Abstract

A method to detect the acoustic oscillation spectrum of giant planets and stars exploits the multiplex properties of a Fourier-transform spectrometer (FTS). It is based on measurement of the small Doppler shift related to the oscillation of the atmosphere measured from all the lines in a portion of the planetary or the stellar spectrum directly from the interferogram. The resulting amplitude modulation of the output signal is recorded continuously over several consecutive nights at a fixed path difference selected from criteria of optimum efficiency. Hence the Fourier transform of this signal yields the pressure-mode spectrum of the object. Applications to Jupiter, Saturn, and Procyon, observed in this mode with the step-scan FTS installed in the Canada–France–Hawaii Telescope, are presented. Future projects are discussed.

© 1996 Optical Society of America

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Infrared Spectroscopy of Planets and Stars

William M. Sinton
Appl. Opt. 1(2) 105-110 (1962)

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