The stellar lines were identified with the general references A Multiplet Table of Astrophysical Interest (Moore 1945) and Wavelengths and Transition Probabilities for Atoms and Atomic Ions, Part 1 (Reader & Corliss 1980) as well as the more specialized references P II (Svendenius et al. 1983), P III (Magnusson & Zetterberg 1987), Mn II (Iglesias & Velasco 1964), Fe II (Johansson 1978), and Ga II (Isberg & Litzen 1985).
For HR 4487, we used CASLEO spectrograms covering 
and 
. We identified lines of H I, He I, C I, C II,
O I, Mg I, Mg II, Si II, S II, Ca I, Sc II, Ti II, Cr II, Mn II, Fe I, Fe II,
Ni I, Ni II, Sr II, Y II, Zr II, Ba II, Hg I, and possibly Mn I. For 14 Hya
we analyed 
. In this region we found lines of H I, He
I, Mg II, Si II, P II, Ti II, Cr II, Mn I, Mn II, Fe II, and
Y II.
For 3 Cen A we compared our equivalent width values with those by
Jugaku et al. (1961) who used photographic plates
taken with the coudé
spectrograph of the 5-m telescope at Palomar. For 52 metal lines we found
with the equivalent widths in mÅ,
which is fair agreement. As to atomic species they identified lines of H I,
He I, C II, N II, O I, O II, Ne I, Mg II, Si II, Si III, P II, P III, S II,
Ar II, Ca II, Fe II, Fe III, Ni II, Ga II, and Kr II. We did not confirm
those of O I, Ne I, and S II, but this is more a choice of spectral region
and found in addition lines of Cr II and Mn II. Our spectrograms covered
, 
, 
, 
, and 
with a few
minor gaps between orders.