Searching for Magnetar Binaries Disrupted by Core-Collapse Supernovae
Monthly Notices of the Royal Astronomical Society(2024)
摘要
Core-collapse Supernovae (CCSNe) are considered to be 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 ∼45% 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≲ f_u ≲ 24%,
which disagrees with population synthesis results. Alternate formation channels
are unlikely to wholly account for the lack of unbound binaries as this would
require 31≲ f_nc≲ 66% of magnetars to descend from such
channels. Our results support a high fraction (48≲ f_m ≲ 86%)
of pre-CCSN mergers, which can amplify fossil magnetic fields to preferentially
form magnetars.
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