($\phi = 270\degree$). For the anti-stellar point ($\phi = 180\degree$), we only perform the chemical simulation and do not perform the haze formation calculation because of the absence of a sufficient radiation field and hence, no photochemistry.

As for the elemental abundance ratios used in the photochemical calculation, we adopt the original solar ones. Though we have also simulated the photochemistry using the reduced oxygen abundance as a result of mineral cloud formation, we have confirmed that the depletion of the oxygen abundance in the cloud-forming region is replenished by the vertical eddy diffusion transport from the lower atmosphere with the solar abundance. However, if we are able to couple mineral cloud formation with photochemical simulation, the oxygen abundance in the cloud-forming region should be kept depleted because of the much shorter timescale of cloud formation compared to that of diffusion. Coupling those two simulations is our future work. For the UV spectrum of WASP-43, since it has not been observed, we use that of HD 85512 constructed by the MUSCLES Treasury Survey [@2016ApJ...820...89F; @Youngblood:2016ib; @2016ApJ...824..102L] because of its similar stellar type to WASP-43. The attenuation of the UV spectrum due to the wavelength-dependent molecular absorption at each altitude is 