(a) Emission areas of SGR J1550−5418, SGR 1900+14, and SGR 1806−20 vs. hot and cold blackbody temperatures. ﹩{R}^{2}\propto {T}^{-3}﹩ and ﹩{R}^{2}\propto {T}^{-4}﹩ are drawn with dashed and solid lines respectively for comparison only. Data points with lighter colors are associated with large propagated uncertainty in R² (i.e., ﹩\delta {R}^{2}/{R}^{2}\geqslant 1﹩). Note that R² errors are propagated neglecting the covariance terms and are thus overestimated. (b) Emission area of SGR 1806−20 vs. hot and cold blackbody temperatures grouped by total flux values with corresponding broken power-law fits. Break indices in kT space (keV) are shown with color-coded arrows. (c) Emission area of SGR J1550−5418 vs. hot and cold blackbody temperatures with fits to a broken power law (red dashed line) and a linear model (black dashed line). Arrows represent the break energy in kT space (keV). (d) Emission area of SGR 1900+14 vs. hot and cold blackbody temperatures with a broken power-law fit shown by the dashed line. The break index in kT space (keV) is shown with the arrows. Note that only unsaturated bursts are included in all correlation analyses and kT uncertainties are included in the fits.