This table contains the stellar population properties obtained during the SED-fitting analysis performed by the code MUFFIT (e.g. age, metallicity, extinction, stellar mass, luminosity, etc.), as well as other parameters of interest such as Chi2, mean signal-to-noise ratio, number of bands used in the analysis, etc. As input set for our code MUFFIT, we used the 23 flux from the ALHAMBRA Gold catalogue, the photometric redshift constraints by BPZ2.0 (also included in the Gold catalogue, see Molino et al. 2014), and the simple stellar population (SSP) models provided by Vazdekis et al. (2016, EMILES) for Padova00 isochrones.

To build our sample of composite population models (mixtures of two SSPs or two burst models), we took 22 ages from 0.05 to 14 Gyr and metallicities [M/H]= -1.31, -0.71, -0.40, 0.00, and 0.22 (Padova00 isochrones). For all the composite population models, dust effects were added as a foreground screen assuming the extinction law by Fitzpatrick et al. (1999) with values in the range A_V=0.0—3.1 and R_V=3.1. Therefore, we do not distinguish between extinction and attenuation laws and the extinction in each composite model component is the same. For this model set, a universal Kroupa (2001) initial mass function was assumed. At any redshift, we only used SSP models with ages that are cosmologically relevant, meaning that SSPs much older than the age of the Universe are excluded during the build of the composite population models.