Mileura Widefield Array – Low Frequency Demonstrator 80 - 300 MHz * Currently in “Early Deployment” phase Goal: HI at redshift 6 to 17.

Slides:

Advertisements

Similar presentations

SKA New Technology Demonstrator Ray Norris CSIRO Australia Telescope National Facility.

Advertisements

SKAMP Square Kilometre Array Molonglo Prototype. Supporting Institutions  University of Sydney  Argus Technologies  ATNF  ICT Centre.

FPGA Programming for Real Time Analysis of Lidar Systems

David Hawkins Exascale Signal Processing for Millimeter-Wavelength Radio Interferometers David Hawkins

NMR Spectroscopy Tuning / Matching Shimming and Lock.

MWA Bangalore Meeting EoR using Drift Scan Strategy N. Udaya Shankar 8-December-2009.

RFI shielding and mitigation techniques for a sensitive search for the 327 MHz line of Deuterium Alan E.E. Rogers, Joseph C. Carter, Preethi Pratap M.I.T.

SKAMP - the Molonglo SKA Demonstrator M.J. Kesteven CSIRO ATNF, T. J. Adams, D. Campbell-Wilson, A.J. Green E.M. Sadler University of Sydney, J.D. Bunton,

2 Jul 2002 ASA-SKAMP 1 The Square Kilometre Array Molonglo Prototype (SKAMP) Molonglo AUSTRALIA Brisbane Darwin Perth Canberra Hobart Adelaide Melbourne.

SKAMP - the Molonglo SKA Demonstrator M.J. Kesteven CSIRO ATNF, T. J. Adams, D. Campbell-Wilson, A.J. Green E.M. Sadler University of Sydney, J.D. Bunton,

Sascha D-PAD Sparse Aperture Array.

Prototype SKA Technologies at Molonglo: 3. Beamformer and Correlator J.D. Bunton Telecommunications and Industrial Physics, CSIRO. Australia. Correlator.

Cylindrical Reflector SKA Update

MWA Project:. Site: Murchison Radio Observatory Australia’s proposed SKA Site Strategy: 512 Antenna “Tiles” Explore “Large N / Small D” regime Correlate.

The Murchison Widefield Array: an SKA Precursor Shep Doeleman - MIT Haystack For the MWA Project.

Signal Processing for Aperture Arrays. AAVS1 256 antenna elements distributed over –4 stations –64 elements each.

Dec 2010 AAVP Cambridge workshop AAVP AAVS1/2-low demonstrators Jan Geralt Bij de Vaate.

July 2001SKA Technologies at Molonglo1 Prototype SKA technologies at Molonglo – 1. Overview & Science Goals Joint project between the University of Sydney,

3 Oct 2001 Adelaide SKA Symposium-Prototyping SKA Technologies at Molonglo 1 Prototyping SKA Technologies at Molonglo Molonglo AUSTRALIA Brisbane Darwin.

What’s Going on in Canada?

AA-mid demonstrator Dion Kant AAVP – 10 December 2010, Cambridge, UK.

Low frequency sky surveys with the Murchison Widefield Array (MWA) Gianni Bernardi Harvard-Smithsonian Center for Astrophysics SKA SA project/MeerKAT observatory.

ASKAP Early Science Workshop Lisa Harvey-Smith & Aidan Hotan | ASKAP Project Scientists August 5 th 2013 ASTRONONY & SPACE SCIENCE.

Sarah Middleton Supervised by: Anton van Wyk, Jacques Cilliers, Pascale Jardin and Florence Nadal 3 December 2010.

Current LBA Developments Chris Phillips CSIRO ATNF 13/7/2005.

Backend electronics for radioastronomy G. Comoretto.

“First Light” From New Probes of the Dark Ages and Reionization Judd D. Bowman (Caltech) Hubble Fellows Symposium 2008.

Wireless PHY: Modulation and Demodulation Y. Richard Yang 09/6/2012.

The Murchison Wide Field Array Murchison, ~300 km from Geraldton.

Scanning Digital Radar Receiver Ryan Hamor Advisor: Dr. Huggins Bradley University ECE Department 5/02/2006.

Andreas Horneffer for the LOPES Collaboration Detecting Radio Pulses from Air Showers with LOPES.

Which dipoles to use to optimize survey speed? –What tapering? –Trade-off between sensitivity, FOV and low side-lobe levels –Station beam stability, pointing.

XNTD/SKAMP/LFD Correlator 4th RadioNet Engineering Forum Workshop Next Generation Correlators for Radio Astronomy and Geodesy June 2006, Groningen,

Correlator Growth Path EVLA Advisory Committee Meeting, March 19-20, 2009 Michael P. Rupen Project Scientist for WIDAR.

Next Generation Digital Back-ends at the GMRT Yashwant Gupta Yashwant Gupta National Centre for Radio Astrophysics Pune India CASPER meeting Cambridge.

Casper 2010Marc Torres Part 2: Building blocks for the next generation.

THE MURCHISON WIDEFIELD ARRAY: FROM COMMISSIONING TO OBSERVING D. Oberoi 1,2, I. H. Cairns 3, L. D. Matthews 2 and L. Benkevitch 2 on behalf of the MWA.

© ASTRON On the Fly LOFAR Station Correlator André W. Gunst.

Australian Astronomy MNRF Development of Monolithic Microwave Integrated Circuits (MMIC) ATCA Broadband Backend (CABB)

ASKAP Capabilities John Reynolds on behalf of the SEIC and ASKAP team.

