Our sample is composed by 180 stars and was selected essentially from the list of Hynek (1938).
Additional objects come from Markowitz (1969), Cowley (1973, 1976),
Hoffleit & Jaschek (1982)
and Stickland (1988). Our sample is contained essentially within the
observational limits V<10 and
. We have excluded all objects which, according to Hynek, are dubious, but we have
included his class VI objects which are mainly Am stars.
Among the 180 stars we have found a number of Am stars and objects hotter than G0 (but with no trace of a hot companion). We are left thus with 120 composite spectra, of which 106 come from Hynek, for which we provide the classification of the cooler component. These stars are listed in Table 1 (click here). As can be seen from a perusal of the table, a certain number of stars has been classified several times in the past (often with widely different results), whereas for others we have been unable to find more than the Henry Draper (HD) classification.
The 25 Am stars and the 35 objects with hot spectra (types B to F) are listed in Table 2 (click here).
In both tables SP denotes spectral classifications given by other authors, whereas SP(IR) denotes our own classifications. Positions, V and B-V values, as well as the bibliographic references given in the tables were provided by the Centre de Données Stellaires (CDS). An asterisk refers to a footnote. A + or - sign following the SP(IR) luminosity class indicates that the object is probably slightly more or less luminous.