  Central compact objects (CCOs) are thought to be young thermally emitting
isolated neutron stars that were born during the preceding core-collapse
supernova explosion. Here we present evidence that at least in one case the CCO
could have been formed within a binary system. We show that the highly reddened
optical source IRAS~17287$-$3443, located $25^{\prime \prime}$ away from the
CCO candidate XMMUJ173203.3$-$344518 and classified previously as a post
asymptotic giant branch star, is indeed surrounded by a dust shell. This shell
is heated by the central star to temperatures of $\sim90$\,K and observed as
extended infrared emission in 8-160\,$\mu$m band. The dust temperature also
increases in the vicinity of the CCO which implies that it likely resides
within the shell. We estimate the total dust mass to be $\sim0.4-1.5\,M_\odot$
which significantly exceeds expected dust yields by normal stars and thus
likely condensed from supernova ejecta. Taking into account that both the age
of the supernova remnant and the duration of active mass loss phase by the
optical star are much shorter than the total lifetime of either object, the
supernova and the onset of the active mass loss phase of the companion have
likely occurred approximately simultaneously. This is most easily explained if
the evolution of both objects is interconnected. We conclude, therefore, that
both stars were likely members of the same binary system disrupted by a
supernova.
