0 Assigned ID: 1563 ----- Attempting Submission 1 (Fri Mar 01 17:24:39 GMT 2013) ----- With rapid technological and computational advances in astrophysics, a multitude of ever fainter objects near and far are being observed with greater and greater precision. Seriously lacking are reliable, comprehensive atomic data needed to interpret the present and future wealth of information. The Fe I atom is a notable example: measurements of the energies of its high-lying levels are woefully incomplete. Here we propose to determine upper energies of Fe I using STIS E230H archival spectra of metal-poor stars spanning 1850A - 3150A. Our spectral calculations match these well, except for lines of unknown identification. The vast majority are due to Fe I lines whose predicted wavelengths are in error because the upper energy level is not measured. We can derive the energy for a particular upper level by adopting a trial value providing a wavelength for one of its strong predicted near-UV lines that matches the wavelength of a strong unidentified spectral line, then checking the new wavelengths of other strong predicted transitions that share the same upper level for coincidence with other strong unidentified lines. To date we have matched three or more transitions for eight levels, deriving energies up to 63183 cm^-1 (7.8 eV), and identifying 1228 individual lines. Our goal is to do this for 100 new levels, and to understand how best to extend this to levels with weaker transitions only. The newly-identified energy levels and resulting line parameters will be placed on the Kurucz website, to enable better use of Hubble archive products by the community, for research ranging from nucleosynthesis at early epochs to deriving age and metallicity for old, distant galaxies. COOL STARS Default Small false true false false false SUPPORTED