Left: values for ﹩\mathrm{log}({\rm{\Psi }})﹩ for GRB 230815A as determined from the light-curve turnovers at 5.5, 9, 16.7, and 21.2 GHz. Middle: values for ﹩\mathrm{log}(\chi )﹩ for GRB 230815A as determined from the light-curve turnovers at 5.5, 9, 16.7, and 21.2 GHz. Right: values for ﹩\mathrm{log}({\rm{\Psi }})﹩ for GRB 230815A as a function of time in days postburst. For each panel, blue circular markers are used for measurements that assume an ISM environment and a jet break at 0.1 days postburst (corresponding to the X-ray jet break); blue star markers are used for measurements that assume an ISM environment and no jet break yet at 400 days postburst (corresponding to the observed radio behavior); and the orange square markers are used for measurements that assume a stellar wind environment. For the left and middle panels, the shaded regions correspond to the 1σ confidence intervals centered on the weighted averages (the solid vertical lines) of the Ψ and χ values, respectively, for the R. A. Duncan et al. (2023) sample in the ISM (blue) and stellar wind (orange) environments. The red dashed line in each panel represents where ν_m passes ν_a (see Section 3.4); this is likely responsible for the apparent evolution of the parameters.