the literature with their references, and adopted log gf values. The lines were fitted to the solar high resolution observations using the same UVES spectrograph [^5] as the present sample of spectra, to spectra from Arcturus (Hinkle et al. 2000), and from the metal-rich giant $\mu$ Leo, with spectra observed with the ESPaDOns/CFHT spectrograph, at a resolution of R $\sim$ 80 000 and a S/N $\sim$ 500 (Lecureur et al. 2007). The fits of 4810.529 and 6362.339 [Å]{} lines in these reference stars are presented in Fig. \[sun\].

Autoionization of lines
-----------------------

The measurement of the 6362.350 line has to take a continuum lowering in the range $\sim$6360.8 - 6363.1 [Å  into account]{}, owing to the 6361.940 auto-ionization line. Mitchell & Mohler (1965) identified depressions that are $\sim$2.6 [Å]{} wide at the locations of the multiplet lines at 6318, 6343, and 6363 [Å]{}, which are caused by auto-ionizing transitions 3d4p 3F$^{\circ}$ - 3d4d 3G. Following the recipe that Lecureur et al. (2007) used for the 6318 [Å]{} line, we adjusted the radiative broadening factor for the 6363 [Å]{} line to match the line profile to standard stars (Sun, Arcturus, $\mu$ Leo), as well as to sample stars, thus taking the 