Other
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.4707b&link_type=abstract
American Astronomical Society, DPS meeting #39, #47.07; Bulletin of the American Astronomical Society, Vol. 39, p.506
Other
Scientific paper
The VIMS instrument aboard the Cassini Spacecraft has a solar port and an occultation mode to observe solar or stellar occultations by Saturn, its rings, and Titan.
Occultations are observed as absorption occultations, due to the proximity of the planet, contrary to the refractive occultations observed from the ground: In the case of VIMS, refraction becomes significant below the 100 km altitude level.
The VIMS solar port was used to observed a solar occultation by the southern hemisphere of Titan on January 15th, 2006. The occultation mode was used on January 29th, 2007 for the ingress of star Gamma Crucis at a latitude about 25°N on Titan.
For both events, the Infrared spectra acquired at different altitudes show several absorption bands of CH4 (1.7 µm, 2.3 µm, 3.2 µm).
In the solar occultation data, the 2.3-µm band system of CH4 is well fitted by models with a uniform profile of 1.83 ±0.3% CH4, in agreement with other measurements.
In those data, the CO band at 4.7 µm is detected below 180 km. Attempts to best fit the data and retrieve a vertical profile will be presented.
This CO absorption is not detected in the stellar occultation data because of the lower signal to noise ratio than in the solar occultation.
In both events, a deep absorption feature at 3.4 µm is seen, blended with the 3.3 µm CH4 band. No gaseous absorbents can fit this feature. Although not identified yet, this absorption might be due to haze particles in the atmosphere.
Baines Kevin Hays
Bellucci Aurelie
Brown Harvey R.
Buratti Bonnie Jean
Cassini/VIMS Team
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