1. Introduction

For many years the nature of the Bootis stars has been controversial. About 20% of all PopulationI A-type stars show abundance peculiarities. Most of these CP stars are characterized by strong overabundances of iron peak elements (Jaschek & Jaschek 1995). In contrast, the Bootis stars are metal poor, Populaton I, A and early F-type stars. Unfortunately, these astrophysically interesting stars are quite rare; the most recent list of confirmed members (Gray & Corbally 1993) had only 20 members. A recent paper (Paunzen et al. 1997) attempted to expand this number by a critical assessment of the literature resulting in a total of 45 members and candidate members. This small sample of stars still makes a sound statistical analysis difficult. Therefore we have started a spectroscopic survey for new members in the galactic field, open clusters and associations. The discovery of Bootis stars in open clusters and associations is especially important because of the possibility of age determination, thus providing the means to distinguish between the two proposed theories - the diffusion/mass loss theory (Michaud & Charland 1986) and the accretion theory (Venn & Lambert 1990). Candidate Bootis stars were discovered in the Orion OB1 association (three new Bootis stars found), NGC2264 (two candidates) and the galactic field (five new Bootis stars). Additional observations in NGC2232 (age ; Mermilliod 1981) and NGC2301 (age10⁸yr; Mermilliod 1981) yielded a null result. We have been able to confirm a number of the candidate members proposed in Paunzen et al. (1997).