Levels at Individual LWA Sites LWA Engineering Memo RFS0012
Detrimental Interference Levels at Individual LWA Sites LWA Engineering Memo RFS0012 Y. Pihlström, University of New Mexico August 4, 2008 1 Introduction The Long Wavelength Array (LWA) will optimally
More informationVERY LONG BASELINE INTERFEROMETRY
VERY LONG BASELINE INTERFEROMETRY Summer Student Lecture Socorro, June 28, 2011 Adapted from 2004 Summer School Lecture and 2005, 2007, and 2009 Summer Student Lectures WHAT IS VLBI? 2 Radio interferometry
More informationGiant Metrewave Radio Telescope (GMRT) - Introduction, Current System & ugmrt
Giant Metrewave Radio Telescope (GMRT) - Introduction, Current System & ugmrt Kaushal D. Buch Digital Backend Group, Giant Metrewave Radio Telescope kdbuch@gmrt.ncra.tifr.res.in Low frequency dipole array
More informationGoldstone Lunar Neutrino Search Nov
Goldstone Lunar Neutrino Search Nov. 16 2000 JPL: Peter Gorham, Kurt Liewer, Chuck Naudet UCLA: David Saltzberg, Dawn Williams (2001) Support: JPL DSN Science Services (G. Resch & M. Klein) (JPL staff)
More informationDense Aperture Array for SKA
Dense Aperture Array for SKA Steve Torchinsky EMBRACE Why a Square Kilometre? Detection of HI in emission at cosmological distances R. Ekers, SKA Memo #4, 2001 P. Wilkinson, 1991 J. Heidmann, 1966! SKA
More informationHans van der Marel Radio Observatory Division, ASTRON, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands
Radio Observatory Division, ASTRON, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands E-mail: marel@astron.nl Pieter Donker Radio Observatory Division, ASTRON, Oude Hoogeveensedijk 4, 7991 PD
More informationUniversity of Bristol - Explore Bristol Research. Peer reviewed version. Link to publication record in Explore Bristol Research PDF-document
Beach, M. A., Eneroth, P., Foo, S. E., Johansson, J., Karlsson, P., Lindmark, B., & McNamara, D. P. (2001). Description of a frequency division duplex measurement trial in the UTRA frequency band in urban
More informationDatasheet. 5 GHz Carrier Backhaul Radio. Model: AF-5X. Up to 500+ Mbps Real Throughput, Up to 200+ km Range. Full-Band Certification including DFS
5 GHz Carrier Backhaul Radio Model: AF-5X Up to 500+ Mbps Real Throughput, Up to 200+ km Range Full-Band Certification including DFS Ubiquiti s INVICTUS Custom Silicon Overview Ubiquiti Networks continues
More informationFigure 1: Worst-Case Emissions *FCC Class B compliance not estimated 4 below 200 MHz due to lack of antenna calibration and chamber reflectivity
On Monday, May 02, 2016, Carla Beaudet performed RFI tests on the Prime Focus Phased Array Feed backend, housed in a RFI chassis built by NRAO, the assembly henceforth referred to as the EUT, (Equipment
More informationCLOUDSDR RFSPACE #CONNECTED SOFTWARE DEFINED RADIO. final design might vary without notice
CLOUDSDR #CONNECTED SOFTWARE DEFINED RADIO final design might vary without notice 1 - PRELIMINARY SPECIFICATIONS http://www.rfspace.com v0.1 RFSPACE CloudSDR CLOUDSDR INTRODUCTION The RFSPACE CloudSDR
More information