A 4 1995AZh....72..855A Antipova L.I., Berdyugina S.V. and Savanov I.S. (1995ARep...39..761A). It is not clear whether the 
  A                       Holweger-Mueller solar model was used in this paper or not (see Holweger H. and Mueller E.A., 
  A                       1974SPh....39...19H). If it was, a zero-point adjustment of the published values of [Fe/H] is required. 
  A                       Further information is awaited.
184   1969CoSka...4...63B Bajcar R. For all EWs, the wavelengths are shortward of 4200 Angstroms.
126   1971JRASC..65..222B akos G.A. For all EWs, the wavelengths are shortward of 4600 Angstroms.
  B 3 1991AZh....68..782B Berdyugina S.V., Boyarchuk M.E., Pavlenko Ya.V., Savanov I.S. and Shavrina A.V. (1992SvA....35..387B) 
  B                       A large temperature correction is required, and the resulting value of [Fe/H] for Alpha Ari has a 
  B                       large residual.
  C 2 1981IzKry..64...13B Boyarchuk A.A. and Eglitis I. (1981BCrAO..64...11B). A large temperature correction is required, and the 
  C                       resulting value of [Fe/H] for Beta Aql has a large residual.
  D 4 1995AZh....72..864B Boyarchuk A.A., Antipova L.I., Boyarchuk M.E. and Savanov I.S. (1995ARep...39..770B).It is not clear 
  D                       whether the Holweger-Mueller solar model was used in this paper or not (see Holweger H. and Mueller E.A.,
  D                       1974SPh....39...19H). If it was, a zero-point adjustment of the published values of [Fe/H] is required. 
  D                       Further information is awaited.
  E 2 1996ARep...40..783B Boyarchuk A.A., Antipova L.I., Boyarchuk M.E. and Savanov I.S. (1996AZh....73..862B). The analysis in 
  E                       this paper is not described in adequate detail.
231   1974CRB...278.1008B Burkhart C. and Van't Veer C. This reference does not appear to exist.
  F 2 1995A&A...297..503C Castilho B.V., Barbuy B. and Gregorio-Hetem J. A zero point for this preliminary report cannot be 
  F                       derived until complete results from these authors are available.  
222 2 ..................C Cayrel de Strobel G, unpublished. No information is available about the wavelength region from which 
222                       these data were derived.
224 2 1970A&A.....7..408C Cayrel de Strobel G., Chauve-Godard J., Hernandez G. and Vaziaga M. Only 8 lines on shoulder and flat 
224                       part of curve of growth are used.
188   1968ApJ...153..169C Cowley C.R. All EWs are from a range of short wavelengths whose upper limit is not known.
  G 2 1995ApJ...439..917D de la Reza R. and da Silva L. This source will be reconsidered when a more extensive discussion of its 
  G                       analysis is published.
  H 2 1994PAZh...20..416G Gopka V.F. and Yushchenko A.V. (1994ApL....20..352G). A result derived by these authors for Alpha Boo 
  H                       disagrees markedly with the catalog value.  See Sec. 5.3 of Taylor B.J., 1998PASP..110..708T. 
414   1983A&A...123..289G Gratton R.G. For all but one star, [Fe/H] is about -0.9dex or less.
550 2 1989A&A...208..171G Gratton R.G. This paper contains a value of [Fe/H] for HD 20038. Gratton has given a parallel result in 
550                       1983A&A...123..289G. The two data differ by 0.5dex. Neither datum is used.
  I 2 1994A&A...287..927G Gratton R.G. and Sneden C. Results from this paper are essentially identical to those by the same authors
  I                       in 1991A&A...241..501G
380 2 1980SvA....24..323K Komarov N.S. and Shcherbak A.N. (1980AZh....57..557K). Results are based only on lines from the flat 
380                       part of the curve of growth.
  J 2 1991A&A...250..451K Krempec-Krygier J., Schmidt M. and Turlo Z. The EWs used by these authors do not extend below the 
  J                       shoulder of the curve of growth.
270 2 1977AcA....27..145K Kuroczkin D. and Wisniewski A. The results in this paper are from subsets of EW data that are analyzed 
270                       in full by other authors.
444   1984ApJ...283..192L Lambert D.L. and Sawyer S.R. Insufficient information is given about the number of lines used.
424 2 1991ApJS...77..515L Luck R.E. and Bond H.E. It is planned to include this source in future catalogs when values of (R-I)c 
424                       are available for all its program stars.
151 3 1974ApJS...27..405O Oinas V. Results from this source are not used because of problems with derived surface gravities and 
151                       continuum placement. (For a discussion of the continuum-placement problems, see Bonnell J. and Branch D.,
151                       1979ApJ...229..175B.)
 22   1963Obs....83..133P Pagel B.E.J. Superseded by Pagel, 1964RGOB...87..227P.
217 2 1976ApJS...30...61P Peterson R.C. Results from this source are not used because of continuum-placement problems. (See 
217                       Bonnell, J., and Branch, D., 1979ApJ...229..175B.)
418 2 1984Thesi.........P Proust D. 1984, thesis. See also Proust D. and Foy R., 1988Ap&SS.145...61P. These data are based on 
418                       log gf values and cannot currently be zeroed to catalog results.
 21 2 1957ApJ...125..123S Schwarzschild M., Schwarzschild B., Searle L. and Meltzer A. Data are from wavelengths shortward of 
 21                       4500 Angstroms and are metallicity indices, not values of [Fe/H].
357 2 1977..............V Vilhu O., Tuominen N., Kyroelaeinen J. and Holsti N. 1977, Obs. Astr. Lab. Univ. Helsinki, Rep. 3. 
357                       Superseded by Kyrolainen J., Tuominen I., Vilhu O. and Virtanen H., 1986A&AS...65...11K.
383   1982ApJ...255..577W Wallerstein G. and Sneden C.  Same as ref. 400.
 16   1965MNRAS.129..263W Warner B. Possible continuum misplacement (see Taylor, 1991ApJS...76..791T; Sec. 3).