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Massive stars are among the main cosmic engines driving the evolution ofstar-forming galaxies. Their powerful ionising radiation and stellar windsinject a large amount of energy in the interstellar medium. Furthermore,mass-loss ($\dot{M}$) through radiatively driven winds plays a key role in theevolution of massive stars. Even so, the wind mass-loss prescriptions used instellar evolution models, population synthesis, and stellar feedback modelsoften disagree with mass-loss rates empirically measured from the UV spectra oflow metallicity massive stars. The most massive young star cluster in the lowmetallicity Small Magellanic Cloud galaxy is NGC346. This cluster contains morethan half of all O stars discovered in this galaxy so far. A similar age,metallicity ($Z$), and extinction, the O stars in the NGC346 cluster areuniquely suited for a comparative study of stellar winds in O stars ofdifferent subtypes. We aim to use a sample of O stars within NGC346 to studystellar winds at low metallicity. We mapped the central 1" of NGC346 with thelong-slit UV observations performed by the Space Telescope Imaging Spectrograph(STIS) on board of the {\em Hubble Space Telescope} and complemented these newdatasets with archival observations. Multi-epoch observations allowed for thedetection of wind variability. The UV dataset was supplemented by opticalspectroscopy and photometry. The resulting spectra were analysed using anon-local thermal equilibrium model atmosphere code (PoWR) to determine windparameters and ionising fluxes. The effective mapping technique allowed us toobtain a mosaic of almost the full extent of the cluster and resolve stars inits core. Among hundreds of extracted stellar spectra, 21 belong to O stars.Nine of them are classified as O stars for the first time. We analyse, indetail, the UV spectra of 19 O stars... (continued)

Stellar wind properties of the nearly complete sample of O stars in the low metallicity young star cluster NGC346 in the SMC galaxy