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The influence of spectral resolution on line blending and wavelength positions in the solar UV spectrum

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Abstract

For representative sections of the solar UV spectrum (λ 2765 Å–λ 2790 Å, λ 2765 Å–λ 2805 Å) the line density and the accuracy of wavelength positions of absorption features are derived as function of the spectral resolution. In low resolution spectrograms unresolved blends may shift intrinsic wavelength positions of absorption lines by amounts up to a few tenths of the spectral resolution.

The results obtained for the solar spectrum are applied to the flux spectrogram of αCMi.

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Authors and Affiliations

  1. Max Planck Institut für Radioastronomie, Bonn, F.R.G.

    A. Greve

  2. Physics Department, Queen's University, Belfast, Northern Ireland

    C. D. McKeith

Authors
  1. A. Greve
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  2. C. D. McKeith
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Additional information

Guest Investigator in the BUSS Program jointly performed by the Space Research Laboratory, Utrecht, The Netherlands, and the NASA L. B. Johnson Space Center, Houston, U.S.A.

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Greve, A., McKeith, C.D. The influence of spectral resolution on line blending and wavelength positions in the solar UV spectrum. Sol Phys 65, 405–409 (1980). https://doi.org/10.1007/BF00152803

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  • DOI: https://doi.org/10.1007/BF00152803

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