We report here the analysis of the near-infrared transit spectrum of the hot-Jupiter HAT-P-32 b which was recorded with the Wide Field Camera 3 ( WFC3 ) on-board the Hubble Space Telescope ( HST ) .
HAT-P-32 b is one of the most inflated exoplanets discovered , making it an excellent candidate for transit spectroscopic measurements .
To obtain the transit spectrum , we have adopted different analysis methods , both parametric and non parametric ( Independent Component Analysis , ICA ) , and compared the results .
The final spectra are all consistent within 0.5 \sigma .
The uncertainties obtained with ICA are larger than those obtained with the parametric method by a factor \sim 1.6 - 1.8 .
This difference is the trade-off for higher objectivity due to the lack of any assumption about the instrument systematics compared to the parametric approach .
The ICA error-bars are therefore worst-case estimates .
To interpret the spectrum of HAT-P-32 b we used \mathcal { T } -REx , our fully Bayesian spectral retrieval code .
As for other hot-Jupiters , the results are consistent with the presence of water vapor ( \log { \text { H } _ { 2 } \text { O } } = -3.45 _ { -1.65 } ^ { +1.83 } ) , clouds ( top pressure between 5.16 and 1.73 bar ) .
Spectroscopic data over a broader wavelength range will be needed to de-correlate the mixing ratio of water vapor from clouds and identify other possible molecular species in the atmosphere of HAT-P-32 b .