Left: e vs. ω posteriors for KOI 247.01 performed with the method from S23; namely, by directly sampling ﹩\sqrt{e}{\rm{\sin }}\omega ﹩ and ﹩\sqrt{e}{\rm{\cos }}\omega ﹩ during the transit fit with the exoplanet software. Right: e vs. ω for KOI 247.01 performed with the method described in Section 3, using the importance sampling method with the jaxoplanet software.