We mapped the surface layers of the Ophir Chasma region using observations made by the Mars Global Surveyor's Thermal Emission Spectrometer (TES) and the Mars Odyssey's Thermal Emission Imaging System (THEMIS). Our goal is to understand the surface physical characteristics and how they relate to the local geology. TES observations indicate that Ophir Chasma possesses some of the most diverse thermal properties on Mars where the approximate global maximum and minimum values of the derived thermal inertia have been detected within ~100 km of each other. The thermal maps, used in conjunction with elevation data, meteorological modeling and high-resolution images, have led to many insights on how the thermal inertia relates to the local morphology and mineralogy. The landslide units on the northern margin of Ophir Chasma have a diverse range of characteristics. A fairly linear relation between elevation and thermal inertia was found that is consistent with the global trend. Recent and/or ongoing aeolian processes are likely closely linked to the current thermal properties of the canyon. These aeolian processes, in turn, are affected by the topography of not only Ophir, but Hebes and Candor Chasmata and neighboring regions. This study has confirmed previous geological interpretations as well as allowed new insights of how the thermal properties of a surface relates to its geology.