  The detection of $\sim 1.5-3.2$ Myr old $^{60}$Fe on Earth indicates recent
nearby core-collapse supernovae. For supernovae in multiple stars, the primary
stars may become neutron stars, while former companions may become unbound and
become runaway stars. We wrote software for tracing back the space motion of
runaway and neutron stars to young associations of massive stars. We apply it
here to the nearby young Scorpius-Centaurus-Lupus groups, all known runaway
stars possibly coming from there, and all 400 neutron stars with known
transverse velocity. We find kinematic evidence that the runaway $\zeta$ Oph
and the radio pulsar PSRB1706-16 were released by a supernova in a binary $1.78
\pm 0.21$ Myr ago at $107 \pm 4$ pc distance (for pulsar radial velocity $260
\pm 43$ km/s); association age and flight time determine the progenitor mass
(16-18 M$_{\odot}$), which can constrain supernova nucleosynthesis yields and
$^{60}$Fe uptake on Earth. In addition, we notice that the only high-mass X-ray
binary in Scorpius-Centaurus-Lupus (1H11255-567 with $\mu^{1}$ and $\mu^{2}$
Cru) may include a neutron star formed in another SN, up to $\sim 1.8$ Myr ago
at $89-112$ pc, i.e. also yielding $^{60}$Fe detectable on Earth. Our scenario
links $^{60}$Fe found on Earth to one or two individual supernovae in multiple
stars.
