The Visual and Infrared Mapping Spectrometer for Cassini

  title={The Visual and Infrared Mapping Spectrometer for Cassini},
  author={Edward A. Miller and Gail Klein and David W. Juergens and Kenneth Mehaffey and Jeffrey M. Oseas and Ramon A. Garcia and Antonio Di Giandomenico and Robert E. Irigoyen and Roger Hickok and David Rosing and Harold R. Sobel and Carl F. Bruce and Enrico Flamini and Romeo DeVidi and Francis M. Reininger and Michele Dami and Alain Soufflot and Y. Langevin and Gerard Huntzinger},
  booktitle={Optics \& Photonics},
The visual and infrared mapping spectrometer (VIMS) is a remote sensing instrument developed for the Cassini mission to Saturn by an international team representing the national space agencies of the United States, Italy, and France. A dual imaging spectrometer, VIMS' unique design consists of two optical systems boresighted and operating in tandem, coordinated by a common electronics unit. The combined optical system generates 352 2D images simultaneously, each in a separate, contiguous… 
Observations with the Visual and Infrared Mapping Spectrometer (VIMS) during Cassini's flyby of Jupiter
Abstract The Cassini Visual and Infrared Mapping Spectrometer (VIMS) is an imaging spectrometer covering the wavelength range 0.3–5.2 μm in 352 spectral channels, with a nominal instantaneous field
The Cassini Visual And Infrared Mapping Spectrometer (Vims) Investigation
The Cassini visual and infrared mapping spectrometer (VIMS) investigation is a multidisciplinary study of the Saturnian system. Visual and near-infrared imaging spectroscopy and high-speed
Optical design of a compact imaging spectrometer for planetary mineralogy
We present the design of a compact, wide-angle pushbroom imaging spectrometer suitable for exploration of solar system bodies from low orbit. The spectrometer is based on a single detector array with
Observations in the Saturn system during approach and orbital insertion, with Cassini's visual and infrared mapping spectrometer (VIMS)
The Visual and Infrared Mapping Spectrometer observed Phoebe, Iapetus, Titan and Saturn's rings during Cassini's approach and orbital insertion. Phoebe's surface contains water ice, CO 2 , and
MWIR imaging spectrometer with digital time delay integration for remote sensing and characterization of solar system objects
An MWIR TDI (Time Delay and Integration) Imager and Spectrometer (MTIS) instrument for characterizing from orbit the moons of Jupiter and Saturn is proposed. Novel to this instrument is the planned
Titan’s surface composition and atmospheric transmission with solar occultation measurements by Cassini VIMS
Abstract Solar occultation measurements by the Cassini Visual and Infrared Mapping Spectrometer (VIMS) reveal the near-infrared transmission of Titan’s atmosphere down to an altitude of ∼40 km. By
AOTF-Based Spectral Imaging for Balloon-Borne Platforms
A balloon-borne Acousto-Optic Tunable Filter (AOTF) hyperspectral imager is ideally suited to address numerous outstanding questions in planetary science. The spectral agility, narrowband wavelength
Correlations between VIMS and RADAR data over the surface of Titan: Implications for Titan’s surface properties
Abstract We apply a multivariate statistical method to Titan data acquired by different instruments onboard the Cassini spacecraft. We have searched through Cassini/VIMS hyperspectral cubes,
Near-infrared spectroscopy of Himalia
Abstract We present the first spectrum through the L band of an irregular satellite from the outer Solar System. Spectra of Himalia (JVI) were obtained with the Visual and Infrared Mapping
The visual spectrum of Jupiter's Great Red Spot accurately modeled with aerosols produced by photolyzed ammonia reacting with acetylene
Abstract We report results incorporating the optical properties of the red-tinted photochemically-generated aerosols of Carlson et al. (2016, Icarus 274, 106–115) in spectral models of Jupiter's


Near-Infrared Mapping Spectrometer For Investigation Of Jupiter And Its Satellites
The Near-Infrared Mapping Spectrometer (NIMS) is one of the science instruments in the Galileo Mission, which will explore Jupiter and its satellites in the early-1990's. The NIMS experiment will map
Visible And Infrared Mapping Spectrometer (VIMS): A Facility Instrument For Planetary Missions
Infrared mapping spectrometry, a new remote sensing tool in which a scene is imaged simultaneously in hun-dreds of wavelengths, will be used on several approved planetary missions. A
Visible and infrared mapping spectrometer for exploration of comets, asteroids, and the saturnian system of rings and moons
The science objectives and system design for a Visible and Infrared Mapping Spectrometer (VIMS), an imaging spectrometer for planetary exploration, are described. The instrument development is the
Remote mineralogy through multispectral imaging: the VIMS-V instrument
The Visible Infrared Mapping Spectrometer--Visible Channel (VIMS-V) has been designed to produce high resolution multispectral images, in the optical waveband, of different planetary bodies. VIMS-V,
Visible Infrared Mapping Spectrometer--visible channel (VIMS-V)
The VIMS-V is a passive remote sensing instrument under development for the Italian Space Agency to perform high resolution spectral imaging in the optical waveband. Its unique design relies
Near-Infrared Mapping Spectrometer Optical Subsystem Development and Testing
  • S. Macenka
  • Physics, Engineering
    Optics & Photonics
  • 1984
The Near-Infrared Mapping Spectrometer (NIMS) is one of the four remote-sensing science instruments of the Galileo Orbiter scientific payload. The NIMS scientific objectives re-quire operating the
Stellar occultation experiment with the CASSINI VIMS instrument
The VIMS instrument (Visible and Infrared Mapping Spectrometer) will be flown in the late 1990s on the CASSINI mission to Saturn and its moons. VIMS is designed to generate two-dimensional
Results from the ISM experiment
THE imaging spectrometer ISM, operating in the near infrared, is the first ever flown in space for planetary observation. With a spectral range of 0.76–3.14μm, its main goals were to obtain
Algorithms for a very high speed universal noiseless coding module
The algorithmic definitions and performance characterizations are presented for a high performance adaptive coding module. Operation of at least one of these (single chip) implementations is expected
Infrared Mapping Spectrometer Subsystem Description," Vol.VII
  • 1990