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Branching fraction measurements from Fourier transform spectra in conjunctionwith published radiative lifetimes are used to determine transitionprobabilities for 263 lines of neutral chromium. These laboratory values areemployed to derive a new photospheric abundance for the Sun: log $\epsilon$(CrI)$_{\odot}$ = 5.64$\pm$0.01 ($\sigma = 0.07$). These Cr I solar abundances donot exhibit any trends with line strength nor with excitation energy and therewere no obvious indications of departures from LTE. In addition, oscillatorstrengths for singly-ionized chromium recently reported by the FERRUM Projectare used to determine: log $\epsilon$(Cr II)$_{\odot}$ = 5.77$\pm$0.03 ($\sigma= 0.13$). Transition probability data are also applied to the spectra of threestars: HD 75732 (metal-rich dwarf), HD 140283 (metal-poor subgiant), and CS22892-052 (metal-poor giant). In all of the selected stars, Cr I is found to beunderabundant with respect to Cr II. The possible causes for this abundancediscrepancy and apparent ionization imbalance are discussed.

Improved Laboratory Transition Probabilities for Neutral Chromium and Re-determination of the Chromium Abundance for the Sun and Three Stars