Searching for Magnetar Binaries Disrupted by Core-Collapse Supernovae

Core-collapse Supernovae (CCSNe) are considered the primary magnetar formation channel, with 15 magnetars associated with supernova remnants (SNRs). A large fraction of these should occur in massive stellar binaries that are disrupted by the explosion, meaning that \(\sim45\%\) of magnetars should be nearby high-velocity stars. Here we conduct a multi-wavelength search for unbound stars, magnetar binaries, and SNR shells using public optical (\(uvgrizy-\)bands), infrared (\(J-\), \(H-\), \(K-\), and \(K_s-\)bands), and radio (\(888\) MHz, \(1.4\) GHz, and \(3\) GHz) catalogs. We use Monte Carlo analyses of candidates to estimate the probability of association with a given magnetar based on their proximity, distance, proper motion, and magnitude. In addition to recovering a proposed magnetar binary, a proposed unbound binary, and 13 of 15 magnetar SNRs, we identify two new candidate unbound systems: an OB star from the Gaia catalog we associate with SGR J1822.3-1606, and an X-ray pulsar we associate with 3XMM J185246.6+003317. Using a Markov-Chain Monte Carlo simulation that assumes all magnetars descend from CCSNe, we constrain the fraction of magnetars with unbound companions to \(5\lesssim f_u \lesssim 24\%\), which disagrees with neutron star population synthesis results. Alternate formation channels are unlikely to wholly account for the lack of unbound binaries as this would require \(31\lesssim f_{nc} \lesssim 66\%\) of magnetars to descend from such channels. Our results support a high fraction (\(48\lesssim f_m \lesssim 86\%\)) of pre-CCSN mergers, which can amplify fossil magnetic fields to preferentially form magnetars.