Wavelength dependance of polarization. III. The lunar surface.

Gehrels, T.; Coffeen, T.; Owings, D.

doi:10.1086/109359

Cited by 169 publications

(31 citation statements)

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“…The question of the colour differences of the lunar regions with possible correlation with physical parameters is not settled up to the present time (Hapke, 1971). Gehrels et al (1964) have detected higher values of albedos than the previous determination. Gehrels et al (1964) have detected higher values of albedos than the previous determination.…”

Section: Introductioncontrasting

confidence: 60%

“…In addition, the data have been normalized using the same method mentioned by Gehrels et al (1964). The correction to the mean Earth-Sun distance is applied by taking the distance R of the Sun to the Earth in astronomical units as it is published in the Nautical Almanac.…”

Section: Lunar Measurements and Correctionsmentioning

confidence: 99%

“…The correction to the mean Earth-Sun distance is applied by taking the distance R of the Sun to the Earth in astronomical units as it is published in the Nautical Almanac. The correction values given by Gehrels et al (1964) for the 82" reflector of McDonald Observatory at Cassegrain focus of the scale 7"4 mm -~ is used in the present correction for the observations of the 74" reflector of the Kottamia Observatory at the Cassegrain focus of scale 6"17 mm -~. To correct for the light scattered into the lunar aureole, mainly by the Earth's atmosphere, the values given by previous workers are used.…”

Section: Lunar Measurements and Correctionsmentioning

confidence: 99%

“…Modern photometric measurements of lunar grounds have been made by Fedoretz (1952) ;Gehrels et al (1964); Peacock (1968); Jones (1969); and Shorthill et al (1969). Fedoretz and Jones' measurements have been carried out using photographic technique.…”

Section: Introductionmentioning

confidence: 99%

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Monochromatic intensity measurements of selected areas of lunar surface for possible investigations

Mikhail

1974

The Moon

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Absolute photoelectric intensity measurements of 104 selected lunar regions are given in five interference filters 4035 A,, 4765 A~, 5538/~, 6692 A_ and 7922 A,. Among these regions, eighteen lunar regions have been measured repeatedly for several phase angles between ÷86 ° and --43 °. They include observations made very close to the full Moon. A catalogue has been compiled to serve as a basin for possible investigations of colour contrasts of lunar grounds, variation of the ratio of reflectivity with wavelengths and phase angles for morphological studies. The study can be extended for the brightness phase variation, opposition effect and radiance factors at zero phase in five colours.

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Section: Introductioncontrasting

confidence: 60%

Section: Lunar Measurements and Correctionsmentioning

confidence: 99%

Section: Lunar Measurements and Correctionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Monochromatic intensity measurements of selected areas of lunar surface for possible investigations

Mikhail

1974

The Moon

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“…The phase reddening was first noted by Gehrels et al (1964) on the lunar surface, and it is potentially attributed to the increased contribution of the multiple scattering at large phase angles as the wavelength and albedo increase, plus a contribution of surface roughness effects (Sanchez et al 2012;Hapke et al 2012;Schroder et al 2014). As reported in Fig.…”

Section: Phase Reddeningmentioning

confidence: 76%

Spectrophotometric properties of the nucleus of comet 67P/Churyumov-Gerasimenko from the OSIRIS instrument onboard the ROSETTA spacecraft

Fornasier

Hasselmann

Barucci

et al. 2015

A&A

215

147

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Context. The Rosetta mission of the European Space Agency has been orbiting the comet 67P/Churyumov-Gerasimenko (67P) since August 2014 and is now in its escort phase. A large complement of scientific experiments designed to complete the most detailed study of a comet ever attempted are onboard Rosetta. Aims. We present results for the photometric and spectrophotometric properties of the nucleus of 67P derived from the OSIRIS imaging system, which consists of a Wide Angle Camera (WAC) and a Narrow Angle Camera (NAC). The observations presented here were performed during July and the beginning of August 2014, during the approach phase, when OSIRIS was mapping the surface of the comet with several filters at different phase angles (1.3• -54• ). The resolution reached up to 2.1 m/px. Methods. The OSIRIS images were processed with the OSIRIS standard pipeline, then converted into I/F radiance factors and corrected for the illumination conditions at each pixel using the Lommel-Seeliger disk law. Color cubes of the surface were produced by stacking registered and illumination-corrected images. Furthermore, photometric analysis was performed both on disk-averaged photometry in several filters and on disk-resolved images acquired with the NAC orange filter, centered at 649 nm, using Hapke modeling. Results. The disk-averaged phase function of the nucleus of 67P shows a strong opposition surge with a G parameter value of −0.13 ± 0.01 in the HG system formalism and an absolute magnitude H v (1, 1, 0) = 15.74 ± 0.02 mag. The integrated spectrophotometry in 20 filters covering the 250−1000 nm wavelength range shows a red spectral behavior, without clear absorption bands except for a potential absorption centered at ∼290 nm that is possibly due to SO 2 ice. The nucleus shows strong phase reddening, with disk-averaged spectral slopes increasing from 11%/(100 nm) to 16%/(100 nm) in the 1.3• −54• phase angle range. The geometric albedo of the comet is 6.5 ± 0.2% at 649 nm, with local variations of up to ∼16% in the Hapi region. From the disk-resolved images we computed the spectral slope together with local spectrophotometry and identified three distinct groups of regions (blue, moderately red, and red). The Hapi region is the brightest, the bluest in term of spectral slope, and the most active surface on the comet. Local spectrophotometry shows an enhancement of the flux in the 700−750 nm that is associated with coma emissions.

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Resolved Hapke parameter maps of the Moon

Sato

Robinson

Hapke

et al. 2014

J. Geophys. Res. Planets

112

125

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reflectance from large numbers of repeated observations (UV: ∼50 and visible: ∼126 on average). The derived mosaic exhibits no significant artifacts with latitude or along the tile boundaries, demonstrating the quality of the normalization procedure. The derived Hapke parameter maps reveal regional photometric response variations across the lunar surface. The b, c (Henyey-Greenstein double-lobed phase function parameters) maps demonstrate decreased backscattering in the maria relative to the highlands (except 321 nm band), probably due to the higher content of both SMFe (submicron iron) and ilmenite in the interiors of back scattering agglutinates in the maria. The h S (angular width of shadow hiding opposition effect) map exhibits relatively lower values in the maria than the highlands and slightly higher values for immature highland crater ejecta, possibly related to the variation in a grain size distribution of regolith.

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Wavelength dependance of polarization. III. The lunar surface.

Cited by 169 publications

References 0 publications

Monochromatic intensity measurements of selected areas of lunar surface for possible investigations

Monochromatic intensity measurements of selected areas of lunar surface for possible investigations

Spectrophotometric properties of the nucleus of comet 67P/Churyumov-Gerasimenko from the OSIRIS instrument onboard the ROSETTA spacecraft

Resolved Hapke parameter maps of the Moon

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