used in astrophysics are frequently assumed to depend on temperature but to have no density dependence. The rigorous treatment of density dependent ionization and recombination rate coefficients is via collisional-radiative modeling. This was introduced by @bates for radiative recombination only and extended to treat the much more complex case of dielectronic recombination by @burgsum. Summers applied their techniques to determine density dependent ionization and recombination rate coefficients, and the consequential ionization balance for collisional plasmas, for H-like thru Ar-like ions. Graphical results were presented for the elements C, O and Ne [@summers1] and then N, Mg and Si [@summers2]. Reduced temperatures and densities were used so as to enable easy interpolation for other elements. Tables of such recombination rate coefficients were made available only via a Laboratory Report — @summersRAL — due to their voluminous nature at that point in history. The ‘difficulty’ in utilizing this pioneering data led to some modelers attempting to develop simplified approaches. For example, @jordan used an approach which was based on truncating the zero-density DR sum over Rydberg states using a simple density dependent cut-off which itself was based on early collisional-radiative calculations by @burgsum; a suppression factor was formed from its ratio to 