Multicolor Photoelectric Photometry of the Brighter Planets. III. Observations from Boyden Observatory

Irvine, William M.; Simon, Theodore; Menzel, Donald H.; Pikoos, C.; Young, A. T.

doi:10.1086/110702

Cited by 115 publications

(44 citation statements)

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“…As a result, although we can take advantage of temporal variation as Mars spins on its axis, visibility geometry only provides limited assistance in reconstructing the surface, since single-pixel observations of always involve a large fraction of the Martian area. [8,9]. By exploiting the time-varying occlusion geometry, we recovered a coarse hyperspectral map of Mars, with a spatial resolution of roughly 6 × 1, shown in false color (d).…”

Section: Mars From Single-pixel Observationsmentioning

confidence: 99%

“…Real planetary photometry data To test the capability of our reconstruction method, we considered a set of singlepixel photometry measurements made of Mars between 1963-1965 [8,9]. Although these data were not collected to recover surface detail, nor have they been previously analyzed in this way, we show that these historical measurements indeed encode coarse surface structure (Fig.…”

Section: Mars From Single-pixel Observationsmentioning

confidence: 99%

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Diffuse reflectance imaging with astronomical applications

Hasinoff¹,

Levin

Goode³

et al. 2011

2011 International Conference on Computer Vision

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Diffuse objects generally tell us little about the surrounding lighting, since the radiance they reflect blurs together incident lighting from many directions. In this paper we discuss how occlusion geometry can help invert diffuse reflectance to recover lighting or surface albedo. Selfocclusion in the scene can be regarded as a form of coding, creating high frequencies that improve the conditioning of diffuse light transport. Our analysis builds on a basic observation that diffuse reflectors with sufficiently detailed geometry can fully resolve the incident lighting. Using a Bayesian framework, we propose a novel reconstruction method based on high-resolution photography, taking advantage of visibility changes near occlusion boundaries. We also explore the limits of single-pixel observations as the diffuse reflector (and potentially the lighting) vary over time. Diffuse reflectance imaging is particularly relevant for astronomy applications, where diffuse reflectors arise naturally but the incident lighting and camera position cannot be controlled. To test our approaches, we first study the feasibility of using the moon as a diffuse reflector to observe the earth as seen from space. Next we present a reconstruction of Mars using historical photometry measurements not previously used for this purpose. As our results suggest, diffuse reflectance imaging expands our notion of what can qualify as a camera.

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Section: Mars From Single-pixel Observationsmentioning

confidence: 99%

Section: Mars From Single-pixel Observationsmentioning

confidence: 99%

Diffuse reflectance imaging with astronomical applications

Hasinoff¹,

Levin

Goode³

et al. 2011

2011 International Conference on Computer Vision

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“…An increase in reflectance with wavelength (reddening) at wavelengths ≥0.6 μm was noted for Mercury (cf. Irvine et al 1968), the Moon (Lane and Irvine 1973), and Vesta (Gehrels 1967) at high phase angles. Notably, Irvine et al also observed reddening in their U-B color of Mercury at phase angle α = 70° compared to lower phase angles, also suggesting the possibility of wavelength-dependent changes with larger phase angles.…”

Section: Introductionmentioning

confidence: 97%

Local topographic effects on photometry and reflectance spectra of planetary surfaces: An example based on lunar photometry

Domingue

Vilas

2007

Meteorit & Planetary Scien

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Abstract-The photometric properties of the average lunar surface are characterized using Hapke's equations and whole disk observations ranging from 0.36 to 1.06 μm. Synthetic spectra across a crater topographic profile are created using the modeling results. The synthetic spectra are examined for spectral variations created by changes in lighting conditions induced by the topography. Changes above the modeling uncertainties are seen in both spectral slope and band depths, though the most pronounced change is in band depth. The data have insufficient spectral resolution to determine if there are any changes in band center due to photometric effects. No additional absorption features are introduced by the photometry. These results have serious implications on the interpretation of spectral observations in terms of abundance estimates and alteration processes as a function of location and association with geologic features.

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“…Results of a program of multicolor photoelectric photometry of the planet Jupiter between the dates June 3, 1963, andDecember 19, 1965, have been reported by Irvine et al (1968a;Paper II) and Irvine et al (1968b;Paper III). Observations were made at both the Le Houga Observatory in France and the Boyden Observatory in South Africa, using 10 narrow bands isolated by interference filters between 3150 A and 1.06 /x, and also in UBV.…”

Section: Introductionmentioning

confidence: 96%

Variations in the color of jupiter

Hopkins¹,

Irvine²

1971

Symp. - Int. Astron. Union

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Abstract. Observations of Jupiter by multicolor photoelectric photometry in 10 narrow bands between 3150 A and 1.06/x and in UBV showed a brightening for shorter wavelengths in 1965 relative to 1963. An opposite effect occurred for the band at 7300 A. These results are consistent with observed activity in the Jovian atmosphere. No obvious correlation could be found between brightness fluctuations and longitude of the central meridian, indicating that the activity was uniform in longitude or occurred on time scales short compared to a month.

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Multicolor Photoelectric Photometry of the Brighter Planets. III. Observations from Boyden Observatory

Cited by 115 publications

References 0 publications

Diffuse reflectance imaging with astronomical applications

Diffuse reflectance imaging with astronomical applications

Local topographic effects on photometry and reflectance spectra of planetary surfaces: An example based on lunar photometry

Variations in the color of jupiter

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