The Cassini Visual and Infrared Mapping Spectrometer (VIMS) Investigation

Brown, R. H.; Baines, K. H.; Bellucci, G.; Bibring, J. P.; Buratti, B. J.; Capaccioni, F.; Cerroni, P.; Clark, R. N.; Coradini, A.; Cruikshank, D. P.; Drossart, P.; Formisano, V.; Jaumann, R.; Langevin, Y.; Matson, D. L.; McCord, T. B.; Mennella, V.; Miller, Edward; Nelson, Robert M.; Nicholson, P. D.; Sicardy, B.; Sotin, C.

doi:10.1007/1-4020-3874-7_3

Cited by 113 publications

(167 citation statements)

References 14 publications

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“…These included 5μm measurements taken by the Visual and Infrared Mapping Spectrometer (VIMS, Brown et al, 2004). VIMS is made up of two imaging spectrometers, one covering the visible spectral range (VIMS-V) and the other covering the infrared (VIMS-IR).…”

Section: Vims Data and Calibrationmentioning

confidence: 99%

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Cloud structure and composition of Jupiter’s troposphere from 5-μm Cassini VIMS spectroscopy

Giles

Fletcher

Irwin

2015

Icarus

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Jupiter's tropospheric composition and cloud structure are studied using Cassini VIMS 4.5-5.1 µm thermal emission spectra from the 2000-2001 flyby. We make use of both nadir and limb darkening observations on the planet's nightside, and compare these with dayside observations. Although there is significant spatial variability in the 5-μm brightness temperatures, the shape of the spectra remain very similar across the planet, suggesting the presence of a spectrally-flat, spatially inhomogeneous cloud deck. We find that a simple cloud model consisting of a single, compact cloud is able to reproduce both nightside and dayside spectra, subject to the following constraints: (i) the cloud base is located at pressures of 1.2 bar or lower; (ii) the cloud particles are highly scattering; (iii) the cloud is sufficiently spectrally flat. Using this cloud model, we search for global variability in the cloud opacity and the phosphine deep volume mixing ratio. We find that the vast majority of the 5-μm inhomogeneity can be accounted for by variations in the thickness of the cloud decks, with huge differences between the cloudy zones and the relatively cloud-free belts. The relatively low spectral resolution of VIMS limits reliable retrievals of gaseous species, but some evidence is found for an enhancement in the abundance of phosphine at high latitudes.

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Section: Vims Data and Calibrationmentioning

confidence: 99%

“…The 5-μm data used in this study were obtained using the Visual and Infrared Mapping Spectrometer (VIMS, Brown et al, 2004) on the Cassini spacecraft. In late 2000 and early 2001, Cassini performed a flyby of Jupiter, reaching a closest approach of 9.7 million km (137 Jovian radii) on December 30 2000.…”

Section: Introductionmentioning

confidence: 99%

Cloud structure and composition of Jupiter’s troposphere from 5-μm Cassini VIMS spectroscopy

Giles

Fletcher

Irwin

2015

Icarus

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“…In order to avoid changes to the original spectral signal, this re-projection is performed using the nearest-neighbor algorithm, which merely shifts a single VIMS pixel into the new location but does not interpolate between several VIMS pixels. The rectification and mosaicking process of VIMS cubes is described in detail in Jaumann et al (2006).…”

Section: Observationsmentioning

confidence: 99%

“…Cryovolcanic induced melting (Sotin et al, 2005) can produce a sudden release of large amounts of liquids that form in combination with unconfined material lahar-like mud flows (Fortes and Grindrod, 2006). Within such flows material settles out while flow velocity decreases providing systematic sediment characteristics as observed in the bluish plains.…”

Section: Accepted M Manuscriptmentioning

confidence: 99%

Fluvial erosion and post-erosional processes on Titan

Jaumann

Brown

Stephan³

et al. 2008

Icarus

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The surface of Titan has been revealed by Cassini observations in the infrared and radar wavelength ranges as well as locally by the Huygens lander instruments. Sand seas, recently discovered lakes, distinct landscapes and dendritic erosion patterns indicate dynamic surface processes. This study focus on erosional and depositional features that can be used to constrain the amount of liquids involved in the erosional process as well as on the compositional characteristics of depositional areas. Fluvial erosion channels on Titan as identified at the Huygens landing site and in RADAR and VIMS observations have been compared to analogous channel widths on Earth yielding average discharges of up to 1600 m 3 /s for short recurrence intervals that are sufficient to move centimetre-sized sediment and significantly higher ones for long intervals. With respect to the associated drainage areas, this roughly translates to 1 -150 cm/day runoff production rates with 10 years recurrence intervals and by assuming precipitation this implies 0.6 -60 mm/hr rainfall rates. Thus the observed surface erosion fits with the methane convective storm models as well as with the rates needed to transport sediment. During Cassini's T20 fly-by, the Visible and Infrared Mapping Spectrometer (VIMS) observed an extremely eroded area at 30°W, 7°S with resolutions of up to 500 m/pixel that extends over thousands of square kilometres. The spectral characteristics of this area change systematically, reflecting continuous compositional and/or particle size variations indicative of transported sediment settling out while flow capacities cease. To account for the estimated runoff production and widespread alluvial deposits of finegrained material, release of area-dependent large fluid volumes are required. Only frequent storms with heavy rainfall or cryovolcanic induced melting can explain these erosional features.

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“…More details on the instrument can be found in Brown et al (2004 Table 3), out of which radiative transfer between 157 atmospheric layers is calculated for twenty-two.…”

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confidence: 99%