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New Radio Telescopes

New Radio Telescopes. Geoff Bower. State of the Art. 27 antennas 25 m in diameter D_eff ~ 130m 400 cm to 0.7 cm wavelength 1- 35 km baselines Resolution: 9 arcmin to 40 milliarcsec. Very Large Array. State of the Art. 10 antennas 25 m in diameter 90 cm --- 0.7 cm

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New Radio Telescopes

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  1. New Radio Telescopes Geoff Bower The Transient Universe: AY 250 Spring 2007

  2. State of the Art • 27 antennas • 25 m in diameter • D_eff ~ 130m • 400 cm to 0.7 cm wavelength • 1- 35 km baselines • Resolution: 9 arcmin to 40 milliarcsec Very Large Array The Transient Universe: AY 250 Spring 2007

  3. State of the Art • 10 antennas • 25 m in diameter • 90 cm --- 0.7 cm • Baselines 100 km --- 8000 km • Resolution: 20 to 0.2 milliarcsec Very Long Baseline Array The Transient Universe: AY 250 Spring 2007

  4. Evolutionary Deadends The Transient Universe: AY 250 Spring 2007

  5. The Transient Universe: AY 250 Spring 2007

  6. The Transient Universe: AY 250 Spring 2007

  7. Key Characteristics of Next Generation Telescopes • Greater sensitivity • More complete image sampling • Broader wavelength coverage • Rapid survey speed • Multi-user capability Large N, Small Diameter LNSD The Transient Universe: AY 250 Spring 2007

  8. Cost Optimization Cost ~ D^2.7 6.1 m The Transient Universe: AY 250 Spring 2007

  9. The Radio Revolution MWA XNTD PAPER FASR PAST LAR LWA The Transient Universe: AY 250 Spring 2007

  10. Allen Telescope Array The Transient Universe: AY 250 Spring 2007

  11. The Transient Universe: AY 250 Spring 2007

  12. Allen Telescope Array • Large N design • 350 x 6.1m antennas • Sensitivity of the VLA • Unprecedented imaging capabilities • Continuous frequency coverage • 0.5 to 11.2 GHz • Wide field of view • 3.5 degrees at 1 GHz • Excellent survey instrument: 17x FOV of VLA • Compact Configuration • 1 arcmin at 1.4 GHz (350), 1 arcmin at 5 GHz (42) • Simultaneous observing with multiple backends • Correlator: 2 x 100 MHz x full Stokes x 1024 channels • Phased array beams: 32 indepent at 4 frequencies • Joint project of UC Berkeley/SETI Inst. • Privately funded construction • $26M from PGAF and others • NSF support for correlator & operations ($2.2M) • USNO support for construction ($3M) The Transient Universe: AY 250 Spring 2007

  13. ATA Log-Periodic Feed Treceiver~35 K TLNA~10 K Feed by Welch & Engargiola LNAs from Weinreb & Wadefalk The Transient Universe: AY 250 Spring 2007

  14. The Antenna • 6.1-m offset Gregorian • Low diffractive spillover ~1% at all elevations • Surface rms ~ 1mm • Works to 25 GHz The Transient Universe: AY 250 Spring 2007

  15. Antenna Configuration 1 km Sidelobes less than 1% The Transient Universe: AY 250 Spring 2007

  16. The Transient Universe: AY 250 Spring 2007

  17. ATA-42 Operational Soon 4 deg/sec in azimuth, 2 deg/sec in elevation The Transient Universe: AY 250 Spring 2007 Movie 3x real time

  18. Andromeda in a Single Pointing • 7 antennas • 2 nights The Transient Universe: AY 250 Spring 2007

  19. ATA Science • SETI • GC survey: 20 sq. deg, 1.4-1.7 GHz, 6 months • 106 stars over 1-10 GHz • Arecibo radar detectable at 300 pc • Simultaneous with correlator • Extragalactic HI survey • Neutral gas SDSS equivalent • L* at z=0.1 over the entire sky • Galactic magnetic fields, HI, long-chain molecules • Pulsars • Radio continuum science • All sky surveys • Transients (1 msec  1 year) Robishaw, Simon & Blitz 2002 LGS 3 The Transient Universe: AY 250 Spring 2007

