  Ultra-stripped supernovae are different from other terminal explosions of
massive stars, as they show little or no ejecta from the actual supernova
event. They are thought to occur in massive binary systems after the exploding
star has lost its surface through interactions with its companion. Such
supernovae produce little to no kick, leading to the formation of a neutron
star without loss of the binary companion, which itself may also evolve into
another neutron star. Here we show that a recently discovered high-mass X-ray
binary, CPD -29 2176 (CD -29 5159; SGR 0755-2933), has an evolutionary history
that shows the neutron star component formed during an ultra-stripped
supernova. The binary has orbital elements that are similar both in period and
in eccentricity to one of 14 Be X-Ray binaries that have both known orbital
periods and eccentricities. The identification of the progenitors systems for
ultra-stripped supernovae is necessary as their evolution pathways leads to the
formation of a binary neutron star systems. Binary neutron stars, such as the
system that produced the kilonova GW170817 that was observed with both
electromagnetic and gravitational energy, are known to produce a large quantity
of heavy elements.
