The resonance line of Hg II at 1942 Å in Sirius and Vega is analyzed quantitatively based on high-resolution UV spectroscopic data. The spectrum synthesis technique is employed. The abundance of Hg in Sirius (log ∊(Hg) = 2.5±0.5) is found to coincide with that found in the two normal late B-type stars ν Cap and π Cet. On the other hand, the obtained upper limit for Vega (log ∊(Hg) ≤ 0.5) is lower than the solar-system abundance log ∊(Hg) = 1.2.
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Sadakane et al. (1988) studied this question.