Netherlands Institute for Radio Astronomy 1 APERTIF beamformer and correlator requirements Laurens Bakker.

Slides:



Advertisements
Similar presentations
Beamformer implementations (Mike Jones, Kris Zarb Adami, David Sinclair, Chris Shenton) Starting with top level considerations for now, ie Not, which FPGA.
Advertisements

Digital Correlated Double Sampling for ZTF Roger Smith and Stephen Kaye California Institute of Technology.
Reconfigurable Computing (EN2911X, Fall07) Lecture 04: Programmable Logic Technology (2/3) Prof. Sherief Reda Division of Engineering, Brown University.
Digital FX Correlator Nimish Sane Center for Solar-Terrestrial Research New Jersey Institute of Technology, Newark, NJ EOVSA Technical Design Meeting.
David Hawkins Exascale Signal Processing for Millimeter-Wavelength Radio Interferometers David Hawkins
Digital FX Correlator Nimish Sane Center for Solar-Terrestrial Research New Jersey Institute of Technology, Newark, NJ EOVSA Technical Design Meeting.
DFT Filter Banks Steven Liddell Prof. Justin Jonas.
PELICAN Imaging Framework Imaging on short timescales leads to very large correlator output data rates. In order to cope with these rates and produce updated.
BDT Radio – 1b – CMV 2009/09/04 Basic Detection Techniques 1b (2009/09/04): Single pixel feeds Theory: Brightness function Beam properties Sensitivity,
BDT Radio – 2b – CMV 2009/10/09 Basic Detection Techniques 2b (2009/10/09): Focal Plane Arrays Case study: WSRT System overview Receiver and.
Front end design Front end like SEQUOIA, except that both signal polarizations combined with ortho-mode transition. Entire signal band down-converted.
Prototype SKA Technologies at Molonglo: 3. Beamformer and Correlator J.D. Bunton Telecommunications and Industrial Physics, CSIRO. Australia. Correlator.
Signal Processing for Aperture Arrays. AAVS1 256 antenna elements distributed over –4 stations –64 elements each.
Solar corona observations at decameter wavelengths Artem Koval Institute of Radio Astronomy Kharkov, Ukraine.
Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Digital Signal Processing.
AA-mid demonstrator Dion Kant AAVP – 10 December 2010, Cambridge, UK.
Name1 SKA(DS) System Design Aspects 4 th SKADS Workshop, Lisbon, 2-3 October 2008 SKA(DS) System Design Aspects: building a system Laurens Bakker.
The ALMA Correlator Gianni Comoretto, J.C. Webber, A. Baudry, C.M. Broadwell, R. P. Escoffier, J.H. Greenberg, R.R. Treacy, P. Cais, B Quertier, P. Camino,
AA-Low Technical Progress Meeting, October 2012, Medicina, Italy AAVS0 & AAVS0.5: System Design and Test Plan Nima Razavi-Ghods Eloy de Lera Acedo.
Backend electronics for radioastronomy G. Comoretto.
ASKAP Signal Processing Overview DIFX Users and Developers Meeting
RN /08/05 National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Implementation of an Antenna.
1 PROPAGATION ASPECTS FOR SMART ANTENNAS IN WIRELESS SYSTEMS JACK H. WINTERS AT&T Labs - Research Red Bank, NJ July 17,
10 January 2006AAS EVLA Town Hall Meeting1 The EVLA: A North American Partnership The EVLA Project on the Web
Danie Ludick MScEng Study Leader: Prof. D.B. Davidson Computational Electromagnetics Group Stellenbosch University Extended Studies of Focal Plane Arrays.
NTD/xNTD Signal Processing Presented by: John Bunton Signal Processing team: Joseph Pathikulangara, Jayasri Joseph, Ludi de Souza and John Bunton Plus.
Paul Alexander & Jaap BregmanProcessing challenge SKADS Wide-field workshop SKA Data Flow and Processing – a key SKA design driver Paul Alexander and Jaap.
XNTD/SKAMP/LFD Correlator 4th RadioNet Engineering Forum Workshop Next Generation Correlators for Radio Astronomy and Geodesy June 2006, Groningen,
Research of long distance clock distribution system Université Libre de Bruxelles (IIHE) Yifan Yang, Kael Hanson, Aongus Ó Murchadha, Thomas Meures, Michael.
Casper Signal Processing Workshop 2009 SKA Signal Processing (Preliminary) Wallace Turner Domain Specialist for Signal Processing.
Next Generation Digital Back-ends at the GMRT Yashwant Gupta Yashwant Gupta National Centre for Radio Astrophysics Pune India CASPER meeting Cambridge.
Mileura Widefield Array – Low Frequency Demonstrator MHz * Currently in “Early Deployment” phase Goal: HI at redshift 6 to 17.
Casper 2010Marc Torres Part 2: Building blocks for the next generation.
© ASTRON On the Fly LOFAR Station Correlator André W. Gunst.
Integrated receivers for mid-band SKA Suzy Jackson Engineer, Australia Telescope National Facility SKADS FP6 Meeting – Chateau de Limelette – 4-6 November,
1 Reconfigurable Acceleration of Microphone Array Algorithms for Speech Enhancement Ka Fai Cedric Yiu, Yao Lu, Xiaoxiang Shi The Hong Kong Polytechnic.
Australian Astronomy MNRF Development of Monolithic Microwave Integrated Circuits (MMIC) ATCA Broadband Backend (CABB)
MeerKAT DBE Past Present Future Alan Langman 28 September 2009.
ASKAP Capabilities John Reynolds on behalf of the SEIC and ASKAP team.
Jason Manley, Aaron Parsons, Don Backer, Henry Chen, Terry Filiba, David MacMahon, Peter McMahon, Arash Parsa, Andrew Siemion, Dan Werthimer, Mel Wright.
Development of FFTS for Radio Astronomy Sheng Li, Zhen-Hui Lin, Ji Yang Wen-Ying Duan, Qi-Jun Yao, Sheng-Cai Shi Purple Mountain Observatory, Chinese Academy.
AAVS processing: Uniboard implementation. UNIBOARD Jive led FP7 project UniBoard, high integration density >> processing / m3
RFI Mitigation at Westerbork: algorithms, test observations, system implementation Willem Baan, Peter Fridman & Rob Millenaar.
Australian SKA Pathfinder (ASKAP) David R DeBoer ATNF Assistant Director ASKAP Theme Leader 06 November 2007.
ASKAP Update David DeBoer ASKAP Project Director 26 May 2010.
Omnisys There are a few different activities at Omnisys that may be of your interests. –New correlation spectrometer IC’s. –New FFT spectrometers –Future.
Philippe Picard1EMBRACE station processing SKADS Conference, Limelette, 4-6 November 2009 EMBRACE station processing P. Picard Station de Radioastronomie.
Philippe Picard 2 nd SKADS Workshop October 2007 Station Processing Philippe Picard Observatoire de Paris Meudon, 11th October 2007.
ATCA GPU Correlator Strawman Design ASTRONOMY AND SPACE SCIENCE Chris Phillips | LBA Lead Scientist 17 November 2015.
The UniBoard a RadioNet FP7 Joint Research Activity Arpad Szomoru, JIVE.
SAGE meeting Socorro, May 22-23, 2007 WIDAR Correlator Overview Michael P. Rupen Project Scientist for WIDAR & Software.
FP7 Uniboard project Digital Receiver G. Comoretto, A. Russo, G. Tuccari, A Baudry, P. Camino, B. Quertier Dwingeloo, February 27, 2009.
Netherlands Institute for Radio Astronomy 1 ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) Board Design Gijs Schoonderbeek.
Netherlands Institute for Radio Astronomy 1 ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) Square Kilometer Array Low Central.
Calculating Beam Pattern Inaccuracies and Their Implications
JIVE UniBoard Correlator External Review
Backprojection Project Update January 2002
ASKAP High Time Res Capabilities
RadioNet FP7 Joint Research Activity
The UniBoard Generic Hardware for Radio Astronomy Signal Processing
Signal Processing for Aperture Arrays
Modern Interferometric Arrays
JIVE UniBoard Correlator (JUC) Firmware
UniBoard2 applied in the Square Kilometer Array
Pulsar Timing with ASKAP Simon Johnston ATNF, CSIRO
John Bunton Casper Workshop, Cape Town 28 September – 2 October, 2009
5 Gsps ADC Developement and Future Collaboration
Aperture Array Station Processing
The Uniboard  FPGA Processing for Astronomy
Realizing an universal digital processing platform
Presentation transcript:

