Thermal Emission Spectrometer (TES)

Objectives:

1. Determine and Map the Composition of Surface Minerals, Rocks and Ices
2. Study the Composition, Particle Size and Spatial and Temporal Distribution of Atmospheric Dust
3. Locate Water-Ice and Carbon Dioxide Condensate Clouds and Determine Their Temperature, Height and Condensate Abundance
4. Study the Growth, Retreat and Total Energy Balance of the Polar Cap Deposits
5. Measure the Thermophysical Properties of the Martian Surface (Thermal Inertia, Albedo) Used to Derive Surface Particle Size and Rock Abundance
6. Determine Atmospheric Temperature, Pressure, Water Vapor and Ozone Profiles, and Seasonal Pressure Variations

Instrumentation:

Michelson Interferometer covering the spectral range 6.25 microns to 50 microns with 5 cm-1 and 10 cm-1 spectral resolution

Separate solar reflectance (0.2 microns to 3.9 microns) and broad band radiance (0.3 microns to 100 microns) channels.

Measurements:

• Michelson Interferometer Plus Two Broadband Radiometric Channels Measure Surface Spectral Properties and Thermal Radiation Ranges
• Interferometer: 6.25 microns to 50 microns
• Radiometric: Solar Reflectance from 0.3 microns to 2.7 microns, Broadband Radiance from 4.5 microns to 100 microns
• Resolution:
  • Spectral: 5 cm-1 and 10 cm-1 (Interferometer)
  • Spatial: 3 km/pixel at Nadir
• Detectors:
  • 3 sets of 2X3 Pyroelectric Arrays (8.3 mrad Pixel size)
  • FOV: 24.9 X 16.6 mrad
  • View Direction: Deep Space and Aft-Limb Track through Nadir to Forward Limb
• Electronics:
  • 80C86 Microprocessor
  • TI Digital Signal Processor (FFT)
  • 0.6 Mbyte RAM for Operatic Program Plus Buffering
  • Data Rates: 688, 1664, 4992 (real-time) bits/sec
  • Commands: ~ 300 words/day as Multiple 16 bit Words

Science Team

P. Christensen, ASU - Principal Investigator

Co-Investigators:

D. Anderson - ASU

S. Chase - Consultant

R. Clark - USGS

H. Kieffer - USGS

M. Malin - MSSS

J. Pearl - NASA/GSFC