Atomic Transition Probabilities for UV and Blue Lines of Fe II and Abundance Determinations in the Photospheres of the Sun and Metal-poor Star HD 84937

We report new branching fractions (BFs) for 121 UV lines from the low-lying odd-parity levels of Fe II belonging to the z(6)D degrees , z(6)F degrees, z(6)P degrees, z(4)F degrees, z(4)D degrees, and z(4)P degrees terms of the 3d(6)(D-5)4p configuration. These lines range in wavelength from 2250 to 3280 angstrom and originate in levels ranging in energy from 38,459 to 47,626 cm(-1). In addition, we report BFs for 10 weak blue lines connecting to the z(4)D degrees term that range in wavelength from 4173 to 4584 angstrom. The BFs are combined with radiative lifetimes from the literature to determine transition probabilities and log(gf) values. Comparison is made to selected experimental and theoretical data from the literature. Our new data are applied to iron abundance determinations in the Sun and in metal-poor star HD 84937. For the Sun, eight blue lines yield log epsilon(Fe) = 7.46 +/- 0.03, in agreement with standard solar abundance estimates. For HD 84937 the observable wavelength range extends to the vacuum UV (lambda >= 2327 angstrom), and from 75 lines we derive log epsilon(Fe) = 5.26 +/- 0.01 (sigma = 0.07), near to the metallicity estimates of past HD 84937 studies.