The Hg ii Line at 5677.10 Å: A New Proxy to Derive Abundances of Mercury in Late B-type Stars?

Abstract Abundance determinations of mercury in late B-type stars in the optical range usually rely on the use of one absorption line of Hg ii at 3983.93 Å. A proposal is made to use another but weaker line of Hg ii located at 5677.10 Å. This line is present in the spectra of two mercury rich stars, κ Cnc and HD 58661, and absent in 53 Tau whose abundance of mercury is less than the solar value. The synthesis of the 5677.10 Hg ii line, using the current atomic parameters available in NIST, confirms that mercury is very abundant in κ Cnc and HD 58661. The abundances derived with 5677.10 Å are currently less than these derived from 3983.93 Å.