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We present here a detailed calculation of opacities for Fe~XVII at thephysical conditions corresponding to the base of the Solar convection zone.Many ingredients are involved in the calculation of opacities. We review theimpact of each ingredient on the final monochromatic and mean opacities(Rosseland and Planck). The necessary atomic data were calculated with the$R$-matrix and the distorted-wave (DW) methods. We study the effect ofbroadening, of resolution, of the extent of configuration sets and ofconfiguration interaction to understand the differences between severaltheoretical predictions as well as the existing large disagreement withmeasurements. New Dirac $R$-matrix calculations including all configurations upto the $n=$ 4, 5 and $6$ complexes have been performed as well as correspondingBreit--Pauli DW calculations. The DW calculations have been extended to includeautoionizing initial levels. A quantitative contrast is made between comparableDW and $R$-matrix models. We have reached self-convergence with $n=6$$R$-matrix and DW calculations. Populations in autoionizing initial levelscontribute significantly to the opacities and should not be neglected. The$R$-matrix and DW results are consistent under the similar treatment ofresonance broadening. The comparison with the experiment shows a persistentdifference in the continuum while the filling of the windows shows someimprovement. The present study defines our path to the next generation ofopacities and opacity tables for stellar modeling.

Quantitative comparison of opacities calculated using the $R$-matrix and Distorted-Wave methods: Fe XVII