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Signal-to-Noise Ratio and Astronomical Fourier Transform Spectroscopy

Published online by Cambridge University Press:  19 July 2016

J. P. Maillard
J. P. Maillard*
Affiliation:
Institut d'Astrophysique de Paris, 98bis Bld Arago, 75014 Paris (France)

Abstract

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The multiplex properties of the Fourier Transform Spectrometer (FTS) can be considered as disadvantageous with modern detectors and large telescopes, the dominant noise source being no longer in most applications the detector noise. Nevertheless, a FTS offers a gain in information and other instrumental features remain: flexibility in choosing resolving power up to very high values, large throughput, essential in high–resolution spectroscopy with large telescopes, metrologic accuracy, automatic substraction of parasitic background. The signal–to–noise ratio in spectra can also be improved: by limiting the bandwidth with cold filters or even cold dispersers, by matching the instrument to low background foreoptics and high–image quality telescopes. The association with array detectors provides the solution for the FTS to regain its full multiplex advantage.

Type
I. Spectrographs, Detectors, Fourier Transform Spectroscopy, and Radial Velocities
Information
Symposium - International Astronomical Union , Volume 132: The Impact of Veryhigh S/N Spectroscopy on Stellar Physics , 1988 , pp. 71 - 78
Copyright
Copyright © Kluwer 1988 

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