Table B.2: Observable spectral lines in red and blue channel. aWavelengths, Pierce & Breckenridge (1974). b Effective Landé factor, Solanki et al. (1987). c Height of line core formation above $\tau _{\rm 500nm}=1$. d all values in this section from J. Bruls (personal note). e Values from H. Schleicher (personal note). f Nave et al. (1994).
Element $\lambda$ Transition gj $\Delta h^{c}$
  [nm] 2S+1LJ   [km]
Solar absorption linesd, CCD 2
Ca II H 396.849 2S 0.5 - 2P0.5 1.33 1480-2130
Fe I 396.452 3P 1 - 5P2 2.00 110-320
Fe If 396.551 5D 3 - 5D4   -
Fe I 396.607 3F 2 - 3D3 2.00 350-520
Fe If 396.665 5D 0 - 5F1   -
Fe If 396.681 3D 2 - 5F1   -
Fe I 396.745 3H 4 - 1G3 0.75 270-450
Fe I 396.792 5D 3 - 3G4 1.00 280-510
Fe I 396.918 3F 4 - 3F3 1.50 510-630
Fe If 396.963 3D3 - 3H4   -
Solar absorption lines, CCD 1
Fe I 630.151a 5P2 - 5D2 1.67b 300-500e
Fe I 630.250a 5P1 - 5D0 2.50 200-460e
Fe I 630.346 5G6 - 5G5   -
Ti I 630.375 3F3 - 3G3    
Telluric absorption lines, CCD 1
O2 630.200a - - earth atm.
O2 630.276a - - earth atm.


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