Working with Cassini VIMS

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Contents

[edit] About Cassini VIMS (Visible and Infrared Mapping System)

[edit] Instrument Overview

VIMS (also known as the Visible and Infrared Mapping System) maps the color properties of the atmospheres of Saturn and Titan, the surfaces of the moons, and the rings in order to study their composition and structure.

See: The Cassini Mission


[edit] Technical Details

VIMS consists of two camera instruments, a "pushbroom" mapping spectrometer that studies visible light (VIMS-VIS) and a "whiskbroom" mapping spectrometer for infrared light (VIMS-IR).

VIMS "image cubes" contain information on 352 different wavelengths of light from ultraviolet to the mid-infrared. The visible channel produces multispectral images spanning the spectral range 0.3-1.05 micrometers over 96 spectral bands. The infrared channel covers the wavelength range 0.85-5.1 micrometers over 256 spectral bands.

This is much higher spectral resolution than the Imaging Science Subsytem ISS, but the spatial resolution of VIMS is approximately 100 times lower than the resolution of ISS.


[edit] References & Related Resources


[edit] Cartographic Processing VIMS Data

[edit] Level 0 Processing

  1. Data Acquisition
  2. Ingestion
  3. SPICE
  4. Raw Camera Geometry


[edit] Level 1 Processing

  1. VIMS Radiometric Calibration
  2. Display a VIMS cube

[edit] Level 2 Processing

Overview of Map Projecting Images

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