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 tex2html_wrap_inline12 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 tex2html_wrap_inline12 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 tex2html_wrap_inline12 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 tex2html_wrap_inline18 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 .