Netherlands Institute for Radio Astronomy 1 ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) From LOFAR design to SKA1 System.

Slides:



Advertisements
Similar presentations
Wind turbines and LOFAR
Advertisements

SKA New Technology Demonstrator Ray Norris CSIRO Australia Telescope National Facility.
SKADSMTAvA A. van Ardenne SKADS Coördinator ASTRON, P.O. Box 2, 7990 AA Dwingeloo The Netherlands SKADS; The.
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 – 2b – CMV 2009/10/09 Basic Detection Techniques 2b (2009/10/09): Focal Plane Arrays Case study: WSRT System overview Receiver and.
Prototype SKA Technologies at Molonglo: 2. Antenna and Front End G.B. Warr 1,2, J.D. Bunton 3, D. Campbell-Wilson 1, R.G. Davison 1, R.W. Hunstead 1, D.A.
Prototype SKA Technologies at Molonglo: 3. Beamformer and Correlator J.D. Bunton Telecommunications and Industrial Physics, CSIRO. Australia. Correlator.
Cylindrical Reflector SKA Update
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.
ATA Antennas Feeds and Systems NSF Review 8/05/08 Jack Welch.
Performance of station array configurations Sparse vs. Dense, Regular vs Random Jaap D. Bregman AAVP Workshop,Cambridge,
Dec 2010 AAVP Cambridge workshop AAVP AAVS1/2-low demonstrators Jan Geralt Bij de Vaate.
Keith Grainge Calibration requirementsAAVP 2010 Calibration and Imaging Requirements Keith Grainge (plus teams at ASTRON, Oxford, Cambridge)
AA-mid demonstrator Dion Kant AAVP – 10 December 2010, Cambridge, UK.
LOFAR Antenna Systems Dion Kant, Wim van Cappellen 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.
Solar dynamic spectra C. Vocks and G. Mann 1. Spectrum of the quiet Sun: First results 2. How to obtain spectra: Beamformed data 3. Single station spectra.
Assessment of RFI measurements for LOFAR Mark Bentum, Albert-Jan Boonstra, Rob Millenaar ASTRON, The Netherlands Telecommunication Engineering, University.
J.M. Wrobel - 25 June 2002 PROPOSALS 1 PROPOSAL WRITING TUTORIAL Outline 30 minutes: Lecture on Generic Issues 60 minutes: Small Groups Write Proposals.
AA-Low Technical Progress Meeting, October 2012, Medicina, Italy AAVS0 & AAVS0.5: System Design and Test Plan Nima Razavi-Ghods Eloy de Lera Acedo.
EMBRACE Local Oscillator distributor EMBRACE (Electronic Multi-Beam Radio Astronomy ConcEpt) has been planned as about 300 square meters aperture array.
Solar observation modes: Commissioning and operational C. Vocks and G. Mann 1. Spectrometer and imaging modes 2. Commissioning proposals 3. Operational.
Phased Array Feeds John O’Sullivan SKANZ 2012 CSIRO Astronomy and Space Science,
November 2009, Lunch talk The most compact E configuration for the EVLA. L. Kogan, G. Stanzione, J. Ott, F. Owen National Radio Astronomy Observatory Socorro,
Analysis of Low Frequency Phased Array Stations Dr. Nima Razavi-Ghods Dr. Eloy de Lera Acedo Cambridge AAVP 2010, 09/12/10 1.
Array Configuration Divya Oberoi MIT Haystack Observatory.
Rosie Bolton1 SKADS Costing work 4 th SKADS Workshop, Lisbon, 2-3 October 2008 SKADS Costing work: Spreadsheets to scalable designs Rosie Bolton Dominic.
Which dipoles to use to optimize survey speed? –What tapering? –Trade-off between sensitivity, FOV and low side-lobe levels –Station beam stability, pointing.
Paul Alexander & Jaap BregmanProcessing challenge SKADS Wide-field workshop SKA Data Flow and Processing – a key SKA design driver Paul Alexander and Jaap.
Netherlands Institute for Radio Astronomy 1 ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) LOFAR Operations and Schedule.
