We aim to identify the birth place of the young pulsar PSR J0826 + 2637 in order to determine its kinematic age and give constraints on its radial and spatial ( kick ) velocity .

Since the majority of neutron star ( NS ) progenitors are in associations or clusters , we search for a possible origin of the NS inside such stellar groups .
We trace back the NS and the centres of possible birth associations and clusters to find close encounters .
The kinematic age is then given by the time since the encounter .
We use Monte Carlo simulations to account for observational uncertainties and the unknown radial velocity of the NS .
We evaluate the outcome statistically .
In order to find further indication for our findings , we also search for a runaway star that could be the former companion if it exists .

We find that PSR J0826 + 2637 was probably born in the small young cluster Stock 7 \sim 3 \mathrm { Myr } ago .
This result is supported by the identification of the former companion candidate HIPÂ 13962 ( runaway star with spectral type G0Ia ) .
The scenario predicts a near-zero radial velocity of the pulsar implying an inclination angle of its motion to the line-of-sight of 87 \pm 11 \mathrm { deg } .

We also present the chemical abundances of HIP 13962 .
We do not find enhanced \alpha element abundances in the highly evolved star .
However , the binary supernova scenario may be supported by the overabundance of r-process elements that could have been ejected during the supernova and accreted by the runaway star .
Also , a high rotational velocity of v \sin i \sim 29 \mathrm { km / s } of HIP 13962 is consistent with evolution in a pre-SN binary system .