SIMBAD references

ESO spectra of HD65949 show it to be unlike any of the well-known types within its temperature range ≃13600K. It is neither a silicon, nor a mercury-manganese star, though it has a huge Hg II line at λ3984. We estimate log(Hg/H)+12.0≃7.4. This is higher than any published stellar mercury abundance. HD65949 is a member of a nearby open cluster, NGC2516, which is only slightly older than the Pleiades, and has been of recent interest because of its numerous X-ray emission stars, including HD65949 itself, or a close companion. A longitudinal magnetic field of the order of -290Gauss at the 4.7σ level was very recently diagnosed from accurate circular spectropolarimetric observations with FORS 1 at the VLT. The spectral lines are sharp, allowing a thorough identification study. Second spectra of Ti, Cr, and Fe are rich. Mn II is well identified but not unusually strong. Numerous lines of S II and P II are found, but not Ga II. The resonance lines of Sr II are strong. While many Y II lines are identified, and Nb II is very likely present, no Zr II lines were found. Xe II is well identified. Strong absorptions from the third spectra of the lanthanides Pr, Nd, and Ho are present, but lines from the second spectra of lanthanides are extremely weak or absent. Among lines from the heavier elements, those of Pt II are clearly present, and the heaviest isotope, ¹⁹⁸Pt, is indicated. The uncommon spectrum of Re II is certain, while Os II and Te II are highly probable. Several of the noted anomalies are unusual for a star as hot as HD 65949.