Rosie Bolton SKADS Workshop April 10th 2008 SKADS Costing work: beyond the benchmark scenario Rosie Bolton Paul Alexander, Andy Faulkner and SKADS Costing.
© ASTRON On the Fly LOFAR Station Correlator André W. Gunst.
FLOW the french LOFAR consortium P. Zarka, M. Tagger + ~30 participants.
Andrew Faulkner 2 nd SKADS Workshop October 2007 SKADS Benchmark Scenario Andrew Faulkner.
MeerKAT DBE Past Present Future Alan Langman 28 September 2009.
Type III radio bursts observed with LOFAR and Nançay radioheliograph Jasmina Magdalenić 1, C. Marqué 1, A. Kerdraon 2, G. Mann 3, F. Breitling 3, C. Vocks.
ASKAP Capabilities John Reynolds on behalf of the SEIC and ASKAP team.
MAG->RCV 2007/09/26 Edinburgh LOFAR Status Internal review of the project (April-July 2007): Main conclusions: R&D developments in good shape (CS1 results)
LOFAR The Low Frequency Array Shep Doeleman LOFAR Group.
Centre of Excellence for All-sky Astrophysics MWA Project: Centre of Excellence for All-sky Astrophysics Centre of Excellence for All-sky.
Murchison Widefield Array (MWA) : Design and Status Divya Oberoi, Lenoid Benkevitch MIT Haystack Observatory doberoi, On behalf.
Answers from the Working Group on AGN and jets G. Moellenbrock, J. Romney, H. Schmitt, V. Altunin, J. Anderson, K. Kellermann, D. Jones, J. Machalski,
AAVS processing: Uniboard implementation. UNIBOARD Jive led FP7 project UniBoard, high integration density >> processing / m3
The Allen Telescope Array Douglas Bock Radio Astronomy Laboratory University of California, Berkeley Socorro, August 23, 2001.
A real-time software backend for the GMRT : towards hybrid backends CASPER meeting Capetown 30th September 2009 Collaborators : Jayanta Roy (NCRA) Yashwant.
EURO-VO: GRID and VO Lofar Information System Design OmegaCEN Kapteyn Institute TARGET- Computing Center University Groningen Garching, 10 April 2008 Lofar.
The SKA: Next Week, the Next 3 Years & Beyond Jim Cordes, Cornell University 24 August 01  Concepts  Science Goals & Payoffs  Configurations, Modes.
Philippe Picard 2 nd SKADS Workshop October 2007 Station Processing Philippe Picard Observatoire de Paris Meudon, 11th October 2007.
A System View on SKA Bandwidth Usage G.W. (Dion) Kant AAVP Dwingeloo, 14 December 2011.
Rosie Bolton 2 nd SKADS Workshop October 2007 SKADS System Design and Costing: Update and next steps Rosie Bolton University of Cambridge.
SKA1-LOW CONFIGURATION CONSULTATION WS P. Dewdney
EoR/Cosmic Dawn SWG Feedback on SKA1-Low Array Configuration Cath Trott Brad Greig, Leon Koopmans, Andrei Mesinger, Garrelt Mellema, Jonathan Pritchard.
Engineering Commissioning May 2016 SKA1 LOW – Assembly, Integration & Verification Adam MacLeod AIV Consortium Manager & ASKAP System Engineer.
Netherlands Institute for Radio Astronomy 1 APERTIF beamformer and correlator requirements Laurens Bakker.
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
Multi-beaming & Wide Field Surveys
Solar and heliosheric WG
The Low Frequency Array (LOFAR)
Mid Frequency Aperture Arrays
Phased Array Feeds SKANZ 2012 John O’Sullivan
Signal Processing for Aperture Arrays
Phased Array Feeds Wim van Cappellen
EGEE NA4 Lofar Lofar Information System Design OmegaCEN
UniBoard2 applied in the Square Kilometer Array
Pulsar Timing with ASKAP Simon Johnston ATNF, CSIRO
LOFAR Beam Formed (BF) Data & Pipeline Overview September 9, 2010
Aperture Array Station Processing
Radio Observatory Report
Presentation transcript:

