Including all the lines
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  (clic sull'immagine per vederla a dimensione reale)  
  A small section of the solar flux spectrum at 599nm plotted at full scale and at 10-times scale. The heavy black lines show the observed spectrum from the Kitt Peak Solar Flux Atlas from 300 to 1000 nm (Kurucz 2005). The resolving power is about 300000 and the signal-to-noise is about 3000. Higher quality spectra would be helpful because the spectrum is not resolved and because weaker features would appear at higher signal-to-noise. The thin lines are the computed spectra: in red for the solar flux, in blue for the telluric atmospheric transmission, and in purple for their product which should be compared to the observed heavy black lines. The computed spectra are broadened to resolving power 0.05666 cm$^{-1}$ to match the observed spectrum. There are solar lines of Ca I, Ti I, Cr I, Cr II, Fe I, Fe II, Co I, Yb II, C$_2$, CN, and telluric lines of H$_2$O. The first number in each line label is the last 3 digits of the wavelength. The second number is the species code which is the atomic number plus 0.01 times the charge. The middle numbers are either the lower energy level in cm$^{-1}$ for atoms or quantum numbers for molecules. The 4th number is the per mil line depth if the line were computed in isolation. Two of the Co I lines have been divided into hyperfine components. The hyperfine and isotopic splittings have not yet been determined for the other lines. Some splittings may be negligible. There are many missing lines. The lines that are present have been adjusted to improve agreement between the calculated and observed spectra. That process is continuing. This sample will be part of a forthcoming flux atlas with line identifications.  
R.L. Kurucz