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Titan's surface albedo from ground based near-infrared spectra and the influence of modeling parameters

Abstract

Titan has been observed with the Fourier Transform Spectrometer (FTS) atthe Canada France Hawaii Telescope (CFHT), the Infrared Spectrometer AndArray Camera (ISAAC) at the ESO Very Large Telescope (VLT) and the NACOadaptive optics system, also at the VLT. These observations were performedfrom 1991 to 2005 and between 0.8 and 2.5 microns. This dataset allowedus to explore five methane windows at 0.94, 1.08, 1.28, 1.58 and 2 micronsat different longitudes and resolutions. The effect of the methaneabsorption coefficients in the modeling and its influence on the retrievalof surface albedos was investigated by performing a comparative study ofthe methane absorption coefficients currently available from differentsources. The obtained surface albedo shows to be very dependent on thecoefficients used, with obvious consequences to the anlysis ofTitan'ssurface composition. Also, the NACO observations, taken two days afterHuygens landing, allowed us to retrieve the surface albedo of theHuygenslanding site as well as of surrounding dark and bright areas. These resultswere then compared with the spectra of possible constituents of Titan'ssurface.
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Dates and versions

insu-00364691 , version 1 (26-02-2009)

Identifiers

  • HAL Id : insu-00364691 , version 1

Cite

A. Negrao, A. Coustenis, M. Hirtzig, E. Lellouch, J.-P. Maillard, et al.. Titan's surface albedo from ground based near-infrared spectra and the influence of modeling parameters. 2006-AOGS 3rd Annual General Assembly, Jul 2006, Singapour, Malaysia. ⟨insu-00364691⟩
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