Using evolutionary population synthesis , we present 13 refined absorption-line indices defined by the Lick Observatory Image Dissector Scanner ( Lick/IDS ) system for an extensive set of instantaneous-burst binary stellar populations ( BSPs ) at high resolution ( \sim 0.3 \AA ) , and 38 indices at intermediate resolution ( 3 \AA ) .
The ages of the populations are at an interval of 1 Gyr in the range 1–15 Gyr , and the metallicities are in the range 0.004–0.03 .
These indices are obtained by two methods : ( 1 ) obtain them by using the empirical fitting functions ( FFs method ) ; ( 2 ) measure them directly from the synthetic spectra ( DC method ) .
Together with our previous paper a database of Lick/IDS spectral absorption-line indices for BSPs at high and intermediate resolutions is provided .
This set of indices includes 21 indices of Worthey et al .
( 3 ) , four Balmer indices defined by Worthey & Ottaviani ( 4 ) and 13 indices with the new passband definitions of Trager et al .
( 2 ) .
The full set of synthetic indices and the integrated pseudo-continuum are listed in the Appendix , which is only available online at http : //www.blackwellpublishing.com/… or from our website ( http : //www.ast9.com/ ) , or on request from the first author .
Moreover , the full set of the integrated spectral energy distributions can be obtained from our website .

We compare the synthetic Lick/IDS indices obtained by FFs method and those by DC method for BSPs with various metallicities , and find that the discrepancies are significant : Ca4455 ( index 6 ) , Fe4668 ( 8 ) , Mg _ { b } ( 13 ) , Fe5709 ( 17 ) , NaD ( 19 ) , TiO _ { 1 } ( 20 ) and TiO _ { 2 } ( 21 , except for Z = 0.02 ) in the W94 system , Ca4455 ^ { T } ( 6 ^ { T } ) , C _ { 2 } 4668 ^ { T } ( 8 ^ { T } ) , NaD ^ { T } ( 19 ^ { T } ) , TiO _ { 1 } { } ^ { T } ( 20 ^ { T } ) and TiO _ { 2 } { } ^ { T } ( 21 ^ { T } , except for Z = 0.02 ) in the T98 system obtained by DC method are less ( bluer ) than the corresponding ones obtained by FFs method for all metallicities .
Ca4227 ( index 3 ) , Fe5782 ( 18 ) , Ca4227 ^ { T } ( 3 ^ { T } ) and Fe5782 ^ { T } ( 18 ^ { T } ) are greater at Z = 0.03 and become to be bluer at Z = 0.004 , Fe5709 ^ { T } ( 17 ^ { T } ) index is less at Z = 0.03 and becomes to be redder at Z = 0.004 than the corresponding ones obtained by FFs method .