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Centre of Excellence for All-sky Astrophysics caastro

Centre of Excellence for All-sky Astrophysics www.caastro.org. Centre of Excellence for All-sky Astrophysics www.caastro.org. MWA Project:. MWA Consortium : CurtinU, ANU, UMelbourne, SwinburneU, USydney, UWestern Australia, UTasmania, MIT, Harvard-Smithsonian CfA, ASU, UW,

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Centre of Excellence for All-sky Astrophysics caastro

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  1. Centre of Excellence for All-sky Astrophysicswww.caastro.org Centre of Excellence for All-sky Astrophysicswww.caastro.org MWA Project: MWA Consortium: CurtinU, ANU, UMelbourne, SwinburneU, USydney, UWestern Australia, UTasmania, MIT, Harvard-Smithsonian CfA, ASU, UW, Raman Research Institute, CSIRO

  2. MWA Project:

  3. MWA: Science Goal: EoR Hydrogen 21cm line @ Z=6-13 80 - 230 MHz … to 320 MHz Statistical Detection through Power Spectrum: angular scales 4’ to 30’

  4. MWA: Science Goal: EoR Hydrogen 21cm line @ Z=6-13 80 - 230 MHz … to 320 MHz • Instrument Strategy: • Geographic Location • Large N / Small D (512/5m) • Compact Array • “Real-time System” Gianni!

  5. Location ofMWA Australia’s SKA site (infrastructure, etc)

  6. The Shire of Murchison is a large agricultural region in the central part of Western Australia, and is the only shire in Australia without a town. Population: 114 (2009) Area: 41173 km² (15,897.0 sq mi) ~ Netherlands • Strategy: • less RFI • lower power levels • fewer bits • lower bandwidths • less complexity • lower cost

  7. Small D ~ 5m Chris Williams (for scale)

  8. Small D => Large Field of View Hydra A 115 MHz 50 deg between nulls HPBW ~ 30 deg

  9. Small D => Large Field of View Virgo A 3C273 Jan 2010

  10. Aerial Photo of “Small N” = 32 Tile Prototype Array:

  11. Locations of Antenna Tiles in 32T Array West-East [m]

  12. Layout of Large N = 512 Tile Array (128 intermediate) COMPACT * Densely populated core for Surface Brightness sensitivity (!!!!!) * Ionospheric wobble treated as rubber sheet sky • Strategy: • less complexity • lower cost 1.5 km

  13. Correlator: • FPGA based “hardware correlator” • and fine Filter Bank (10KHz channels) • Correlate all pairs => 130,816 Interferometer Baselines • (Prototyping & Testing … baseband recorders, software filter banks, • correlators, and beamformers, …)

  14. Hydra A 115 Mhz Jan 2010

  15. Hydra A 121 Mhz Chris Williams Sep 2010

  16. Pictor A Parkes Catalog

  17. Pictor A Parkes Catalog MWA Sources

  18. ~10 x 2min over wide HA range 21 57 05.8 -69 41 22 UV coverage 32T Image 114 MHz

  19. Centaurus A

  20. Centaurus A

  21. CenA Left: MWA contours on ACTA+PKS image Right: MWA 115MHz image

  22. The Sun with MWAComparison with X-ray observations

  23. Solar Radio Bursts 170-200 MHz Oberoi, Matthews, et al

  24. Oberoi, Matthews, et al Grid of Radio Spectra across the face of the Sun

  25. Instantaneous 32T uv-coverage Oberoi, Matthews, et al

  26. Ord, Mitchell & Greenhill “2PiP” baseband recording system Vela Pulsar

  27. Ord, Mitchell & Greenhill “2PiP” baseband recording system

  28. Chris Williams, MIT MWA EoR Target Fields

  29. MWA Future August 2011 - lay in the infrastructure December 2011 - lay tiles - populate CSIRO facility bldg (with correlator/RTS hardware) February 2012 - place receivers June 2012 - 128T hardware installed - commissioning phase

  30. Experiment: Tb = Tb(moon) - Tb(sky) BB spectrum: smooth & known Not Smooth !? Tb Tb Contrast between Tb(Moon) and Tb(Sky) Tb(Sky) Non-thermal + EoR,etc Tb(Moon) Thermal ~B.B.

  31. Recent Data Sets… LOFAR … several long observations at Full Moon Nov, Dec, Jan, …(?) MWA… few hours near Full Moon, Sept.

  32. Moon Field - 83 MHz Ben McKinley, ANU

  33. Moon Field - 156 MHz

  34. Moon Field - 105 MHz Day 1

  35. Moon Field - 105 MHz Day 2

  36. Tb = Tb(moon) - Tb(sky) 80 100 120 140 160 MHz

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