An R-Matrix analysis of the 5337 keV resonance in 19F.

15N(α,γ)19F is believed to be the primary means of stellar nucleosynthesis of fluorine. The tail of the strong J=0.5(+) resonance at 5337 keV in 19F extends down to the astrophysically relevant energies. There remains disagreement between several experimental measurements of the partial alpha-particle and partial gamma-ray widths of this particular resonance. These differences affect extrapolations of the cross-section down to the Gamow window and the resulting reaction rate of 15N(α,γ)19F. In this work, we aim to resolve these differences using an R-matrix fit of several experimental datasets, including recently published results from measurements of the inverse reaction using a bubble chamber.