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The Wide Field Camera 3 (WFC3) on Hubble Space Telescope (HST) is currentlyone of the most widely used instruments for observing exoplanetary atmospheres,especially with the use of the spatial scanning technique. An increasing numberof exoplanets have been studied using this technique as it enables theobservation of bright targets without saturating the sensitive detectors. Inthis work we present a new pipeline for analyzing the data obtained with thespatial scanning technique, starting from the raw data provided by theinstrument. In addition to commonly used correction techniques, we take intoaccount the geometric distortions of the instrument, whose impact may becomeimportant when combined to the scanning process. Our approach can improve thephotometric precision for existing data and also push further the limits of thespatial scanning technique, as it allows the analysis of even longer spatialscans. As an application of our method and pipeline, we present the resultsfrom a reanalysis of the spatially scanned transit spectrum of HD 209458 b. Wecalculate the transit depth per wavelength channel with an average relativeuncertainty of 40 ppm. We interpret the final spectrum with T-Rex, our fullyBayesian spectral retrieval code, which confirms the presence of water vaporand clouds in the atmosphere of HD 209458 b. The narrow wavelength range limitsour ability to disentangle the degeneracies between the fitted atmosphericparameters. Additional data over a broader spectral range are needed to addressthis issue.

A new approach to analysing HST spatial scans: the transmission spectrum of HD 209458 b