Photoelectric search for peculiar stars in open clusters. XV. Feinstein   1, NGC 2168, NGC 2323, NGC 2437, NGC 2547, NGC 4103, NGC 6025, NGC 6633,   Stock 2, and Trumpler 2
  The chemically peculiar (CP) stars of the upper main sequence are mainly characterized by strong overabundances of heavy elements. Two subgroups (CP2 and CP4) have strong local magnetic fields which make them interesting targets for astrophysical studies. This star group, in general, is often used for the analysis of stellar formation and evolution in the context of diffusion as well as meridional circulation. In continuation of a long term study of CP stars (initiated in the 1980ies), we present new results based on photoelectric measurements for ten open clusters that are, with one exception, younger than 235Myr. Observations in star clusters are favourable because they represent samples of stars of constant age and homogeneous chemical composition. The very efficient tool of Delta a photometry was applied. It samples the flux depression at 5200A typically for CP stars. In addition, it is able to trace emission line Be/Ae and lambda Bootis stars. Virtually all CP2 and CP4 stars can be detected via this tool. For all targets in the cluster areas, we performed a kinematic membership analysis. We obtained new photoelectric Delta a photometry of 304 stars from which 207 objects have a membership probability higher than 50%. Our search for chemically peculiar objects results in fifteen detections. The stars have masses between 1.7 M(Sun) and 7.7 M(Sun) and are between the zero- and terminal-age-main-sequence. We discuss the published spectral classifications in the light of our Delta a photometry and identify several misclassified CP stars. We are also able to establish and support the nature of known bona fide CP candidates. The new and confirmed CP stars are interesting targets for spectroscopic follow-up observations to put constraints on the formation and evolution of CP stars. 
E. Paunzen, M. Netopil, H.M. Maitzen, K. Pavlovski, A. Schnell, and M.   Zejda
astro-ph.SR