who present a full-orbit phase curve in the warm Spitzer bands 3.6$\mu$m and 4.5$\mu$m. WASP-43b is classified as a giant gas planet similar to HD189733b and HD209458b but appears to show less day-night heat distribution (@2017ApJ...835..198K) despite orbiting closer to its host star compared to HD189733b (a$\approx 0.0031$au) and HD209458b (a$\approx 0.0047$au). We note that both, HD189733b and HD209458b, have smaller mean bulk densities of 1.8 g cm$^{-3}$ and 0.616 g cm$^{-3}$, respectively (Table 1 in [@2016MNRAS.460..855H]). [@2015ApJ...801...86K] and [@2014Sci...346..838S; @2017AJ....153...68S] point out that the day-side phase curve can be fitted with a cloud-free GCM but such a GCM predicts too high flux on the nightside. [@2018ApJ...869..107M] discuss non-equilibrium chemistry caused by advection for CO, , , and , suggesting a general advection driven overabundance of CO and for a high C/O=2.0, and for on the night side if C/O=0.5. [@2019AJ....157..205M] reanalysed the WASP-43b data suggesting a nightside brightness between the results of [@2017AJ....153...68S] and [@2018ApJ...869..107M]. [ [@kchubb2019] performed a re-analysis of the HST/WFC3 and Spitzer/IRAC transmission data for WASP-43b using all available opacity data, and report the detection of AlO and H$_2$O in transmission with a high statistical significance. No evidence for the presence of , nor in transmission 