Poster
P. Machado, A. Ribeiro
Abstract
With the end of the Cassini-Huygens mission, the only way to obtain information about the chemical and physical properties of the atmosphere of Titan is through ground base observations. Through high-resolution spectroscopy one can probe the atmosphere of the moon at different optical depths based on the wavelength, get its chemical signatures, construct the temperature and pressure profile and constrain its physical properties. The IA's High-Resolution Spectroscopy pipeline is able to produce these high -resolution spectra and measure winds through the Doppler velocimetry method with high quality results, by calculating the wavelength Doppler shift, due to the winds, between the spectrum corresponding to the central pixel and the spectra from the remaining pixels the target occupies in along the slit. This work is the learning and adaptation of the pipeline to the case of Titan using the dedicated VLT-UVES observations with the blue arm in collaboration with the University of Bordeux, the use of the HITRAN and ExoMol databases for the retrieval of relevant chemical species expected to be found in Titan's atmosphere within the UVES blue arm wavelength range and the learning and use of the NEMESIS Radiative Transfer model in order to obtain the temperature and pressure profiles and constrain the altitude level.
XXIX Encontro Nacional de Estudantes de Astronomia
Lisboa, Portugal
2019 September
