First row: stellar surface density as a function of Galactic radius for stars with distance from the midplane | z | < 3 kpc. In addition to the total mass (pink symbols), subsamples grouped by narrow bins of age (left panel), [Mg/Fe] (middle panel), and [Fe/H] (right panel) are shown by different colors, as indicated. The corresponding bin values are shown on top of the figure. The color–coded values in each panel indicate the scale-length, r_d, fitted as a single exponential in the range 5 <r< 16.5 kpc, shown by the dotted lines (dashed pink line for the total population). Decrease in scale-length is seen with increasing age for all three distances from the disk plane. While single exponential fits are appropriate for mono-age populations (left column), stars binned by [Mg/Fe] or [Fe/H] show truncation (a change to a steeper exponential) around 5–10 kpc for the younger stars (black and blue curves). Second row: same as above, but for stars with | z | < 0.5 kpc. Third row: same as above, but for stars with 0.5 < | z | < 3 kpc. At this distance from the disk plane (similar to SEGUE G-dwarfs), the breaks in the high-[Fe/H] and low-[Mg/Fe] profiles are mostly gone.