A photometric function for analysis of lunar images in the visual and infrared based on Moon Mineralogy Mapper observations

[1] Changes in observed photometric intensity on a planetary surface are caused by variations in local viewing geometry defined by the radiance incidence, emission, and solar phase angle coupled with a wavelength-dependent surface phase function f(α, λ) which is specific for a given terrain. In this paper we provide preliminary empirical models, based on data acquired inflight, which enable the correction of Moon Mineralogy Mapper (M3) spectral images to a standard geometry with the effects of viewing geometry removed. Over the solar phase angle range for which the M3 data were acquired our models are accurate to a few percent, particularly where thermal emission is not significant. Our models are expected to improve as additional refinements to the calibrations occur, including improvements to the flatfield calibration; improved scattered and stray light corrections; improved thermal model corrections; and the computation of more accurate local incident and emission angles based on surface topography.

[1]  B. Hapke.  Bidirectional reflectance spectroscopy: 4. The extinction coefficient and the opposition effect , 1986 .

[2]  J. Veverka,et al.  Photometry of rough planetary surfaces: The role of multiple scattering , 1985 .

[3]  H. Kieffer,et al.  The Spectral Irradiance of the Moon , 2005 .

[4]  Bruce Hapke,et al.  Coherent backscatter and the radar characteristics of outer planet satellites , 1990 .

[5]  Hugh H. Kieffer,et al.  Establishing the Moon as a Spectral Radiance Standard , 1996 .

[6]  B. Buratti.  Application of a radiative transfer model to bright icy satellites , 1984 .

[7]  B. Hapke.  Bidirectional reflectance spectroscopy , 1984 .

[8]  Eric M. Eliason,et al.  Lunar Reconnaissance Orbiter Camera: First results , 2010 .

[9]  B. Buratti.  Voyager disk resolved photometry of the Saturnian satellites , 1984 .

[10]  M. D. Dyar,et al.  Character and Spatial Distribution of OH/H2O on the Surface of the Moon Seen by M3 on Chandrayaan-1 , 2009, Science.

[11]  Bonnie J. Buratti,et al.  A wavelength-dependent visible and infrared spectrophotometric function for the Moon based on ROLO data , 2011 .

[12]  B. Hapke.  Bidirectional reflectance spectroscopy: 1. Theory , 1981 .

[13]  James L. Elliot,et al.  Scattering of light from particulate surfaces. I - A laboratory assessment of multiple-scattering effects. [planetary simulation , 1978 .

[14]  B. Buratti,et al.  THE LUNAR OPPOSITION SURGE : OBSERVATIONS BY CLEMENTINE , 1996 .

[15]  Y. Shkuratov,et al.  The phase ratios of the color index: Mapping of two regions of the near side of the Moon , 2010 .

[16]  C. M. Pieters,et al.  Strength of mineral absorption features in the transmitted component of near-infrared reflected light - First results from RELAB. [spectrogoniometer for planetary and lunar surface composition experiments] , 1983 .

[17]  B. Hapke.  Theory of reflectance and emittance spectroscopy , 1993 .

[18]  Bonnie J. Buratti,et al.  Multispectral photometry of the Moon and absolute calibration of the Clementine UV/Vis camera , 1999 .

[19]  William M. Irvine,et al.  The shadowing effect in diffuse reflection , 1966 .

[20]  G. Rybicki.  Radiative transfer , 2019, Climate Change and Terrestrial Ecosystem Modeling.