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We investigate $^{60}$Fe in massive stars and core-collapse supernovaefocussing on uncertainties that influence its production in 15, 20 and 25$M_\odot$ stars at solar metallicity. We find that the $^{60}$Fe yield is amonotonic increasing function of the uncertain $^{59}$Fe$(n,\gamma)^{60}$Fecross section and that a factor of 10 reduction in the reaction rate results ina factor 8-10 reduction in the $^{60}$Fe yield; while a factor of 10 increasein the rate increases the yield by a factor 4-7. We find that none of the 189simulations we have performed are consistent with a core-collapse supernovatriggering the formation of the Solar System, and that only models using$^{59}$Fe$(n,\gamma)^{60}$Fe cross section that is less than or equal to thatfrom NON-SMOKER can reproduce the observed $^{60}$Fe/$^{26}$Al line flux ratioin the diffuse ISM. We examine the prospects of detecting old core-collapsesupernova remnants (SNRs) in the Milky Way from their $\gamma$-ray emissionfrom the decay of $^{60}$Fe, finding that the next generation of gamma-raymissions could be able to discover up to $\sim100$ such old SNRs as well asmeasure the $^{60}$Fe yields of a handful of known Galactic SNRs. We alsopredict the X-ray spectrum that is produced by atomic transitions in $^{60}$Cofollowing its ionization by internal conversion and give theoretical X-ray linefluxes as a function of remnant age as well as the Doppler and fine-structureline broadening effects. The X-ray emission presents an interesting prospectfor addressing the missing SNR problem with future X-ray missions.

$^{60}$Fe in core-collapse supernovae and prospects for X-ray and $\gamma$-ray detection in supernova remnants