of magnitudes.

Our modeling is parameterized in terms of two stellar population parameters, the age and metallicity, whose priors are set by the limits of the model ranges. In this work, we use the E-MILES models [@2016MNRAS.463.3409V], assuming prior distributions given by

$$\begin{aligned}
 \text{[Fe/H]}(\text{dex}) \sim \textrm{Uniform}(-1.79, 0.4)\\  
 \text{Age} (\text{Gyr}) \sim \textrm{Uniform}(0.4, 14)\text{.}\end{aligned}$$

The main reason to set the limits above is to ensure that the models have good quality in the ultra-violet according to the classification of @2010MNRAS.404.1639V, resulting in the exclusion of SSP models with \[Fe/H\]$=-2.27$, which may not be appropriate for metallicity estimation. Additionally, we also require a regular grid in the parameter space to perform linear interpolation of the SSP models, allowing a continuous coverage of ages and metallicities. As a consequence, we had to restrict the models to ages greater than 0.4 Gyr because part of the young SSP models are not extended to the near-infrared, which is necessary to cover the $z$ band properly. In particular, we adopt models with bimodal , a piecewise function defined by @1996ApJS..106..307V that matches the Salpeter for masses $>0.8M_\odot$ but is flattened at lower masses similarly to the Milky Way [e.g. @2003PASP..115..763C]. Given that the current version of the 