Effect of the age uncertainties on the age-[α/Fe] distribution (left column), age-metallicity distribution (middle column), and [α/Fe]-[Fe/H] distribution (right column) for APOGEE DR17 local dwarfs. The ages in this case were obtained with the observational input G absolute magnitude, MG₀, and Gaia DR3 de-reddened color (Bp - Rp)₀. The stars in these plots were selected to have ages above 1 Gyr, [Fe/H] lower than −1 dex, and (BP - RP)₀ lower than 0.95. We compare three different cuts: e_age < 0.3 Gyr, e_age < 0.5 Gyr, e_age < 0.7 Gyr with the total distribution to which no selection on age uncertainty is applied (bottom row). The stars are color-coded for [Fe/H], [α/Fe], and age, respectively. The number of candidate YARs (with age below 7 Gyr and [α/Fe] above 0.12 dex) is written in orange in each age-[α/Fe] panel. Black lines are plotted in the age-[α/Fe] relation for stars with e_age < 0.3 Gyr to highlight the presence of two distinct slopes in the thick disk sequence. We note that the age scale in this image may be shifted by 1-2 Gyr toward older ages if the age scale from Nissen et al. (2020) is correct when making comparisons (see Section 2.4 and Fig. 3).