This table shows the line-strength predictions computed for: CaT, NaI, and MgI in the near infrared and Mgb, Mg2, Fe52, Fe53, NaD and H{beta}, in the blue-visible range, for Single Stellar Population (SSP) of 6 different metallicities, (Z=0.0004, 0.001, 0.004, 0.008, 0.02 and 0.05), and ages from log(age)=6.60 (4Gyr) to log(age)=10.30 (20Gyr), in steps of 0.10dex from 6.60 until 10.00, and 0.02 afterwards. (Therefore there are 50 records for each metallicity except that Z=0.001 has only 47). All indices have been computed taken the model atmospheres from Lejeune et al. (1997, Cat. , 1998, Cat. ) and Clegg & Middlemass (1987MNRAS.228..759C) for hot stars (Teff > 50000 K). The used isochrones are from the Padova group (Bressan et al., 1993, Cat. ). The total mass of every SSP is 10^9^M_{sun} with a Salpeter-type IMF, Phi(m)=m^-{alpha}^, with {alpha}=2.35, from m_low=0.6M{sun} to m_up=100M_{sun}_. The fitting functions for blue indices are those from Worthey et al. (1994, Cat. ).
