Thermal Emission Spectrometer (TES)
Objectives:
- Determine and Map the Composition of Surface Minerals, Rocks
and Ices
- Study the Composition, Particle Size and Spatial and Temporal
Distribution of Atmospheric Dust
- Locate Water-Ice and Carbon Dioxide Condensate Clouds and
Determine Their Temperature, Height and Condensate Abundance
- Study the Growth, Retreat and Total Energy Balance of the
Polar Cap Deposits
- Measure the Thermophysical Properties of the Martian Surface
(Thermal Inertia, Albedo) Used to Derive Surface Particle Size and
Rock Abundance
- 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