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.

The Mission  Explore the Dark Ages through the neutral hydrogen distribution  Constrain the populations of the first stars and first black holes.  Measure.

ASKAP Update David DeBoer ASKAP Project Director 26 May 2010.

Potential of a Low Frequency Array (LOFAR) for Ionospheric and Solar Observations ABSTRACT: The Low Frequency Array (LOFAR) is a proposed large radio telescope.

The Allen Telescope Array Douglas Bock Radio Astronomy Laboratory University of California, Berkeley Socorro, August 23, 2001.

Review of developments in Australasia and mainland Asia Steven Tingay Swinburne University of Technology Next Generation correlator meeting, JIVE 27 -

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.

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.

First Exploration of MWA Deep Field Point Source Population C. Williams - PhD Thesis J. Hewitt – reporting some analysis.

Observing Cosmic Dawn with the LWA-1 PIs: Judd Bowman (ASU), Greg Taylor (UNM) Jake Hartman (JPL) Jayce Dowell, Joe Craig (UNM) Steve Ellingson (Virginia.

Prototype SKA Technologies at Molonglo: 1. Overview and Science Goals A.J. Green 1, J.D. Bunton 2, D. Campbell-Wilson 1, L.E. Cram 1, R.G. Davison 1, R.W.

Single Dish Summer School, Green Bank 2007 Things to do with Single Dish: VLBI Tapasi Ghosh NAIC/Arecibo Observatory Outline: Interferometry Basic.

Upcoming Instruments to Probe Reionization… Frank Briggs ANU.

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

IPS Observations Using the Big Scanning Array of the Lebedev Physical Institute: Recent Results and Future Prospects I.V.Chashei, V.I.Shishov, S.A.Tyul’bashev,

Andrew Faulkner April 2016 STFC Industry Day: Low Frequency Aperture Array Andrew Faulkner Project Engineer.

Developing a Sonar Sub-System for a Submarine to Obtain Time Delays between Received Signals Gary Eades Dy Eang Diana Fuertes 12/04/2007 ECE4884 L03 Dr.

Multi-beaming & Wide Field Surveys

EVLA Availability - or - When Can I Use It?

PCM (Pulse Code Modulation)

HERA Imaging and Closure

A Software Defined Radio for the Masses, Part 4

Technical Foundations & Enabling Technologies – DS4

Correlator Growth Path

On the ground and “On the Air” in Mileura Goal: HI at redshift 6 to 17

EVLA Advisory Panel Mtg. System Overview

SKAMP Square Kilometre Array Molonglo Prototype

Presentation transcript:

Mileura Widefield Array – Low Frequency Demonstrator MHz * Currently in “Early Deployment” phase Goal: HI at redshift 6 to 17

Tile 1

Ultimately…. 500 Tiles… 500 Tiles Layout in field instantaneous UV coverage Distance [km] 1 km

Beamformer

16 dual-pol dipoles MHz 200m coax IF Converter A/D 16Msampl/sec MHz Linux box+VSIB +TByte RAID +software processing LVDS Current Signal Path (Early Deployment) “Tile” … for each tile… Tile 2 Tile 3

Beamformer 16 dual-pol dipoles MHz 200m coax IF Converter A/D 16Msampl/sec MHz Linux box+VSIB +TByte RAID +software processing LVDS Current Signal Path (Early Deployment) “Tile” … for each tile… Tile 2 Tile 3

Beamformer 16 dual-pol dipoles MHz 200m coax IF Converter A/D 16Msampl/sec MHz Linux box+VSIB +TByte RAID +software processing LVDS Current Signal Path (Early Deployment) “Tile” … for each tile… Tile 2 Tile 3

Eric’s IF Converter 0-300MHz in 26-30MHz out 10 MHz4 MHz

Beamformer 16 dual-pol dipoles MHz 200m coax IF Converter A/D 16Msampl/sec MHz Linux box+VSIB +TByte RAID +software processing LVDS Current Signal Path (Early Deployment) “Tile” … for each tile… Tile 2 Tile 3

Analog MHz in 8bit digital out Portable Toolkit for Radio Expts software suite

Beamformer 16 dual-pol dipoles MHz 200m coax IF Converter A/D 16Msampl/sec MHz Linux box+VSIB +TByte RAID +software processing LVDS Current Signal Path (Early Deployment) “Tile” … for each tile… Tile 2 Tile 3

Verification of electronic Beam Steering

Observation of Sun: natural 100 MHz

Phases are well behaved for all declinations

Fornax A

Power relative to Sky [dB] Sample deep Spectra - 1kHz resolution 1/2 hr 1 hr

ED1 - Complete Spectral Scan - 250,000 channels

Beamformer 16 dual-pol dipoles MHz 200m coax IF Converter A/D 16Msampl/sec MHz Linux box+VSIB +TByte RAID +software processing LVDS Current Signal Path (Early Deployment) “Tile” … for each tile… Tile 2 Tile 3

Group 16 tiles into “NODE” Next Generation Signal Path Beamformer Node Electronics 16 x 2 pol inputs MHz Correlator < 1 km fibre

Node serves 16 tiles: Next Generation Signal Path Beamformer Node Electronics 16 x 2 pol inputs MHz Correlator < 1 km fibre 6bit A/D PP Filter select 32 MHz 8 KHz Channels …………