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). We measured CASLEO spectrograms which cover

for

Leo,

for 7 Sex,

for HR 4817, and

for 28 Her. Although these spectra extended further into the blue, we did not utilize these regions as they were too heavily line blanketed at our dispersion for equivalent width comparisons.

For 7 Sex, the previous spectroscopic material consisted of

KPNO CCD spectrograms covering approximately

, and

and a DAO

Reticon spectrogram of

. In the region of overlap

, comparison of the equivalent widths of 18 unblended lines yields

which indicates good agreement except for a minor offset in the zero point.

For

Lep, the previous analysis used coadded

DAO IIaO spectrograms (9 U plates and 11 V plates). Comparison of 17 equivalent widths in the

region yields

and for 28 Her whose previous analysis also used a similar coaddition (14 U and 20 V plates), comparison of 20 equivalent widths in the

region, yields

a result which is in not as good agreement.

For HR 4817, the previous spectroscopic material is

KPNO CCD spectrograms covering approximately

, and

. In the region of overlap

, comparison of the equivalent widths of 18 lines yields

in better agreement than for 7 Sex.

Thus the CASLEO equivalent width scale is marginally larger than that based on KPNO CCD and DAO Reticon spectrograms. The discrepancies with the photographic DAO equivalent widths may well reflect problems with the calibration and continuum placement. But please note that only isolated lines which were typically

and larger were used for the comparison.

**Table 1:** He/H Values
(Å)	Lep	7 Sex	HR 4817	28 Her
4009	0.02	...	...	...
4026	0.03	...	...	0.01
4120	0.03	...	...	...
4144	0.02	...	0.06	...
4388	0.04	0.10	...	0.01
4438	0.03	...	...	0.01
4472	0.02	0.12	0.04	0.02
4713	0.02	0.11	0.04	0.01
4921	0.02	0.08	...	...

average	0.03	0.10	0.05	0.01

**Table 2:** Determination of the microturbulences
Star	Species	gf values	n		log Fe/		log Fe/
				km/s		km/s
7 Sex	Fe I	MF+KX	51	1.7	-4.19 0.25	1.6	-4.19 0.25
		MF	46	1.7	-4.22 0.23	1.7	-4.22 0.23
	Fe II	MF+KX	67	1.5	-4.35 0.26	1.4	-4.33 0.26
		MF	37	1.8	-4.48 0.19	1.8	-4.48 0.19
	adopted			1.7

Lep	Fe II	MF+KX	107	0.2	-4.60 0.24	0.4	-4.61 0.23
		MF	44	0.3	-4.67 0.25	0.4	-4.68 0.28
	adopted			0.3

HR 4817	Fe II	MF+KX	65	0.0	-4.85 0.27	0.0	-4.85 0.27
		MF	25	0.0	-4.94 0.23	0.0	-4.94 0.23
	adopted			0.0

28 Her	Fe I	MF+KX	90	0.0	-4.37 0.31	0.0	-4.37 0.31
			83	0.0	-4.38 0.32	0.0	-4.38 0.32
	Fe II	MF+KX	223	0.2	-4.35 0.22	0.0	-4.35 0.22
		MF	56	0.5	-4.40 0.20	0.5	-4.40 0.20
	adopted			0.2

2. Reduction of spectrograms