Search for recent Core-collapse Supernovae in the Solar Neighborhood

Core-collapse supernovae (CC-SNe) are pivotal processes for the synthesis and dispersal of heavy elements, e.g. 60-Fe, in our Galaxy. The detection of 60-Fe isotopes in the Earth's crust and on the moon indicates a few recent (ca. 2 Myr) CC-SNe within the Solar neighborhood (ca. 100 pc). Since the overwhelming majority of massive young stars are in multiples, most CC-SNe are expected to occur in those systems. These systems either get disrupted from such an explosion, leaving a neutron star and an unbound runaway star, or both components remain bound and form a high mass X-ray binary (HMXB), if furthermore their separation is small enough. Investigating these CC-SNe and also their corresponding HMXBs will enhance our understanding of SNe and their yields. For evidence of recent nearby SNe in binaries, one can trace back the space motion of neutron stars and runaway stars through the Galactic potential to identify places and times where such SNe have occurred - the limitations are pulsar beaming and missing radial velocities, etc.. A second way is to search for HMXBs, whose crucial feature is the emission of X-rays, caused by material accreting onto the compact object. In the course of comprehensive investigations, we applied both methods, analyzing all OB-type stars in the Solar Neighborhood. With the potential HMXB 1H11255-567 with mu1 and mu2 Cru and the pulsar-runaway-pair PSRB1706-16 and zeta Oph, one case for each type could already be suggested (Neuhäuser et al., 2020, MNRAS 498, 899). Several further promising HMXB candidates, which could possibly be sources of the detected 60Fe, were identified and characterized through the analysis of numerous observations of our targets in X-rays (e.g., ROSAT, XMM-Newton, Chandra, Einstein) and optical/IR (e.g., Gaia DR3, Hipparcos, 2MASS), combined with the astrometric search for close compact binary components. Here, we will present the principal methodology and the latest results of our survey.