Searching at the right time of day: Evidence for aqueous minerals in Columbus crater with TES and THEMIS data
Article first published online: 12 FEB 2013
©2012. American Geophysical Union. All Rights Reserved.
Journal of Geophysical Research: Planets
Volume 118, Issue 2, pages 179–189, February 2013
How to Cite
2013), Searching at the right time of day: Evidence for aqueous minerals in Columbus crater with TES and THEMIS data, J. Geophys. Res. Planets, 118, 179–189, doi:10.1029/2012JE004225., , and (
- Issue published online: 2 APR 2013
- Article first published online: 12 FEB 2013
- Manuscript Accepted: 14 NOV 2012
- Manuscript Revised: 8 NOV 2012
- Manuscript Received: 3 AUG 2012
- aqueous minerals;
- orbit time
 The primary objective of the Thermal Emission Imaging System (THEMIS) experiment, which has been in orbit at Mars since early 2002, is to identify minerals associated with hydrothermal and subaqueous environments. Data from THEMIS have supported the presence of clays, silica-rich deposits, and chlorides but has not before provided definitive evidence for the presence of sulfates. This is an especially puzzling result given that sulfates have been extensively identified with other instruments at Mars. If present, sufficiently exposed, and in high enough abundances, such minerals should be detectable in orbital thermal infrared spectra at the resolution of THEMIS. The extended mission proposal for THEMIS on Mars Odyssey suggests that the detection of all minerals may be enhanced by observing at an earlier time of day and thus at warmer temperatures. Therefore, in 2009, Odyssey moved to an earlier orbit time. Here, we examine THEMIS data collected when the earlier orbit time coincided with the Martian local (southern) late summer (Ls = 270) for Columbus crater where Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) data have detected a number of aqueous minerals. Some of the warmest THEMIS images show evidence for aqueous minerals, although not in the same locations where CRISM finds the highest concentrations. Several factors contribute to this result, including differences in the diurnal temperature curve and levels of induration and particle size. For THEMIS, earlier time-of-day and proper seasonal observations combine to provide warm surface temperatures and ideal low atmospheric opacity that significantly increases the ability to definitively identify low spectral contrast aqueous minerals at the surface of Mars.