Solar occultation observations by the Visual and Infrared Mapping Spectrometer (VIMS) aboard Cassini provide detailed information about Titan’s atmospheric structure and composition. As the Sun passed behind Titan as viewed from Cassini, VIMS recorded how sunlight was absorbed and scattered at different altitudes.

Dataset Information

Property Value
Source Cassini VIMS
Target Titan atmosphere
Type Solar occultation spectra
Wavelength 0.35–5.1 μm

Scientific Background

Titan’s thick atmosphere is rich in nitrogen, methane, and complex organic molecules. Solar occultations allow us to measure the vertical distribution of these species and study atmospheric haze layers with high precision. By probing Titan’s atmospheric transmission, we were able to more clearly “see” Titan’s surface and determine its composition. This approach revealed an icy surface, similar in composition to other icy satellites, but with an imprint of precipitated hydrocarbon particles.

Dataset Contents

This dataset includes processed VIMS solar occultation spectra with:

  • Calibrated transmission spectra as a function of altitude
  • Retrieved atmospheric profiles
  • Associated geometric and timing information

Detailed format documentation to be provided with data release.

Status

Coming soon: This dataset is being prepared for public release.

Further information:

  • Hayne, P. O., McCord, T. B., & Sotin, C. (2014). Titan's surface composition and atmospheric transmission with solar occultation measurements by Cassini VIMS. Icarus, 243, 158–172. Link
  • McCord, T. B., Hayne, P., et al. (2008). Titan's surface: Search for spectral diversity and composition using the Cassini VIMS investigation. Icarus, 194, 212–242. Link