Evolutionary Population Synthesis for Binary Stellar Population at High Spectral Resolution: Integrated Spectral Energy Distributions and Absorption-feature Indices

Using evolutionary population synthesis we present high resolution (0.3 Å) integrated spectral energy distributions from 3000 to 7000 Å 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− 15Gyr 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 TiO1 and TiO2 are insignificant for populations with Z = 0.004 and Z = 0.02. The high resolution Ca4227, Fe5015 and Mgb 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 Mg1, 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, Mgb 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.