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Accurate atomic data are essential in various field of astrophysics, from solar physics to QSO spectroscopy. Recent calculations made by a large international collaboration known as the Opacity Project (OP) covered energy levels, oscillator strengths and photoionization cross sections of all stages of ionization of astrophysically abundant elements ($1 \leq Z \leq 14$ and $Z=16,18,20,26$). In the meantime, Verner \& Yakovlev (1995, A\&AS, in press) obtained a compact, uniform and complete set of analytic fits to the partial photoionization cross sections of the ground state shells of all atoms and ions of all elements up to zinc ($Z=30$). The latter fits include inner shell ionization and are much more accurate than the OP cross sections at high energies. We are preparing new fits to the photoionization cross sections from the excited states. New photorecombination coefficients based on the OP and the high energy fits to the photoionization cross sections are being calculated. We present the first results of this work, and discuss their implications to ionization balancing calculations and models of astrophysical plasmas.
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