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Description of an observational method for determining absolute intensities in the solar spectrum between λ 2962 Å and λ 4087 Å

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Abstract

The results of measurements of absolute intensities in the spectrum of the centre of the sun's disk in the wavelength region 2977–4087 Å have already been published (Houtgast 1965, 1968) and use has been made of them on different occasions. The intensities at 206 spectral points have been given, chosen as much as possible between the Fraunhofer lines, but well divided over the region. Each strip of the Utrecht (Minnaert et al., 1940) and Göttingen (Brückner, 1960) Atlases contains at least two points. Later (Houtgast and Namba, 1968) four more points were added below λ 2977 Å.

In order to judge the reliability of the published intensities one requires a description of the observational method. This description includes the apparatus, the correction for atmospheric extinction and the number of observations from which the final mean values of the absolute intensities are deduced. Finally a discussion of the most important sources of error is given.

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  1. The Astronomical Institute, Utrecht, The Netherlands

    J. Houtgast

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  1. J. Houtgast
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Houtgast, J. Description of an observational method for determining absolute intensities in the solar spectrum between λ 2962 Å and λ 4087 Å. Sol Phys 15, 273–287 (1970). https://doi.org/10.1007/BF00151832

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  • DOI: https://doi.org/10.1007/BF00151832

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