Radio Wavelength Observations of Titan with the VLA

Details Radio Wavelength Observations of Titan with the VLA Radio Wavelength Observations of Titan with the VLA

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004dps....36.0604b&link_type=abstract

American Astronomical Society, DPS meeting #36, #06.04; Bulletin of the American Astronomical Society, Vol. 36, p.1075

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Scientific paper

Radio wavelength observations of Titan are a powerful technique for probing through the atmosphere to the surface and subsurface. For more than 20 years, the VLA has been used to observe Titan at wavelengths from 0.7cm to 6cm. A synopsis of these observations will be presented. Three results in particular will be focused on. First, in 1992 seventeen short observations at 3.5cm were used to create a radio light curve for Titan. Preliminary reduction of that data showed no believable light curve (Grossman & Muhleman 1992, BAAS, 24, 954). New reduction, including incorporation of sophisticated algorithms for removing confusing sources (including Saturn), shows a detectable light curve, peaking around 180o longitude, with a peak-to-peak amplitude of ˜10%. The mean brightness temperature of 79.3 ± 2.4 K (including absolute uncertainty) is consistent with that found from the earlier reduction. Second, in 1993 two long observations were performed in an attempt to directly measure the dielectric constant of the surface. The result from those experiments is a dielectric constant of 2.7 ± 1.7. Third, in 1999 three long observations were performed at 0.7cm in an attempt to detect C3H2 in the atmosphere. As a byproduct of these observations, brightness maps at 0.7 and 1.3cm were produced - the highest resolution radio maps of Titan ever made ( ˜0.2''). These and other results will be presented.

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