Nucleosynthesis of $^{60}$Fe and constraints on the nuclear level density and photon strength function.

$^{60}$Fe is created in massive stars prior to core collapse supernova. The signature $\gamma$-rays from $\beta$-decay of this isotope indicate ongoing nucleosynthesis in the Galaxy among other interesting astrophysical processes. In order to understand these observations a complete understanding of the creation, destruction and nuclear properties of $^{60}$Fe in the astrophysical environment are required. Due to the short half-life of $^{59}$Fe a direct capture reaction experiment to determine the cross section of $^{59}$Fe(n,$\gamma$)$^{60}$Fe has been a challenge and remains the most uncertain link in the reaction chain to date. Using the $\beta$-decay of a $^{60}$Mn radioactive beam to populate high energy states in the $^{60}$Fe nucleus, an indirect constraint for this reaction was made using the $\beta$-Oslo Method. Results from this analysis were used as input in TALYS and the new constraint on $^{59}$Fe(n,$\gamma$)$^{60}$Fe will be presented.