  20. The EVLA • Upgrade of the VLA • Bandwidth • 100 MHz  8 GHz • Correlator • 256 channels  256k • Continuous frequency coverage • 1.0 to 50 GHz The Transient Universe: AY 250 Spring 2007

  21. EVLA Phase I - Key Science Examples • Measuring the three-dimensional structure of the Sun's magnetic field • Mapping the changing structure of the dynamic heliosphere • Measuring the rotation speed of asteroids • Observing ambipolar diffusion and thermal jet motions in young stellar objects • Measuring three-dimensional motions of ionized gas and stars in the center of the Galaxy • Mapping the magnetic fields in individual galaxy clusters • Conducting unbiased searches for redshifted atomic and molecular absorption • Looking through the enshrouding dust to image the formation of high-redshift galaxies • Disentangling starburst from black hole activity in the early universe • Providing direct size and expansion estimates for up to 100 gamma-ray bursts every year The Transient Universe: AY 250 Spring 2007

  22. EVLA continuum The Transient Universe: AY 250 Spring 2007

  23. Mileura Wide Field Array --- Low Frequency Demonstrator The Transient Universe: AY 250 Spring 2007

  24. Dipole Antennas The Transient Universe: AY 250 Spring 2007

  25. The Transient Universe: AY 250 Spring 2007

  26. The Transient Universe: AY 250 Spring 2007

  27. The Square Kilometer Array The Transient Universe: AY 250 Spring 2007

  28. LNSD Optimization Weinreb 2007 The Transient Universe: AY 250 Spring 2007

  29. Science Goals • The Cradle of Life • Strong field tests of gravity using pulsars and black holes • Origin and evolution of magnetism • Galaxy evolution and cosmoly • Dark energy The Transient Universe: AY 250 Spring 2007

  30. fundamental questions in physics and astronomy “What are the basic properties of the fundamental particles and forces?” Neutrinos, Magnetic Fields, Gravity, Gravitational Waves, Dark Energy “What constitutes the missing mass of the Universe?” Cold Dark Matter (e.g. via lensing), Dark Energy, Hot Dark Matter (neutrinos) “What is the origin of the Universe and the observed structure and how did it evolve?” Atomic hydrogen, epoch of reionization, magnetic fields, star-formation history…… “How do planetary systems form and evolve?” Movies of Planet Formation, Astrobiology, Radio flares from exo-planets…… “Has life existed elsewhere in the Universe, and does it exist elsewhere now?” SETI The Transient Universe: AY 250 Spring 2007

  31. Technical Specs • 1 km^2 collecting area • D_eff ~ 1000 m • Frequency coverage from 0.1 to 25 GHz • Baselines of 20 m to 3000 km • FOV >~ 1 sq deg • Goal of 200 sq deg at 0.7 GHz The Transient Universe: AY 250 Spring 2007

  32. The Transient Universe: AY 250 Spring 2007

  33. Reference Design Inner core Station Reference Design Wide-angle radio camera + radio “fish-eye lens” The Transient Universe: AY 250 Spring 2007

  34. 1% SKA Pathfinders -proving SKA technology • Radio camera: small dishes+smart feeds -SKA Design Study (Europe) -Karoo Array Telescope (South Africa) -Extended New Technology Demonstrator (Australia) -Allen Telescope Array (USA) • Radio fish-eye lens: aperture array tiles -SKA Design Study (Europe) -LOFAR (Netherlands) • SKADS – study of end-to-end design EC-FP6, European countries, Australia, South Africa, Canada The Transient Universe: AY 250 Spring 2007

  35. SKA 10^6 EVLA continuum The Transient Universe: AY 250 Spring 2007

  36. SKA timeline ‘1% SKA’ Science Inter-governmental discussions Initial concept ‘10% SKA’ Science First SKA Working Group ISSC MoAs Science Case published Site ranking Site Selection SKA Complete { { { { 92 96 0405 06 07 08 09 1014 18 22 { 2000 2000 { { Feasibility study Concept exposition Optimise Reference Design Define SKA System Phase 1 Build 10% SKA Full array Build 100% SKA Construct 1% SKA “pathfinders” The Transient Universe: AY 250 Spring 2007

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