Spectra as given in Fig.1 and Fig.4 from our paper
"Infrared stealthy surfaces: Why TES and THEMIS may miss substantial mineral deposits on Mars."

These spectra illustrate the effects of reduced spectral contrast and altered band shape that surface texture causes. Preprint .


Spectrum of a hematite-rich coating, and TES spectra.

This gives a spectrum of a hematite-rich coating on a ferricrete sample, and also TES spectra of Mars. These are in one of our LPSC 2002 abstracts (in Adobe PDF).


Spectra derived of Mars' surface using a unique atmospheric compensation.

This compensation method has the advantage that was developed and tested using terrestrial hyperspectral airborne data. The data are in one of our LPSC 2002 abstracts (in Adobe PDF).


Field spectrometer data.

This gives spectra of the diffuse aluminum target laboratory emissivity; a diffuse aluminum target field spectrum; spectrum of a region with near 100% coverage by indurated carbonate (calcrete); and a blackbody fit to the measured data. These values will be published in June 2002 in our Remote Sensing of Environment paper (in Adobe PDF).


TES signal-to-noise ratio values.

These values are published in our Applied Optics paper (in Adobe PDF). The signal-to-noise ratio indicates how sensitive the measurement is as a function of wavenumber.


2001 THEMIS band centers, band widths, and signal-to-noise ratio values.

These values are published in the Mars Odyssey Participating Scientist Proposal Information Package, and we also give values at 270K for more direct comparison to other Mars instruments. The signal-to-noise ratio indicates how sensitive the measurement is as a function of wavelength.


SEBASS band centers and signal-to-noise ratio values.

These values are published in Remote Sensing of Environment (2002). We give the values for a blackbody at 270K (a standard for Mars) and 300K (a standard for Earth). The signal-to-noise ratio indicates how sensitive the measurement is as a function of wavelength.


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