Accuracy of the hscpipe PSF photometry for synthetic stars measured by the difference between input and output forced PSF magnitudes. Plots (a), (b), (c), (d), and (e) show the results for the g, r, i, z, and y band, respectively. The left-hand panel in each plot shows the relation between input magnitude and magnitude difference. Filled and open contours are for the synthetic galaxies from goodSeeing and badSeeing tracts. Highly blended stars with b > 0.05 are highlighted using scattered points. The long-dashed lines mark zero magnitude difference, while the pairs of dashed lines outline the running-median of PSF magnitude errors (including the uncertainties in aperture correction). The right-hand panel in each plot shows the distributions of the magnitude differences for objects in goodSeeing (filled) and badSeeing (solid line) tracts. The dashed lines identify the distribution of highly blended objects. (Color online)