Near-Infrared Absolute Photometric Imaging of the Uranian System

Baines, K. H.; Yanamandra-Fisher, P.; Lebofsky, L. A.; Momary, T.; Golisch, W.; Kaminski, C.; Wild, Walter J.

doi:10.1006/icar.1998.5894

Cited by 28 publications

(45 citation statements)

References 42 publications

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“…As the J band spectral segment does not overlap the 1.8-µm band spectrum, there is some uncertainty in the colors including J. The H -K color derived from the broadband spectral reflectance values of the UKIRT spectra ( p H −K = 0.04 ± 0.01) agree within the formal errors with values reported by Baines et al (1998) …”

Section: Photometrysupporting

confidence: 55%

“…• in comparison to values reported in Karkoschka (1997), Kesten et al (1998), and Baines et al (1998) from 0.3 to 2.5 µm at phase angle 1…”

Section: Photometrymentioning

confidence: 78%

“…Subsequent ground-based observations (Buratti et al 1992) revealed a strong opposition surge in brightness at optical wavelengths indicative of a "fluffy" porous surface. The JHH K photometry of Baines et al (1998) showed that the opposition effect likely extends into the infrared. A fluffy, multiply cratered surface may imply a history of bombardments by small bodies.…”

Section: Introductionmentioning

confidence: 98%

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The Near Infrared Spectrum of Miranda Evidence of Crystalline Water Ice

Bauer¹

2002

Icarus

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Section: Photometrysupporting

confidence: 55%

“…• in comparison to values reported in Karkoschka (1997), Kesten et al (1998), and Baines et al (1998) from 0.3 to 2.5 µm at phase angle 1…”

Section: Photometrymentioning

confidence: 78%

Section: Introductionmentioning

confidence: 98%

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The Near Infrared Spectrum of Miranda Evidence of Crystalline Water Ice

Bauer¹

2002

Icarus

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“…Uranus' faint rings and close moons are difficult to detect at visible wavelengths due to scattered light from the planet, but can be more easily observed at wavelengths near 2 µm, where the planet appears dark due to strong methane absorption. Baines et al (1998) and Sromovsky et al (2000) published ground-based images of Uranus and its rings in which the ring with its asymmetric brightness distribution was easily observed, but due to the relatively low spatial resolution (typically ∼ 0.5 from the ground) none of the other rings could be seen. Karkoschka (2001a) published photometry of the uranian moons and ring system from Hubble Space Telescope images, including the ring and the three inner ring groups at visible to near-infrared wavelengths.…”

Section: Introductionmentioning

confidence: 99%

Near-infrared adaptive optics imaging of the satellites and individual rings of Uranus

Gibbard¹,

Pater²,

Hammel³

2005

Icarus

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We present the first Earth-based images of several of the individual faint rings of Uranus, as observed with the adaptive optics system on the W.M. Keck II telescope on four consecutive days in October 2003. We derive reflectivities based on multiple measurements of 8 minor moons of Uranus as well as Ariel and Miranda in filters centered at wavelengths of 1.25(J), 1.63(H), and 2.1(Kp) µm. These observations have a phase angle of 1.84 • -1.96 • . We find that the small satellites are somewhat less bright than in observations made by the HST at smaller phase angles, confirming an opposition surge effect. We calculate albedoes for the ring groups and for each ring separately. We find that the ring particles, as well as the particles in the three other ring groups, have albedoes near 0.043 at these phase angles. The equivalent depths of some of the individual rings are different than predicted based upon ring widths from occultation measurements (assuming a constant particle ring brightness); in particular the γ ring is fainter and the η ring brighter than expected. Our results indicate that q, the ratio of ring intensity at apoapse vs. periapse, is close to 3.2 ± 0.16. This agrees well with a model that has a filling factor for the ring of 0.06 (Karkoschka, 2001, Icarus 151, 78-83). We also determine values of the north to south brightness ratio for the individual rings and find that in most cases they are close to unity.

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“…Kesten et al (1998) for Miranda, and Cruikshank (1980) for Oberon). However, we can note values of the K reflectivity slightly different (around 0. m 016, sensible lower than the V magnitude drop) for Miranda in the article of Baines et al (1998). For our study we consider the V band magnitude drop estimation also reasonable for the K band.…”

Section: The Observation Of the 2007 July 30 Miranda-oberon Occultationmentioning

confidence: 81%

Photometric and astrometric analysis of a mutual event between the Uranian satellites Miranda and Oberon

et al. 2008

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Observations of the predicted occultation between the satellites Miranda and Oberon were performed on 2007 July 30. Data analysis reveals that the predicted magnitude drop for this phenomenon was overestimated and we establish an upper limit of 0.m 05 for the phenomenon, perhaps due to a non-lambertian limb scattering. The new astrometry obtained from this run is in good agreement with the LA06 numerical model and these new data will improve the dynamical models of the Uranus system. The paper concludes with an uncertainty analysis on the parameters for the event, determined by the uncertainty of the magnitude drop of about 0.04 mag, and the difficulty to observe mutual phenomena between satellites in the Uranian system.

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Near-Infrared Absolute Photometric Imaging of the Uranian System

Cited by 28 publications

References 42 publications

The Near Infrared Spectrum of Miranda Evidence of Crystalline Water Ice

The Near Infrared Spectrum of Miranda Evidence of Crystalline Water Ice

Near-infrared adaptive optics imaging of the satellites and individual rings of Uranus

Photometric and astrometric analysis of a mutual event between the Uranian satellites Miranda and Oberon

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