Netherlands Institute for Radio Astronomy 1 ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) From LOFAR design to SKA1 System André Gunst

2 Conclusions  System Engineering Process Crucial for the SKA  Non-astronomical requirements are even (more) important  Twice the number of LBAs are used to cover 1.5 octave freq. range  HBA hierarchical beamforming used to invest more in “area”

3 Reflection  Questions, questions, questions …  Should be structured and prioritized in the risk register  Then they should be assigned and mitigated (or not)  Without we will not answer the right questions in time

4 LOFAR Documentation Plan

5 Not only astro req.’s

6 SKA Requirements

7 Potsdam Juelich Tautenburg Garching Effelsberg Nancay Chilbolton Onsala Jena

8 Number and Size of Stations  Total required sensitivity  Minimum size required for station calibration  Instantaneous imaging capability (snapshots)  UV coverage in synthesis mode  System costs  Station electronics: ~ antennas * stations  Network electronics: ~ stations  Correlator: ~ stations 2 * beams  Post processing: ~ stations 2 * beams * (B max /D s )*N ch  Cost efficient to make FOV with multiple beams and smaller amount of stations

9 LOFAR station MHz MHz Optional 10- … MHz

10 Station “Backend” Electronics  Shared in LOFAR over multiple arrays  LBA optimized for MHz (original target MHz)  Possibility for two configurations  HBA optimized for MHz  “LBL” usable from MHz

11 Central Systems  Shared in LOFAR as well over the multiple arrays  Can only observe one array at the same time  For SKA thought should be given as well to share central systems for all AA arrays and the dishes

12 HBA Hierarchical Beamforming

13 HBA Mechanical Started with “eye catching spiders”

14 HBA Mechanical Ended with “boring boxes”

15 How Could That Happen …  Because  Needs a 15 year lifetime  Needs to withstand storm, snow, sun load  Needs to be assembled in the field efficiently  Needs to have “zero cost”  Industry was involved  All non-astronomical requirements

16 HBA Assembly

17 Station Subrack

18 What if: the money is really limited …  Money shortage leads to creativity

19 Creative Changes  Dutch stations half as large  Two LBA fields in Dutch stations (low cost penalty):  LBA outer array  LBA inner array  Enabled by extra analog input in receiver  HBA field of Core Stations split  UV coverage improved  Station calibration “deproved”  Enabled by scalability of station hardware  Number of output bits  16, 8 or 4 bit  Exchange between bits for beams  Enabled by usage of FPGAs

20 International Stations (≥ 8)

21 Remote Stations (16)

22 Core Stations (24)

23 Nancay Super Station  Add an extra low band antenna array to the LOFAR station  Uses the “third” receiver input  96 mini arrays  Each array consists of ~ 10 antenna elements  Optimized for < 30 MHz region

24 What SKA can use …  AA low bandwidth: MHz (2.5 octave)  One antenna type or two?  Depends on  Sensitivity profile over frequency  Technology + cost  Possibility as well to share backend electronics  Keep doing system engineering  Freeze requirements at System Requirements Review (latest)  Everyone benefits: gives focus and clarity  Track changes in requirements and analyze impact  Changes can ripple through all layers of the system  Change = money and sensitivity ~ money!

25 Conclusions  System Engineering Process Crucial for the SKA  Non-astronomical requirements are even (more) important  Twice the number of LBAs are used to cover 1.5 octave freq. range  HBA hierarchical beamforming used to invest more in “area”

26 The End