A spectroscopic survey for λ Bootis stars^*

III. Final results

¹ Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria
² Zentraler Informatikdienst der Universität Wien, Universitätsstr. 7, 1010 Wien, Austria

Received: 3 April 2001
Accepted: 27 April 2001

Abstract

In the third paper of a series dedicated to the spectroscopic survey for new λ Bootis stars, we present all new and confirmed members of the group as well as a detailed analysis of the observed sample. The nature of this small group of chemically peculiar stars of the upper main sequence still challenges our understanding of processes like diffusion, mass-loss and accretion. The typical abundances pattern (nearly solar values for C, N, O and S whereas the Fe-peak elements are moderate to strong underabundant) can still not be explained by any proposed theory. Hence, the significant increase of new members gives the opportunity to investigate the group properties in more detail. We report the discovery of 26 new members of the group and the confirmation of 18 candidates from the literature. This almost triples the number of known λ Bootis stars. The existence of one member in the young open cluster NGC 2264 and four members in the Orion OB1 association proves that the λ Bootis phenomenon already works at very early stages of stellar evolution. Recent results from the Hipparcos mission have shown that the well established λ Bootis stars of the Galactic field comprise the whole area from the Zero Age Main Sequence to the Terminal Age Main Sequence (≈ 10⁹ yr for an A-type star). There is a continuous transition between very young and rather evolved evolutionary stages. We find that the overall percentage of λ Bootis type among all normal type stars in the spectral range from B8 to F4 is 2% in the Galactic field as well as in open clusters. Furthermore, 44 metal-weak objects are listed which might be connected with the λ Bootis phenomenon. Our biased sample (chosen by photometric boxes) is not distinguished from all A-type stars in the corresponding spectral region by the rotational velocity distribution. Only for the luminosity classes IV and III (especially for the cooler program stars) the determined mean v sin i values are very high compared to those of the literature.