Published June 11, 2021 | Version 1
Dataset Open

THEMIS-derived Thermal Inertia of Jezero Crater, Mars

  • 1. Northern Arizona University

Description

The Thermal Emission Imaging System (THEMIS) inertia mosaic of Jezero Crater was created following the methods of Edwards et al. (2011) and Edwards et al. (2018) with modifications following THEMIS thermal inertia generation in Piqueux et al. (2019). First individual THEMIS images were processed following standard nighttime image processing procedures for THEMIS data (Edwards et al., 2011). Then individual images where processed to thermal inertia using the methods of Edwards et al. (2018), which were updated in Piqueux et al. (2019) to modify the derivation method to use TES albedo as opposed to THEMIS albedo. The outcome of this process results in a product that is similar to the thermal inertia derived by Edwards and Ehlmann (2015) where small scale albedo differences can cause ~20 J/m2/K1/s1/2 differences with units of the same thermal inertia.

Following the production of thermal inertia, individual images were allowed to be offset by matching the average thermal inertia of overlapping regions, resulting in a maximum of ~20 J/m2/K1/s1/2 offset, well within the derivation uncertainty when accounting for THEMIS temperature uncertainty (e.g. Fergason et al., 2006). Images were then mosaicked following the standard processes for creating quantitative mosaics (Edwards et al., 2011) with overlapping regions being linearly blended together via a two dimensional linear ramp.

The image is in GeoTIFF format, has a null (black space) value of 0, and units of J/m2/K1/s1/2

 


 

Notes

Funding for this dataset is provided by the 2001 Mars Odyssey Project - THEMIS Instrument

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Additional details

References

  • Edwards, C. S., Nowicki, K. J., Christensen, P. R., Hill, J., Gorelick, N., & Murray, K. (2011). Mosaicking of global planetary image datasets: 1. Techniques and data processing for Thermal Emission Imaging System (THEMIS) multi-spectral data. Journal of Geophysical Research-Planets, 116. doi: 10.1029/2010JE003755
  • Edwards, C. S., Piqueux, S., Hamilton, V. E., Fergason, R. L., Herkenhoff, K. E., Vasavada, A. R., Bennett, K. A., Sacks, L., Lewis, K. W., & Smith, M. D. (2018). The Thermophysical Properties of the Bagnold Dunes, Mars: Ground-Truthing Orbital Data. Journal of Geophysical Research: Planets, 123(5), 1307-1326. doi: 10.1029/2017je005501
  • Edwards, C. S., & Ehlmann, B. L. (2015). Carbon sequestration on Mars. Geology, 43(10), 863-866. doi: 10.1130/G36983.1
  • Fergason, R. L., Christensen, P. R., & Kieffer, H. H. (2006). High resolution thermal inertia derived from THEMIS: Thermal model and applications. J. Geophys. Res., 111, E12004. doi: 10.1029/2006JE002735
  • Piqueux, S., Buz, J., Edwards, C. S., Bandfield, J. L., Kleinböhl, A., Kass, D. M., Hayne, P. O., MCS, & Teams, T. (2019). Widespread Shallow Water Ice on Mars at High Latitudes and Midlatitudes. Geophysical Research Letters, 46(24), 14290-14298. doi: 10.1029/2019GL083947