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7. Conclusions

We built two samples of stars: one of them made up of CP2 stars and the other of normal stars. The application of the Multiple Discriminant Analysis gave a combination of the Strömgren-Crawford photometric indices which was able to optimally distinguish both samples. The analysis was conducted separately for the early, intermediate and late photometric regions defined by Strömgren. We used both observed and reddening free indices. The best result was obtained, for the early region, using the observed indices as variables to characterize the unreddened populations (Eqs. (1) and (2)). For these stars, a peculiarity level of tex2html_wrap_inline1785 detects 50% of the CP2 stars with a contamination of around 2%. Furthermore, tex2html_wrap_inline1701 presented a high correlation with peculiarity indices in other photometric systems, such as tex2html_wrap_inline1533 and tex2html_wrap_inline1857.

The ability of tex2html_wrap_inline1701 to detect peculiar stars is smaller than that of the tex2html_wrap_inline1533 or tex2html_wrap_inline1857 indices. This was not unexpected, because they specifically measure the depression at tex2html_wrap_inline1515. However, the efficiency of tex2html_wrap_inline1701 was higher than that of tex2html_wrap_inline1943 or tex2html_wrap_inline1945 used elsewhere.

For the intermediate and late regions, even though a small separation between peculiar and normal stars was present, the correlation of tex2html_wrap_inline1701 index with tex2html_wrap_inline1533 was very poor. New observations enlarging the sample of cool peculiar stars with available tex2html_wrap_inline1475 photometry are needed in order to carry out a more accurate study of these stars. On the other hand, tex2html_wrap_inline1701 cannot discriminate between cool CP2 stars and Am stars.

A list of 60 new early CP2 candidates among those stars with only tex2html_wrap_inline1475 measurements was proposed.

Finally, the difference between the E(b-y) of CP2 stars computed from the calibrations suitable for normal stars and the actual E(b-y) was shown to correlate with the peculiarity index tex2html_wrap_inline1701 (Eq. (7)).


This work was supported by the CICYT under contract ESP95-0180 and by the Ayudas para la utilización de recursos científicos de carácter especıfico by the DGICYT. We should like to thank X. Luri for his kind collaboration in performing the observations in September 1995. We thank Prof. C. Jaschek for his comments on an earlier draft of this paper and Dr. J.-C. Mermilliod for providing us with the latest version of Geneva's photometric catalogue. The authors also thank the referee, Dr. P. North, whose comments have contributed greatly to the paper.

The 1.52 m telescope is operated by the Observatorio Astronómico Nacional in the Calar Alto Observatory of the Centro Astronómico Hispano-Alemán. The 50 cm Danish telescope is operated by the ESO in La Silla Observatory.

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