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We present observations of the most bright main sequence stars in the SmallMagellanic Cloud stellar cluster NGC330 obtained with the integral fieldspectrograph MUSE@VLT. The use of this valuable instrument allows us to studyboth photometric and spectroscopic properties of stellar populations of thisyoung star cluster.  The photometric data provide us a precise color magnitude diagram, whichseems to support the presence of two stellar populations of ages of $\sim$ 18Myr and $\sim$ 30 Myr assuming a metallicity of Z = 0.002. Thanks to thespectroscopic data, we derive helium abundance of 10 main sequence stars withinthe effective radius Reff= 20" of NGC330, thus leading to an estimation of$\epsilon(He)$ = 10.93 $\pm$ 0.05 (1$\sigma$ ). The helium elemental abundancesof stars likely belonging to the two possible stellar populations, do not showdifferences or dichotomy within the uncertainties. Thus, our results suggestthat the two stellar populations of NGC330, if they exist, share similaroriginal He abundances.  If we consider stellar rotation velocity in our analysis, a coeval (30 Myr)stellar population, experiencing different values of rotation, cannot beexcluded. In this case, the mean helium abundance < $\epsilon(He)$ >rotobtained in our analysis is 11.00 $\pm$ 0.05 dex. We also verified thatpossible NLTE effects cannot be identified with our analysis because of thespectral resolution and they are within our derived abundance He uncertainties.  Moreover, the analysis of the He abundance as a function of the distance fromthe cluster center of the observed stars do not show any correlation.

MUSE observations of NGC330 in the Small Magellanic Cloud. Helium abundance of bright main sequence stars