SIMBAD references

From high-resolution spectra a non-local thermodynamic equilibrium analysis of the Mgii 4481.2-Åfeature is implemented for 52 early and medium local B stars on the main sequence (MS). The influence of the neighbouring line Aliii 4479.9-Åis considered. The magnesium abundance is determined; it is found that logε(Mg) = 7.67±0.21 on average. It is shown that uncertainties in the microturbulent parameter V_t are the main source of errors in logε(Mg). When using 36 stars with the most reliable V_t values derived from Oii and Nii lines, we obtain the mean abundance logε(Mg) = 7.59±0.15. The latter value is precisely confirmed for several hot B stars from an analysis of the Mgii 7877-Åweak line. The derived abundance logε(Mg) = 7.59±0.15 is in excellent agreement with the solar magnesium abundance logε_☉(Mg) = 7.55±0.02, as well as with the proto-Sun abundance logε_ps(Mg) = 7.62±0.02. Thus, it is confirmed that the Sun and the B-type MS stars in our neighbourhood have the same metallicity.