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The Wide Field Camera 3 is one of the instruments currently onboard theHubble Space Telescope and, since 2012, with the use of the spatial scanningtechnique, has provided the largest number of observed exoplanetary atmosphere,ranging from super-Earths to hot Jupiters. This technique enables theobservation of bright targets without saturating the sensitive detectors, butat the same time requires more complicated data reduction and calibrationtechniques to extract the planetary signal from the observations. In absence ofabsolute calibration sources, the validation of current data analysistechniques is not possible as the planetary signal is not known. Here, wedemonstrate how simulated observations can help us understand the effect ofdifferent analysis processes, and potential unknown systematics on the finaltransmission spectra of exoplanets. We test and validate the robustness of twoof the most precise WFC3 exoplanetary spectra - HD 209458 b and 55 Cancri e -against three different known and potential sources of systematics. Inaddition, we identify the horizontal shifts seen in WFC3 observations as themost important source of systematic errors in the planetary spectra, concludingthat a precision better that 1% of a pixel is necessary.

Testing known and unknown systematics in HST/WFC3 spatial scans with the Wayne simulator