Using evolutionary population synthesis we present high resolution ( 0.3 \AA ) integrated spectral energy distributions from 3000 to 7000 \AA and absorption-line indices defined by the Lick Observatory image dissector scanner ( referred to as the Lick/IDS ) system , for an extensive set of instantaneous burst binary stellar populations with binary interactions .
The ages of the populations are in the range 1 - 15 Gyr and the metallicities are in the range 0.004 - 0.03 .
This high resolution synthesis results can satisfy the needs of modern spectroscopic galaxy surveys , and are available on request .

By comparing the synthetic continuum of populations at high and low resolution we show that there is a good agreement for solar metallicity and a tolerable disagreement for non-solar metallicity .
The strength of the Balmer lines at high spectral resolution is greater than that at low resolution for all metallicities .
The comparison of Lick/IDS absorption-line indices at low and high resolution , both of which are obtained by the fitting functions , shows that the discrepancies in all indices except for TiO _ { 1 } and TiO _ { 2 } are insignificant for populations with Z = 0.004 and Z = 0.02 .
The high resolution Ca4227 , Fe5015 and Mg _ { b } indices are redder than the corresponding low resolution one for populations with Z = 0.01 and Z = 0.03 , this effect lowers the derived age and metallicity of the population .
The high resolution Mg _ { 1 } , Fe5709 and Fe5782 indices are bluer than those at low resolution , it raises the age and metallicity .
The discrepancy in these six indices is greater for populations with Z = 0.03 in comparison to Z = 0.01 .

At high resolution we compare the Lick/IDS spectral absorption indices obtained by using the fitting functions with those measured directly from the synthetic spectra , and see that Ca4455 , Fe4668 , Mg _ { b } and Na D indices obtained by the use of the fitting functions are redder for all metallicities , Fe5709 is redder at Z = 0.03 and becomes to be bluer at Z = 0.01 and 0.004 , and other indices are bluer for all metallicities than the corresponding values measured directly from the synthetic spectra .