The Thermal Emission Imaging System (THEMIS) for the Mars 2001 Odyssey Mission

By Philip R. Christensen, B. Jakosky, Hugh H. Kieffer, Michael C. Malin, H. McSween, Kenneth Nealson, G. Mehall, S. Silverman, S. Ferry, Michael A. Caplinger and 1 more. 2004

1,006 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/39afd04622e5a134c2676c0fe786f86e558e27d9

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Formation timescales of large Martian valley networks (2011, methodology): “…that was manually drawn along the outer walls of the visible valleys from coregistered topographic data and Mars Odyssey (MO) Thermal Emission Imaging System (THEMIS) daytime infrared (IR) images (256 m/pix) (Christensen et al., 2004), and accounting for the local slope of the surrounding surface.”
Mars Global Digital Dune Database and initial science results (2007, background): “Slipface orientations are less well correlated, suggesting that local topographic effects may play a larger role in dune orientation than regional winds.”
Updated global map of Martian valley networks and implications for climate and hydrologic processes (2010, background): “Carr and Malin [2000] noted that at high resolution (few meters/ pixel), the Noachian highlands were largely undissected and suggested that this observation implies precipitation and that surface runoff may not have been important across much of Mars.”
Radar evidence for ice in lobate debris aprons in the mid‐northern latitudes of Mars (2009, background): “Their geomorphic expression and restricted occurrence in latitude has led numerous workers to conclude that LDAs contain water ice, but the suggested amount of ice involved in their formation and evolution has ranged from minor interstitial ice in rocky talus [e.g., Squyres, 1978] to predominantly i”
Geologic Constraints on Early Mars Climate (2018, methodology): “Most large gaps in the latitude-longitude distribution of valley networks in THEMIS and MOLA databases (Hynek et al. 2010, Luo et al. 2017) correspond to post-fluvial resurfacing (i.e., Amazonian lava or Amazonian ice-rich mantling deposits).”
Selection of the Mars Science Laboratory Landing Site (2012, methodology): “…useful for MSL site selection included: (1) 100 m THEMIS thermal images and global mosaic for siting ellipses in smooth, flat locations (Christensen et al. 2004), (2) HRSC multiple orbit stereo orthophotos (12.5 m/pixel) and DEMs (∼50 m elevation postings) that are excellently…”
Mineralogy of the Martian Surface (2014, background): “…et al. 2001 2001–present THEMIS Thermal Emission Imaging System Orbit Thermal infrared multispectral imaging (6.7–14.8 μm; 7 bands; 100-m pixels) Christensen et al. 2004 2004–2011 (Spirit) 2004–present (Opportunity) Mini-TES Miniature Thermal Emission Spectrometer Rover Thermal…”