Thermal removal from near-infrared imaging spectroscopy data of the Moon
Article first published online: 24 JUN 2011
Copyright 2011 by the American Geophysical Union.
Journal of Geophysical Research: Planets (1991–2012)
Volume 116, Issue E6, June 2011
How to Cite
2011), Thermal removal from near-infrared imaging spectroscopy data of the Moon, J. Geophys. Res., 116, E00G16, doi:10.1029/2010JE003751., , , , and (
- Issue published online: 24 JUN 2011
- Article first published online: 24 JUN 2011
- Manuscript Accepted: 8 MAR 2011
- Manuscript Revised: 1 FEB 2011
- Manuscript Received: 30 SEP 2010
 In the near-infrared from about 2 μm to beyond 3 μm, the light from the Moon is a combination of reflected sunlight and emitted thermal emission. There are multiple complexities in separating the two signals, including knowledge of the local solar incidence angle due to topography, phase angle dependencies, emissivity, and instrument calibration. Thermal emission adds to apparent reflectance, and because the emission's contribution increases over the reflected sunlight with increasing wavelength, absorption bands in the lunar reflectance spectra can be modified. In particular, the shape of the 2 μm pyroxene band can be distorted by thermal emission, changing spectrally determined pyroxene composition and abundance. Because of the thermal emission contribution, water and hydroxyl absorptions are reduced in strength, lowering apparent abundances. It is important to quantify and remove the thermal emission for these reasons. We developed a method for deriving the temperature and emissivity from spectra of the lunar surface and removing the thermal emission in the near infrared. The method is fast enough that it can be applied to imaging spectroscopy data on the Moon.