  The $^{15}$N($\alpha,\gamma$)$^{19}$F reaction produces $^{19}$F in
asymptotic giant branch (AGB) stars, where the low energy tails of two
resonances at $E_{\rm{c.m.}} = 1323 \pm 2$ and $1487 \pm 1.7$ keV are estimated
to contribute about $30\%$ of the total reaction rate in these environments.
However, recent measurements have shown discrepancies in the energies, the
strengths, and the corresponding alpha widths of these two resonances,
resulting in an increase in the systematic uncertainty of the extrapolated
cross section to helium burning energies. With this motivation, we have
undertaken new measurements of the $^{15}$N$(\alpha,\gamma)^{19}$F at the
University of Notre Dame Nuclear Science Laboratory. The setup consisted of an
alpha particle beam impinged on a solid Ti$^{15}$N target with gamma-ray
spectroscopy accomplished using a high purity germanium detector. Using the
Doppler corrected gamma-ray energies, we confirmed the lower resonance energy
to be $1321.6 \pm 0.6$ keV and found a value for the higher one of $1479.4 \pm
0.6$ keV that is more consistent with those found from previous elastic
scattering studies. We found that the resonance strengths for both were
consistent with most values found in the literature, but a larger alpha width
has been recommended for the $E_{\rm{c.m.}} = 1487$ keV resonance. The larger
alpha width suggests a reaction rate increase of about $15\%$ at temperatures
$T < 0.1$ GK relevant to low mass AGB stars. The impact of the increased
reaction rate requires further investigations.
