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In this paper an analytical theory is used to complete the transmissionspectrum of HD189733b from near-ultraviolet to infrared (0.33 - 7.85 $\mu m$).The model suggests a new approach which take into account the quantity of lighttransmitted through the planetary atmosphere and the thermal emissions from thenight side of the planet, to describe the transmission spectrum of HD189733b inphotometric study. The availability of measures in different wavelengths hasallowed us to validate our model with more efficiency. We found an agreementbetween our transmission spectrum model of HD189733b and data from the infraredto the UV. The model predicts a value of $R_p /R_\star$ $= 0.1516$ at $7.3 \mum$, which is a low value compared to all observations at different wavelengths.We interpreted this value by a fluorescence emission from sulphur dioxide($SO_2$). Therefore, the likely presence of these molecules in the atmosphereof HD 189733b. The second objective of this paper is to study the effect ofstarspots on the transmission spectrum of this hot-Jupiter. To reach this goal,we developed an analytical theory considered as an extension of the approachproposed by Berta et al. (2011). The model shows clearly that the unoccultedspots would significantly increase the transit radius ratio at visible andnear-ultraviolet wavelengths, while having a minimal impact at infraredwavelengths. Therefore, the wavelength dependence of the spots effect has beenclearly shown by this new model. At the end of this paper, we reported the wayin which this model can provide an estimation of the percentage of theunocculted spots area relative to stellar disk area for an observation ofHD189733 performed in a given epoch and at a given wavelength.

An analytical model for the 0.33 - 7.85 micron transmission spectrum of HD189733b : Effect of stellar spots