  The presence of an anomalously large population of Be stars in the young
cluster NGC 330 in the SMC has been noted by Feast (1972), Bessell & Wood
(1993), Grebel (1996) and most recently Keller et al. (1998). We present
results from follow-up medium resolution spectra of the bright Be stars
identified in Keller et al. (1998) and in the spectroscopic study of Mazzali et
al. (1996). We find that the study of Mazzali et al. has overestimated the
number of Be stars within NGC 330. Many of the bright B type stars identified
by Mazzali et al. as Be stars show no signs of emission after correction for
the diffuse HII emission pervading the cluster field.
  In the study of Mazzali et al. (1996) evidence is presented suggesting that
all Be stars in NGC 330 have a common inclination of their rotation axes to the
line of sight. For our sample of Be stars we present the emission equivalent
widths and observed rotational velocities. An examination of these quantities
shows that there is no evidence of a preferential alignment of the rotational
axes, rather we are observing a population with random rotational axis
alignment and disk size.
