SIMBAD references

Context. For the spectral analysis of high-resolution and high-signal-to-noise spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that is used for their calculation.
Aims. To search for zirconium and xenon lines in the ultraviolet (UV) spectra of G191-B2B and RE 0503-289, new ZrIV-VII, XeIV-V, and XeVII oscillator strengths were calculated. This allows, for the first time, determination of the Zr abundance in white dwarf (WD) stars and improvement of the Xe abundance determinations.
Methods. We calculated ZrIV-VII, XeIV-V, and XeVII oscillator strengths to consider radiative and collisional bound-bound transitions of Zr and Xe in our NLTE stellar-atmosphere models for the analysis of their lines exhibited in UV observations of the hot WDs G191-B2B and RE 0503-289.
Results. We identified one new ZrIV, 14 new ZrV, and ten new ZrVI lines in the spectrum of RE 0503-289. Zr was detected for the first time in a WD. We measured a Zr abundance of -3.5±0.2 (logarithmic mass fraction, approx. 11 500 times solar). We identified five new XeVI lines and determined a Xe abundance of -3.9±0.2 (approx. 7500 times solar). We determined a preliminary photospheric Al abundance of -4.3±0.2 (solar) in RE 0503-289. In the spectra of G191-B2B, no Zr line was identified. The strongest ZrIV line (1598.948Å) in our model gave an upper limit of -5.6±0.3 (approx. 100 times solar). No Xe line was identified in the UV spectrum of G191-B2B and we confirmed the previously determined upper limit of -6.8±0.3 (ten times solar).
Conclusions. Precise measurements and calculations of atomic data are a prerequisite for advanced NLTE stellar-atmosphere modeling. Observed ZrIV-VI and XeVI-VII line profiles in the UV spectrum of RE 0503-289 were simultaneously well reproduced with our newly calculated oscillator strengths.