Resolved Hapke parameter maps of the Moon

Sato, Hiroyuki; Robinson, M. S.; Hapke, Bruce; Denevi, Brett W.; Boyd, A. K.

doi:10.1002/2013je004580

Cited by 113 publications

(138 citation statements)

References 77 publications

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“…Other future work in asteroid photometry might result in sufficient sampling of spatially resolved scattering behavior such that actual physically meaningful scattering model parameters can be mapped across the surface, such as in the work of Sato et al (2014), who present and interpret Hapke model parameter maps of the lunar surface. These workers find decreased backscattering in the maria relative to the lunar highlands, consistent with known compositional and space weathering differences between maria and highlands, and suggesting powerful new ways to potentially study variations across the surface of an asteroid.…”

Section: ! 27!mentioning

confidence: 99%

Asteroid Photometry

Li¹,

Helfenstein²,

Buratti³

et al. 2015

Asteroids IV

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Asteroid photometry has three major applications: providing clues about asteroid surface physical properties and compositions, facilitating photometric corrections, and helping design and plan ground-based and spacecraft observations. The most significant advances in asteroid photometry in the past decade were driven by spacecraft observations that collected spatially resolved imaging and spectroscopy data. In the mean time, laboratory measurements and theoretical developments are revealing controversies regarding the physical interpretations of models and model parameter values. We will review the new developments in asteroid photometry that have occurred over the past decade in the three complementary areas of observations, laboratory work, and theory. Finally we will summarize and discuss the implications of recent findings. ! 2!

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Section: ! 27!mentioning

confidence: 99%

Asteroid Photometry

Li¹,

Helfenstein²,

Buratti³

et al. 2015

Asteroids IV

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“…(433) Eros, orbited by NEAR Shoemaker (Clark et al, 2002), Phobos and Deimos, visited by Viking Orbiter (Thomas et al, 1996;Simonelli et al, 1998) and (25143) Itokawa, orbited by Hayabusa (Kitazato et al, 2008) and (4) Vesta, orbited by Dawn (Li et al, 2013b), are examples of small bodies which had their global Hapke parameters obtained. However, only recently, efforts have been taken to derive a spatially resolved Hapke parameters out of disk-resolved data (Spjuth et al, 2012;Sato et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

Asteroid (21) Lutetia: Disk-resolved photometric analysis of Baetica region

Hasselmann

Fornasier

Leyrat

et al. 2016

Icarus

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ABSTRACT. (21) Lutetia has been visited by Rosetta mission on July 2010 and observed with a phase angle ranging from 0.15 to 156.8 degrees. The Baetica region, located at the north pole has been extensively observed by OSIRIS cameras system. Baetica encompass a region called North Pole Crater Cluster (NPCC), shows a cluster of superposed craters which presents signs of variegation at the small phase angle images. For studying the location, we used 187 images distributed throughout 14 filter recorded by the NAC (Narrow Angle Camera) and WAC (Wide Angle Camera) of the OSIRIS system on-board Rosetta taken during the fly-by. Then, we photometrically modeled the region using Minnaert diskfunction and Akimov phase function to obtain a resolved spectral slope map at phase angles of 5 • and 20 • . We observed a dicothomy between Gallicum and Danuvius-Sarnus Labes in the NPCC, but no significant phase reddening (−0.04 ± 0.045% · microns −1 deg −1 ). In the next step, we applied the Hapke (2008Hapke ( ,2012 model for the NAC F82+F22 (649.2 nm), WAC F13 (375 nm) and WAC F17 (631.6 nm) and we obtained normal albedo maps and Hapke parameter maps for NAC F82+F22. On Baetica, at 649.2 nm, the geometric albedo is 0.205 ± 0.005, the average single-scattering albedo is 0.181 ± 0.005, the average asymmetric factor is −0.342 ± 0.003, the average shadow-hiding opposition effect amplitude and width are 0.824 ± 0.002 and 0.040 ± 0.0007, the average roughness slope is 11.45 • ± 3 • and the average porosity is 0.85 ± 0.002. We are unable to confirm the presence of coherent-backscattering mechanism. In the NPCC, the normal albedo variegation among the craters walls reach 8% brighter for Gallicum Labes and 2% fainter for Danuvius Labes. The Hapke parameter maps also show a dicothomy at the opposition effect coefficients, single-scattering albedo and asymmetric factor, that may be attributed to the maturation degree of the regolith or to compositonal variation. In addition, we compared the Hapke (2008Hapke ( , 2012 and Hapke (1993) parameters with laboratory samples and other small-solar system bodies visited by space missions.

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“…In addition, information regarding the interior and exterior orientation parameters that is stored in a series of SPICE kernels (Acton, 1996) are attached to the header of each image. For Clementine images, we follow the calibration procedures and photometric correction described in McEwen et al, 1998) while we follow the calibration procedures described in (Robinson et al, 2010) and use photometric function and parameters defined in (Sato et al, 2014) when processing LROC WAC images. These procedures are carried out using Integrated Software for Imagers and Spectrometers (ISIS) (Anderson et al, 2004), which is developed and maintained by the Astrogeology Research Program at the USGS.…”

Section: Image Preparationmentioning

confidence: 99%

“…Since the LROC WAC has acquired over 60 global mosaics (from 1 January 2010 to 15 March 2016), images will be selected such that the lighting conditions are nearly identical to the Clementine images they overlap. All 12 bands will be photometrically normalized to common viewing and illumination angles (incidence = 30°, emission = 0°, and phase = 30°) using methods and photometric parameters defined by the UVVIS and WAC imaging teams (McEwen et al, 1997;Sato et al, 2014).…”

Section: Next Stepsmentioning

confidence: 99%

Geometric Calibration of the Clementine Uvvis Camera Using Images Acquired by the Lunar Reconnaissance Orbiter

Speyerer

Wagner

Robinson

2016

Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci.

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ABSTRACT:The Clementine UVVIS camera returned over half a million images while in orbit around the Moon in 1994. Since the Clementine mission, our knowledge of lunar topography, gravity, and the location of features on the surface has vastly improved with the success of the Gravity Recovery and Interior Laboratory (GRAIL) mission and ongoing Lunar Reconnaissance Orbiter (LRO) mission. In particular, the Lunar Reconnaissance Orbiter Camera (LROC) has returned over a million images of the Moon since entering orbit in 2009. With the aid of improved ephemeris and on-orbit calibration, the LROC team created a series of precise and accurate global maps. With the updated reference frame, older lunar maps, such as those generated from Clementine UVVIS images, are misaligned making cross-mission analysis difficult. In this study, we use feature-based matching routines to refine and recalibrate the interior and exterior orientation parameters of the Clementine UVVIS camera. After applying these updates and rigorous orthorectification, we are able generate precise and accurate maps from UVVIS images to help support lunar science and future cross-mission investigations.

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Resolved Hapke parameter maps of the Moon

Cited by 113 publications

References 77 publications

Asteroid Photometry

Asteroid Photometry

Asteroid (21) Lutetia: Disk-resolved photometric analysis of Baetica region

Geometric Calibration of the Clementine Uvvis Camera Using Images Acquired by the Lunar Reconnaissance Orbiter

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