SCYON Abstract

Received on September 27 2006

Be stars in open clusters in the Small Magellanic Cloud.

AuthorsC. Martayan (1,2), D. Baade (1), A.-M. Hubert (2), M. Floquet (2), J. Fabregat (3), E. Bertin (4), and C. Neiner (2)
Affiliation
(1) European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching b. München, Germany
(2) GEPI, UMR8111 du CNRS, Observatoire de Paris-Meudon, 92195 Meudon Cedex, France
(3) Observatorio Astronómico de Valencia, edifici Instituts d'investigació, Poligon la Coma, 46980 Paterna Valencia, Spain
(4) Institut d'Astrophysique de Paris (IAP), 98bis boulevard Arago, 75014 Paris
To appear inSF2A2006
Contactchristophe.martayan@obspm.fr
URLhttp://arxiv.org/abs/astro-ph/0609678
Links NGC 346 / OGLE-SMC2 / OGLE-SMC8 / OGLE-SMC9 / OGLE-SMC11 / OGLE-SMC12 / OGLE-SMC13 / OGLE-SMC15 / OGLE-SMC16 / OGLE-SMC17 / OGLE-SMC18 / OGLE-SMC19 / OGLE-SMC20 / OGLE-SMC25 / OGLE-SMC32 / OGLE-SMC33 / OGLE-SMC38 / OGLE-SMC39 / OGLE-SMC43 / OGLE-SMC47 / OGLE-SMC49 / OGLE-SMC54 / OGLE-SMC59 / OGLE-SMC61 / OGLE-SMC64 / OGLE-SMC66 / OGLE-SMC67 / OGLE-SMC68 / OGLE-SMC69 / OGLE-SMC70 / OGLE-SMC71 / OGLE-SMC72 / OGLE-SMC73 / OGLE-SMC74 / OGLE-SMC75 / OGLE-SMC76 / OGLE-SMC77 / OGLE-SMC78 / OGLE-SMC81 / OGLE-SMC82 / OGLE-SMC83 / OGLE-SMC89 / OGLE-SMC90 / OGLE-SMC92 / OGLE-SMC98 / OGLE-SMC99 / OGLE-SMC104 / OGLE-SMC105 / OGLE-SMC107 / OGLE-SMC109 / OGLE-SMC112 / OGLE-SMC115 / OGLE-SMC117 / OGLE-SMC118 / OGLE-SMC120 / OGLE-SMC121 / OGLE-SMC124 / OGLE-SMC126 / OGLE-SMC128 / OGLE-SMC129 / OGLE-SMC134 / OGLE-SMC137 / OGLE-SMC138 / OGLE-SMC139 / OGLE-SMC140 / OGLE-SMC141 / OGLE-SMC142 / OGLE-SMC143 / OGLE-SMC144 / OGLE-SMC145 / OGLE-SMC146 / OGLE-SMC147 / OGLE-SMC149 / OGLE-SMC153 / OGLE-SMC155 / OGLE-SMC156 / OGLE-SMC160 / OGLE-SMC177 / OGLE-SMC187 / OGLE-SMC194 / OGLE-SMC195 / OGLE-SMC198 / OGLE-SMC200 / OGLE-SMC210

Abstract

We report on the study of the population of B and Be stars in SMC young clusters, performed with the Wide Field Imager in slitless spectroscopic mode at ESO/T2.2m with a filter centered at Hα. First, we explain the reduction methods we used and our selection of different types of objects. Second, we present results on the proportion of Be stars in 85 SMC clusters, and we compare this proportion to the one observed in the Milky Way. Finally, we also present results on a statistical study of variability of Be stars with OGLE.