  The 22Ne({\alpha},n)25Mg reaction is an important source of neutrons for the
s-process. In massive stars responsible for the weak component of the
s-process, 22Ne({\alpha},n)25Mg is the dominant source of neutrons, both during
core helium burning and in shell carbon burning. For the main s-process
component produced in Asymptotic Giant Branch (AGB) stars, the
13C({\alpha},n)16O reaction is the dominant source of neutrons operating during
the interpulse period, with the 22Ne+{\alpha} source affecting mainly the
s-process branchings during a thermal pulse. Rate uncertainties in the
competing 22Ne({\alpha},n)25Mg and 22Ne({\alpha},{\gamma})26Mg reactions result
in large variations of s-process nucleosynthesis. Here, we present up-to-date
and statistically rigorous 22Ne+{\alpha} reaction rates using recent
experimental results and Monte Carlo sampling. Our new rates are used in
post-processing nucleosynthesis calculations both for massive stars and AGB
stars. We demonstrate that the nucleosynthesis uncertainties arising from the
new rates are dramatically reduced in comparison to previously published
results, but several ambiguities in the present data must still be addressed.
Recommendations for further study to resolve these issues are provided.
