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Brightness Temperature Distribution of the Moon

Brightness Temperature Distribution of the Moon. Jianfeng Zhou. Center for Astrophysics, Tsinghua University, China. Background BT observations from Change-1&2 Probes BT observations from Ground Based Arrays and Single-dish Telescopes Conclusions. Outline. Black Body Radiation.

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Brightness Temperature Distribution of the Moon

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  1. Brightness Temperature Distribution of the Moon Jianfeng Zhou Center for Astrophysics, Tsinghua University, China

  2. Background • BT observations from Change-1&2 Probes • BT observations from Ground Based Arrays and Single-dish Telescopes • Conclusions Outline

  3. Black Body Radiation Planck's law

  4. Brightness Temperature Bυ(T) = 2kTυ2/c2 Rayleigh-Jeans Law

  5. Brightness Temperature Radio spectrum for a 106 K plasma that is optically thick below about 10 GHz, and optically thin at higher frequencies.  The brightness below 10 GHz corresponds to a million degree blackbody.

  6. Moon at Different Bands Infrared Radio X-Ray Optical UV

  7. Radiation of the Moon

  8. Science Objectives of BT Observation

  9. Change-1&2 Probes • Stereo CCD Camera • Laser Altimeter • Microwave Radiometer • X-ray Gamma-ray Detectors • Imaging Interferometer in Visible and Near IR band

  10. Microwave antennas at 3.0GHz, 7.8GHz, 19.35GHz and 37GHz. Change-1&2 Probes For calibration. For observation . Wang et al., Science in China, 2009, Vol. 39, 1029

  11. Change-1&2 Probes BT Distributions at 3.0GHz from Change-1 Probe Wang et al., Science in China, 2009, Vol. 39, 1029

  12. Ground Based Observation

  13. Miyun 50m MiYun 50m S/X Observation

  14. Miyun 50m

  15. DRAO at L-Band :

  16. DRAO at L-Band :

  17. GMRT at L-Bands :

  18. GMRT L-Bands

  19. GMRT at L-Bands

  20. VLA at L-Bands

  21. VLA at L-Bands

  22. VLA at L-Band : Peak brightness temperature is 272.4K，64% , 32% and 16% contours correspond to 174.4K，87.2Kand 43.6K respectively。

  23. Multi-band and multi-epoch brightness temperature observations are essential for studying the physical and geometric properties of the regolith of the moon. • Ground based observations (array and single-dish) are important complementary to the Change-1&2’s data. • Preliminary results of the ground based observations are obtained, but need improvement. • Further multi-epoch observations are needed. Conculsions

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