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The long-lived $^{60}$Fe (with a half-life of 2.62 Myr) is a crucialdiagnostic of active nucleosynthesis in the Milky Way galaxy and in supernovaenear the solar system. The neutron-capture reaction$^{59}$Fe(n,$\gamma$)$^{60}$Fe on $^{59}$Fe (half-life = 44.5 days) is the keyreaction for the production of $^{60}$Fe in massive stars. This reaction crosssection has been previously constrained by the Coulomb dissociation experiment,which offered partial constraint on the $E$1 $\gamma$-ray strength function buta negligible constraint on the $M$1 and $E$2 components. In this work, for thefirst time, we use the surrogate ratio method to experimentally determine the$^{59}$Fe(n,$\gamma$)$^{60}$Fe cross sections in which all the components areincluded. We derived a Maxwellian-averaged cross section of 27.5 $\pm$ 3.5 mbat $kT$= 30 keV and 13.4 $\pm$ 1.7 mb at $kT$= 90 keV, roughly 10 - 20% higherthan previous estimates. We analyzed the impact of our new reaction rates innucleosynthesis models of massive stars and found that uncertainties in theproduction of $^{60}$Fe from the $^{59}$Fe(n,$\gamma$)$^{60}$Fe rate are atmost of 25%. We conclude that stellar physics uncertainties now play a majorrole in the accurate evaluation of the stellar production of $^{60}$Fe.

The $^{59}$Fe(n, {\gamma})$^{60}$Fe Cross Section from the Surrogate Ratio Method and Its Effect on the $^{60}$Fe Nucleosynthesis