the sum of the squared residuals between a linear combination of a set of pre-chosen spectra and the target galaxy SED (Mateu, Bruzual, Magris 2007, in preparation). The model spectra are from the Bruzual and Charlot (2003) models.

Our results are presented in 7 text files and 7 figures.

In each text file we show for each target spectrum:

The derived velocity dispersion after removing the intrinsic width of the

STELIB stellar library

The B-V, g-r colors and the 4000A break for the target spectrum (OBS),

and for the derived spectrum (MOD)

The table contains:

column 1: The central value of each bin age (yr))

column 2: The accumulated mass fraction from 14 Gyr to the bin centered in the column 1 value

column 3 - 8: Mass fraction formed in the indicated bin age with the abundance (Z) labeled in each column

Summarizing the properties of each spectrum:

Spectrum 1 (ps, table): Very old (age > 8Gyr), solar metallicity stellar population

Spectrum 2 (ps, table): Old, mainly subsolar (84% Z=0.008) with traces of Z=0.004, and possibly a 3% of solar stellar population

Spectrum 3 (ps, table): Old, 80% solar and 15% Z=0.004, 2% of solar, younger (3-9 Gyr) population

Spectrum 4 (ps, table): Old, 60% solar 38% Z=0.004

Spectrum 5 (ps, table): Intermediate age (>3 Gyr), solar and subsolar stellar population

Spectrum 6 (ps, table): 82% of solar metallicity and 9% of Z=0.008 mass with age > 9 Gyr, and 8% of younger (3-9) Gyr of solar metallicity

Spectrum 7 (ps, table): 92% of old (> 9 Gyr), solar metallicity, 2% of Z=0.008 and 5% of Z=0.004

Gladis Magris, Gustavo Bruzual, Juan Mateu