New Linelists for Fe I - VI Robert L. Kurucz Harvard-Smithsonian Center for Astrophysics I am computing atomic line lists for generating stellar opacities, model atmospheres, and predicted spectra, and for interpreting observed spectra using my own versions of programs that I got from Robert Cowan. I compute the whole E1, M1, and E2 transition arrays for configurations up through n = 9 or higher. Hartree-Fock starting guesses are used for the Slater-parameter expansion of the Hamiltonians. All configuration interactions are included. Slater integrals are adjusted by least squares fitting the calculated eigen- values to the observed energies. Once the least squares fits have converged, all the eigenvectors and eigenvalues are computed. The eigenvalues are replaced by the observed energies. The LS transition array is computed with Hartree- FocK transition integrals. Finally the LS transition array is transformed to the observed coupling using the eigenvector matrices. Here are numbers that indicate the scope of the calculations: config levels E1 lines eve odd eve odd good wl total Fe I 61 50 18655 18850 93508 6029023 Fe II 46 39 19771 19652 85362 7615097 Fe III 49 41 19720 19820 33982 9770250 Fe IV 61 54 13767 14211 8408 14617228 Fe V 61 61 6560 7526 11417 7785320 Fe VI 61 61 2094 2496 3535 1386203 The calculations are compared with other calculations and with laboratory measurements. Comparisons are given with Iron Project calculations and with all the NIST compiled data for allowed and forbidden lines, and with other data. I attempt to collect all other work from the literature and, in making the working line iists for interpreting spectra, I try to incorporate the best data available. I include data for measured isotopic and hyperfine splittings. The calculations are repeated whenever new energy level data become available. Each new energy level moves many lines from the predicted list to the list with known wavelengths. On my web site kurucz.harvard.edu under /atoms, are posted complete line lists, reduced linelists with only good wavelengths, energies, compositions, A-sums, C4, C6, Lande' g, lifetimes, branching fractions, partition functions, and programs for reading and reformatting the data.