Volume 404, Number 2, June III 2003
|Page(s)||749 - 762|
|Section||Atomic, molecular, and nuclear data|
|Published online||02 June 2003|
Accurate atomic parameters for near-infrared spectral lines
Max–Planck Institut für Aeronomie, 37191 Katlenburg-Lindau, Germany
2 Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany
3 Uppsala Astronomical Observatory, Box 515, 751–20 Uppsala, Sweden
4 Instituto de Astrofísica de Andalucía, CSIC, Apdo. de Correos 3004, 18080 Granada, Spain
Corresponding author: J. M. Borrero, firstname.lastname@example.org
Accepted: 10 April 2003
A realistic two-component model of the quiet solar photosphere is used to fit the intensity spectrum of the Sun in the wavelength range 0.98–1.57 μm. Our approach differs from earlier attempts in many respects: proper account of convective inhomogeneities is made, accurate collisional broadening parameters from quantum mechanical computations are used, and the effects of possible blends in the local continuum are corrected empirically. This allows us to derive oscillator strengths and central wavelengths for virtually any unblended line of the solar spectrum. The accuracy of the inferred atomic parameters, about 0.06 dex for oscillator strengths and 5 mÅat 1 μm for central wavelengths, is similar to that of the best laboratory measurements. We apply our method to 83 near-infrared lines belonging to 6 different atomic species. The availability of accurate oscillator strengths and central wavelengths for lines of different species is essential for the interpretation of high resolution spectroscopic observations. The method is especially useful in the infrared, a wavelength domain where laboratory measurements are scarce.
Key words: atomic data / line: profiles / Sun: abundances / stars: abundances
© ESO, 2003
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