Age (top row), metallicity (middle row), and extinction (bottom row) of the inner star-forming ring of NGC 3351 obtained using three different sets of templates: E-MILES (left column), CB07, excluding templates younger than 30 Myr (CB07-A; central column), and CB07 including young templates (CB09-B; right column). Adding younger templates to our template grid slightly alleviates the problem of extremely metal-poor and young regions in the sense that the young clusters are younger and mildly less metal-poor. However, the improvement is marginal, and these regions are still significantly more metal-poor than the surrounding pixels. Panels in the last row show, additionally, an abnormally low extinction in the young and metal-poor regions (marked as white circles in the left column). This is likely a consequence of the same issue, as it is partially improved when younger templates are included. Overall, adding templates younger than 30 Myr to our age-metallicity grid does not provide a solution to the issue of young and extremely metal-poor regions.