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A tool for modelling telluric spectra

Published online by Cambridge University Press:  21 October 2010

Alain Smette
Affiliation:
ESO, Alonso de Cordova 3107, Casilla 19001, Vitacura Santiago, Chile email: [email protected]
Hugues Sana
Affiliation:
ESO, Alonso de Cordova 3107, Casilla 19001, Vitacura Santiago, Chile email: [email protected] Universiteit van Amsterdam, Sterrenkundig Instituut ‘Anton Pannekoek’, Postbus 94249, – NL-1090 GE Amsterdam, The Netherlands email: [email protected]
Hannes Horst
Affiliation:
ESO, Alonso de Cordova 3107, Casilla 19001, Vitacura Santiago, Chile email: [email protected] now at EOS GmbH - Electro Optical Systems, Niederlassung Chemnitz, Annaberger Strasse 240, D-09125 Chemnitz, Germany email: [email protected]
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Accurate synthetic telluric spectra are required for efficient use of telescope time, in particular, with large telescopes and high-resolution NIR spectroscopy: (i) In the preparation of observations, are the telluric features at the same wavelength as spectroscopic features of scientific interest? Since water vapor is the molecule whose abundance varies most in the atmosphere, what values of precipitable water vapor are suitable to carry out successful observations? Are the observations of a telluric star required? Or better, can telluric features in the science spectrum be accurately represented by an appropriate synthetic spectrum? This point is also very important in the planning of telescope time, as observations of a telluric star may sometimes take longer than the one of the science target. (ii) In the analysis of the observations, how do telluric lines affect the scientifically interesting features in the observed spectrum? Is it possible to recover the useful information when telluric star observations could not be obtained, do not have sufficient SNR, or suffer from a significant change in instrumental or observing conditions?

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2010

References

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