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THE FUTURE OF RADAR ASTRONOMY

THE FUTURE OF RADAR ASTRONOMY. DON CAMPBELL. Planetary Radar Sensitivity vs Date. 40. Second upgrade and 1.0 MW transmitter. Primary surface reset. 30. First upgrade and 420 kW S-band transmitter. Relative Sensitivity db. 20. New “Love” 430 MHz line feed. 10. First observations. 1964.

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THE FUTURE OF RADAR ASTRONOMY

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  1. THE FUTURE OF RADAR ASTRONOMY DON CAMPBELL

  2. Planetary Radar Sensitivity vs Date 40 Second upgrade and 1.0 MW transmitter Primary surface reset 30 First upgrade and 420 kW S-band transmitter Relative Sensitivity db 20 New “Love” 430 MHz line feed 10 First observations 1964 1974 1984 1994 2004 Date

  3. A X-band Planetary Radar? Where is the next increment in planetary radar sensitivity to come from? • At Arecibo by increasing the frequency (i.e. the antenna gain) • Wait for the SKA? The Canadian Large Adaptive Reflector? • Other?

  4. Is sensitivity still the most important consideration?Resolution? Unambiguous imaging?All?

  5. Spectrum of the reflected echo – from CW observations

  6. Delay-Doppler imaging PLUS SHAPE MODELING for SMALL BODIES

  7. Radar synthesis imaging (plane of sky)

  8. What are likely to be the major scientific drivers in the field over the next 10 to 20 years? Small solar system bodies – asteroids and comets Astrometry – i.e. predicting future orbits Characterization – shapes, sizes, surface properties, ages, etc Dynamics – rotation states, binary configurations

  9. Planetary satellites: Lunar 3-D topographic measurements The icy satellites of the giant outer planets Imaging of the icy Galilean satellites and Titan (?) Reflection properties of the smaller icy satellites of Jupiter, Saturn and Uranus Reflection properties of Neptune’s moon Triton

  10. The Terrestrial Planets: Mercury will continue to be a target even after Messenger Specialized Venus studies – depends on maintaining S-band. Mars – not clear Rotation states of the terrestrial planets via interferometry Very important over next few years

  11. RADAR ASTRONOMY BASICS Normalized Backscatter Cross Section, the radar albedo Radar Equation: Transmitting Antenna Gain 4 At /2 Average Transmitter Power Target Area Integration time Distance Rotational Doppler Broadening  -1 Receive Antenna Collecting Area System Temperature

  12. S-Band C-Band X-Band SKA Wavelength(cm) 13 6 3.5 3.5? Gain (K/Jy) 11 10 8 Power (kW) 1000 1000 500 Sys Temp 20 20 20 Rel. Sensitivity 1.0 2.5 1.8 20 to 30 Best Range Res (m) 10 <10 5 5? EVLA Synth. Res. 2500 1200 700 at 0.04 AU (m) VLBA Synth Res 100 50 26 SKA Synth Res 300 150 75

  13. PLANETARY RADAR ASTRONOMYRecent Advances in Techniques NAIC • VLA Synthesis Imaging of Radar Illuminated Bodies – Terrestrial Planets, Satellites and Asteroids (Muhleman, Butler, de Pater, Grossman, Harcke) • Shape Modeling from Delay-Doppler Images of Near-Earth and Mainbelt Asteroids (Hudson, Ostro) • Coded Long Pulse Technique for Overspread Targets (Time Dispersion  Doppler Broadening > 1.0  Aliasing) (Harmon, Sulzer) • Altimetry from Interferometric Delay-Doppler Imaging (Recent work by Margot, Campbell, Jurgens, Slade) • Polarimetric Delay-Doppler Imaging (Stacy, Carter, Campbell) • VLBI Radar Synthesis Imaging of Near-Earth Asteroids (Black, Campbell, Zaitsev) • Radar Speckle Displacement Interferometry (Proposed by Holin)

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