  We report new branching fractions for 121 UV lines from the low-lying
odd-parity levels of Fe II belonging to the z6Do, z6Fo, z6Po, z4Fo, z4Do and
z4Po terms of the 3d6(5D)4p configuration. These lines range in wavelength from
2250 - 3280 {\AA} and originate in levels ranging in energy from 38459 - 47626
cm-1. In addition, we report branching fractions for 10 weak blue lines
connecting to the z4Do term which range in wavelength from 4173 - 4584 {\AA}.
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 {\AA}), 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.
