Spectro-Cam 10 observations of Mars at low (R=100) and high (R=2000) resolution during the 1997 Apparition.
D.L. Blaney (JPL)
The infrared spectrum of Mars between 8-14 
m is a complex
nonlinear function of thermal emission from the surface,
absorption features by atmospheric dust, and absorption by
atmospheric gases. Data was collected at the 200" Hale
telescope at Palomar Mountain Ca, using Spectro-Cam 10 in
both high and low spectral resolution modes on April 19, 1997
and May 15, 1997. Low resolution observations covered the
entire 8-13 m range to measure dust opacity, surface
temperature, and broad mineral absorption features.
Pollack et al. (1990) showed that when limb and center of the disk
spectra were ratioed, mineralogic absorption features were
detected at 8.7 and 9.8 m that were attributable to sulfates or
bisulfates. Observations were made centered around the 8.7
sulfate feature at high spectral resolution (R=2000) using five
grating positions to try and define the spectral shape of this
feature.
Data is currently undergoing reduction and analysis
to be presented in Boston. Signal to noise of both the high
and low resolution data set are good. Initial reduction of the
low resolution data show the classical broad silicate dust
absorption feature, as well as 
gas absorption. Low and
high resolution spectra for specific locations on Mars will be
presented.
Thanks go to Tom Hayward (Cornell) and Martha Hanner, Padama Yamadra-Fisher, and Terry Martin (JPL) for their assistance in making these observations.
Pollack et al. , JGR, 95, 14,595-14,627, 1990.
This work performed at JPL/CALTECH under contract by
NASA .