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

We present a spectroscopic study of early type emission line stars in the f ield 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 prog ram stars investigated can be confirmed to show Balmer emission lines super imposed on an early type spectrum. Two new Be stars in the field of NGC 330 have been detected. Hoc emission equivalent width, FWHM and profile shapes (as far as resolved) do not differ from galactic Be stars, hence we sugges t that rotation axis of Be stars in NGC 330 are not aligned, rather they ar e distributed randomly. Quantitative spectral analysis for Be40 and Be59 re sults in T-eff = 18 000 +/- 1 500 K, log g = 3.3 +/- 0.2 and T-eff = 17 000 +/- 1 500 K, log g = 3.1 +/- 0.2 respectively.