  Accurate atomic data is an essential ingredient for the calculation of
reliable non-local thermodynamic equilibrium (NLTE) model atmospheres that are
mandatory for the spectral analysis of hot stars. We aim to search for and
identify for the first time spectral lines of copper (atomic number Z = 29) and
indium (Z = 49) in hot white dwarf (WD) stars and to subsequently determine
their photospheric abundances. Oscillator strengths of Cu IV - VII were
calculated to include radiative and collisional bound-bound transitions of Cu
in our NLTE model-atmosphere calculations. Oscillator strengths of In IV - VI
were compiled from the literature. We newly identified 1 Cu IV, 51 Cu V, 2 Cu
VI, and 5 In Vlines in the ultraviolet (UV) spectrum of DO-type WD RE 0503-289.
We determined the photospheric abundances of 9.3 X 10**-5 (mass fraction, 132
times solar) and 3.0 X 10**-5 (56 600 times solar), respectively; we also found
Cu overabundances in the DA-type WD G191-B2B (6.3 X 10**-6, 9 times solar). All
identified Cu IV - VI lines in the UV spectrum of RE 0503-289 were
simultaneously well reproduced with our newly calculated oscillator strengths.
With the detection of Cu and In in RE 0503-289, the total number of trans-iron
elements (Z > 28) in this extraordinary WD reaches an unprecedented number of
18.
