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tokens: with other techniques for measuring half-mass radii are presented in Suess et al. ( 2019 ). Suess et al. ( 2019 ) also show that the half-mass radii recovered using our technique are not significantly biased by the galaxy’s half-light radius, stellar mass, or redshift. In Figure 1 , we show the strength of galaxy color gradients (i.e., r e,mass / r e,light ) as a function of stellar mass for two redshift slices in our new low-redshift sample. We divide the sample into star-forming and quiescent populations using the UVJ diagram and the quiescent definition from Whitaker et al. ( 2012 ). In Suess et al. ( 2019 ), we found that there was a significant trend between color gradient strength and stellar mass for galaxies at 1.0 ≤ z ≤ 2.5. Here, we find that this trend continues to lower redshifts. The only exception is in the lowest-redshift quiescent bin, where our sample is quite small. In the lower panels of Figure 1 , we also show how the best-fit relation between r e,mass / r e,light and stellar mass varies as a function of redshift for our full 0 ≲ z ≤ 2.5 sample. Figure 1. Top: color gradient strength as a function of stellar mass for two redshift intervals. Small light blue points and light red squares show individual star-forming and quiescent galaxies; large blue points and red squares show a running median. The blue and red lines show best-fit linear relations to each trend; lines are outlined in black if the slope of the relation is inconsistent with zero, and outlined in gray if the slope is consistent with zero. Dashed vertical blue and red lines show the mass completeness of the star-forming and quiescent samples. Bottom: best-fit relation between color gradient strength and stellar mass for star-forming (left) and quiescent (right) galaxies as a function of redshift. Dashed lines represent fits whose slopes are consistent with zero. We see clear redshift evolution in the best-fit color gradient-mass relations for both quiescent and star-forming galaxies. In Figure 2 , we show the median strength of color gradients for all galaxies with , the completeness limit of our full sample. In Suess et al. ( 2019 ), we showed that the strength of galaxy color gradients decreases sharply between z ∼ 2.5 and z ∼ 1. Here we find that this evolution may flatten below z ∼ 1; r e,mass / r e,light for both quiescent and star-forming galaxies remains roughly constant at a value of ∼0.7. Figure 2. Median half-mass to half-light radius ratio for star-forming and quiescent galaxies (blue circles and red squares) as a function of redshift. r mass / r light traces the strength of radial color gradients; values less than one indicate negative color gradients, where the center of the galaxy is redder than the outskirts. Only galaxies with , where our sample is complete, are included. Error bars show the central 68% of 500 bootstrap samples. The strong color gradient evolution previously observed at z ≳ 1 appears to flatten at z ≲ 1. 3. The Growth of Quiescent