FE-I LINES IN LATE-TYPE STELLAR UV SPECTRA

It has been suggested that Fe I lines may constitute a major part of t he many absorption lines observed in the (near-UV) solar spectrum and in those of late type stars. We use the table of Fe I lines recently m easured in the laboratory by Nave et al. (1994) and examine the solar spectrum between 2756 - 2831 A observed by us previously with the high est spectral resolution to date, R = 1.75 10(5). We exploit this exist ing observation since only such high spectral resolution allows suffic ient isolation of weak lines in an underlying haze of absorption featu res. In this solar spectrum we detect similar to 90% of the tabulated Fe I lines. Investigations of this kind are relevant, for instance, to primordial abundances of beryllium and boron in late type metal poor halo stars requiring complete model atmosphere line opacities and disc rimination of possible line blending. We illustrate the case of Be wit h the spectrum of the late type star HD 165908 observed with R approxi mate to 5 10(4).