Netherlands Institute for Radio Astronomy 1 APERTIF beamformer and correlator requirements Laurens Bakker

2 APERTIF system  Focal Plane Arrays for 12 of 14 Westerbork 25 m dishes  7*8 (or 8*9) dual polarized Vivaldi arrays  25 beams, 300 MHz bandwidth, full Stokes  Aeff/Tsys > 100 m 2 /K (N tel =14  a =0.75 T sys =50 K)  Frequency range: 1000 – 1750 MHz Current system architecture

3 Beamformer requirements  56 or 72 dual polarization elements per telescope  Polarizations can be treated independently in beamformer  ADC sampling speed 800MHz, 8 bit  LVDS connection between ADC and Uniboard required  Synchronization between all elements required  16 ADCs (or more) per Uniboard  Subbands <1MHz required  25 beams per polarization, all elements of 1 polarization used for all beams of this polarization (for now)  Weights don’t have to be updated very often ( in principle only once during 12 hour measurement)

4 Determining weights  Full covariance matrix for every subband required  Both on and off source  Not required at the same time as the beamformer, is a separate measurement  Not required to be determined for every subband at the same time  Only required once for every beam that needs to be made for a 12 hours measurement

5 Beamformer processing requirements Assume 4 Uniboards for 1 polarization of 1 telescope(64 elements):  Filterbank: 64*400MHz*(2*16+2*9)=1280GMAC/s  Beamformer:64*25*300MHz*4=1920GMAC/s  Total:3200GMAC/s  Per Uniboard: 800GMAC/s ->~100GMAC/s FPGA  Memory requirements: limited, only for FFT coefficients and beamforming weights  Interconnect between these boards required  120Gb/s output datarate (240Gb/s for both polarizations)  to correlator, max 2km distance  Total beamforming processing all telescopes:3200*12*2=76800GMAC/s

6 Correlator requirements (preliminary) Requirements as a whole  Full stokes -> both polarizations needed in correlator  Total input data rate 2880Gbps (12 telescopes, 240Gbps each)  Visibilities (25*24*(24+1))/2=7500  Number of input subbands: 384, MHz/subband  X-subband width: 6.1kHz (X-subbands:128)  Total nof X-subbands:  Integration time: 1-10s  Output data rate: 1-10Gb/s  24*25*300MHz*(4*8+2*8)+4*7500*300MHz=17640GMAC/s  Correlator can be treated as many independent correlators

7 APERTIF timeline  2010Q1:  operational Uniboard with 4 receivers (800MHz, 8bit), fft and beamformer on 4 elements implemented  2010Q4:  4 Uniboards in a backplane structure, 64 receivers and fft and full beamformer across all elements implemented