Context : Both recent observations and stellar evolution models suggest that pair-instability supernovae ( PISNe ) could occur in the local Universe , at metallicities below \lesssim Z _ { \odot } / 3 .
Previous PISN models were mostly produced at very low metallicities in the context of the early Universe .

Aims : We present new PISNe models at a metallicity of Z = 0.001 , which are relevant for the local Universe .

Methods : We take the self-consistent stellar evolutionary models of pair-instability progenitors with initial masses of 150 M _ { \odot } and 250 M _ { \odot } at metallicity of Z = 0.001 by Langer et al .
( 2007 ) and follow the evolution of these models through the supernova explosions , using a hydrodynamics stellar evolution code with an extensive nuclear network including 200 isotopes .

Results : Both models explode as PISNe without leaving a compact stellar remnant .
Our models produce a nucleosynthetic pattern that is generally similar to that of Population III PISN models , which is mainly characterized by the production of large amounts of \alpha - elements and a strong deficiency of the odd-charged elements .
However , the odd-even effect in our models is significantly weaker than that found in Population III models .
The comparison with the nucleosynthetic yields from core-collapse supernovae at a similar metallicity ( Z = 0.002 ) indicates that PISNe could have strongly influenced the chemical evolution below Z \approx 0.002 , assuming a standard initial mass function .
The odd-even effect is predicted to be most prominent for the intermediate mass elements between silicon and calcium .

Conclusions : With future observations of chemical abundances in Population II stars , our result can be used to constrain the number of PISNe that occurred during the past evolution of our Galaxy .