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Astron. Astrophys. 352, L31-L35 (1999)

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Letter to the Editor

A spectroscopic study of Be stars in the SMC cluster NGC 330 *

W. Hummel 1, T. Szeifert 2,3, W. Gässler 1, B. Muschielok 1, W. Seifert 2, I. Appenzeller 2 and G. Rupprecht 4

1 Institut für Astronomie und Astrophysik und Universitätssternwarte München, Scheinerstrasse 1, D-81673 München, Germany
2 Landessternwarte Heidelberg, Königsstuhl 12, D-69117 Heidelberg, Germamy
3 ESO Santiago, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile
4 ESO, Karl-Schwarzschild-Strasse 2, D-85745 Garching, Germany

Received 12 August 1999 / Accepted 7 September 1999


We present a spectroscopic study of early type emission line stars in the field of the young open SMC cluster NGC 330 which have been identified as Be stars by CCD imaging photometry by Grebel et al. (1992). 18 of the 20 program stars investigated can be confirmed to show Balmer emission lines superimposed on an early type spectrum. Two new Be stars in the field of NGC 330 have been detected. H[FORMULA] emission equivalent width, FWHM and profile shapes (as far as resolved) do not differ from galactic Be stars, hence we suggest that rotation axis of Be stars in NGC 330 are not aligned, rather they are distributed randomly. Quantitative spectral analysis for Be40 and Be59 results in [FORMULA], [FORMULA] and [FORMULA], [FORMULA] respectively.

Key words: line: formation – line: profiles – radiative transfer – stars: circumstellar matter – stars: emission-line, Be

* Based on observations collected during the commissioning 1 of FORS1 at ESO, VLT observatory, Paranal, Chile

Send offprint requests to: W. Hummel

Correspondence to: hummel@bigbang.usm.uni-muenchen.de

© European Southern Observatory (ESO) 1999

Online publication: November 23, 1999