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(shortened) The SMC is ideally suited to investigating the recent starformation history from X-ray source population studies. It harbours a largenumber of Be/X-ray binaries, and the supernova remnants can be easily resolvedwith imaging X-ray instruments. We search for new supernova remnants in the SMCand in particular for composite remnants with a central X-ray source. We studythe morphology of newly found candidate supernova remnants using radio, opticaland X-ray images and investigate their X-ray spectra. Here we report on thediscovery of the new supernova remnant around the recently discovered Be/X-raybinary pulsar SXP 1062 in radio and X-ray images. The Be/X-ray binary system isfound near the centre of the supernova remnant, which is located at the outeredge of the eastern wing of the SMC. The remnant is oxygen-rich, indicatingthat it developed from a type Ib event. From XMM-Newton observations we findthat the neutron star with a spin period of 1062 s shows a very high averagespin-down rate of 0.26 s per day over the observing period of 18 days. From thecurrently accepted models, our estimated age of around 10000-25000 years forthe supernova remnant is not long enough to spin down the neutron star from afew 10 ms to its current value. Assuming an upper limit of 25000 years for theage of the neutron star and the extreme case that the neutron star was spundown by the accretion torque that we have measured during the XMM-Newtonobservations since its birth, a lower limit of 0.5 s for the birth spin periodis inferred. For more realistic, smaller long-term average accretion torquesour results suggest that the neutron star was born with a correspondinglylonger spin period. This implies that neutron stars in Be/X-ray binaries withlong spin periods can be much younger than currently anticipated.

SXP 1062, a young Be X-ray binary pulsar with long spin period; Implications for the neutron star birth spin