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The WFI Hα spectroscopic survey of the Magellanic Clouds: Be stars in SMC open clusters

Published online by Cambridge University Press:  01 July 2008

Christophe Martayan ,
Dietrich Baade  and
Juan Fabregat
Christophe Martayan
Affiliation:
Royal Observatory of Belgium, 3 avenue circulaire 1180 Brussels, Belgium email: [email protected] GEPI, Observatoire de Paris, CNRS, Université Paris Diderot; 5 place Jules Janssen 92195 Meudon Cedex, France
Dietrich Baade
Affiliation:
ESO – European Organisation for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2, D-85748 Garching b. Muenchen, Germany email: [email protected]
Juan Fabregat
Affiliation:
Observatorio Astronómico de Valencia, edifici Instituts d'investigació, Poligon la Coma, 46980 Paterna Valencia, Spain, email: [email protected]
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Abstract

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At low metallicity, B-type stars show lower loss of mass and, therefore, angular momentum so that it is expected that there are more Be stars in the Magellanic Clouds than in the Milky Way. However, till now, searches for Be stars were only performed in a very small number of open clusters in the Magellanic Clouds. Using the ESO/WFI in its slitless spectroscopic mode, we performed a Hα survey of the Large and Small Magellanic Cloud. Eight million low-resolution spectra centered on Hα were obtained. For their automatic analysis, we developed the ALBUM code. Here, we present the observations, the method to exploit the data and first results for 84 open clusters in the SMC. In particular, cross-correlating our catalogs with OGLE positional and photometric data, we classified more than 4000 stars and were able to find the B and Be stars in them. We show the evolution of the rates of Be stars as functions of area density, metallicity, spectral type, and age.

Keywords

techniques: spectroscopicsurveysstars: emission-lineBegalaxies: individual (SMC)Magellanic Cloudsgalaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S256: The Magellanic System: Stars, Gas, and Galaxies , July 2008 , pp. 349 - 354
Copyright
Copyright © International Astronomical Union 2009

References

Baade, D., Meisenheimer, K., Iwert, O., et al. 1999, The Messenger, 95, 15Google Scholar
Bertin, E. & Arnouts, S. 1996, A&AS, 117, 393Google Scholar
Fabregat, J. & Torrejón, J. M. 2000, A&A, 357, 451Google Scholar
Kudritzki, R. P., Pauldrach, A., & Puls, J. 1987, A&A, 173, 293Google Scholar
Lang, K. R. 1992, Astrophysical Data, Springer VerlagCrossRefGoogle Scholar
Maeder, A., Grebel, E. K., & Mermilliod, J.-C. 1999, A&A, 346, 459Google Scholar
Martayan, C., Frémat, Y., Hubert, A.-M., et al. 2007, A&A, 462, 683Google Scholar
Martayan, C., Floquet, M., Hubert, A.-M., et al. 2008a, A&A, 489, 469Google Scholar
Martayan, C., Baade, D., Hubert, A.-M., et al. 2008b, The 2007 ESO instrument calibration workshop, p. 595Google Scholar
McSwain, M. V. & Gies, D. R. 2005, ApJS, 161, 118CrossRefGoogle Scholar
Meyssonnier, N. & Azzopardi, M. 1993, A&AS, 102, 451Google Scholar
Pietrzyński, G. & Udalski, A. 1999, AcA, 49, 157Google Scholar
Porter, J. M. & Rivinius, T. 2003, A&A, 115, 1153Google Scholar
Udalski, A., Szymański, M., Kubiak, M., et al. 1998, AcA, 48, 147Google Scholar
Udalski, A. 2000, AcA, 50, 279Google Scholar
Wallace, P. T. & Gray, N. 2003, User guide of ASTROMGoogle Scholar
Wisniewski, J. P. & Bjorkman, K. S. 2006, ApJ, 652, 458CrossRefGoogle Scholar
Zorec, J. & Frémat, Y. 2005, SF2A-2005: Semaine de l'Astrophysique Française, p. 361Google Scholar