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 PSR B1706-16 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 .