  We report here the analysis of the near-infrared transit spectrum of the
hot-Jupiter HAT-P-32b which was recorded with the Wide Field Camera 3 (WFC3)
on-board the Hubble Space Telescope (HST). HAT-P-32b 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$1.6 - 1.8.
This difference is the trade-off for higher objectivity due to the lack of any
assumption about the instrument systematics compared to the parametric
approach. The ICA error-bars are therefore worst-case estimates. To interpret
the spectrum of HAT-P-32b, we used T-Rex, our fully Bayesian spectral retrieval
code. As for other hot-Jupiters, the results are consistent with the presence
of water vapor ($\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-32b.
