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The interpretation of HII region spectrophotometric data and the characteristics of their ionizing stars are important to our understanding of the formation and chemical evolution of stars and galaxies. The study of single-star ionized regions facilitates HII region modeling. Long slit spectra were collected for 14 single-star ionized HII regions in the Large Magellanic Cloud. Electron densities for most of the regions were estimated form the ratio of the density sensitive sulphur lines. Electron temperature and excitations were calculated using the intensities of the forbidden [OIII] lines and the H-Beta (Hb) line. Using the diagnostic diagrams of Evans and Dopita (1985) we argue that these regions have low metallicities. Using our data, we also show that there is a linear correlation between the line intensity ratios ([OII]/Hb)([OII]/[SII]) and [OII]+[OIII]/Hb. We present results form narrow band imaging and long-slit spectroscopic data and show that the HII region excitation is correlated with the emission measure.
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