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While Euclid is an ESA mission specifically designed to investigate thenature of Dark Energy and Dark Matter, the planned unprecedented combination ofsurvey area ($\sim15\,000$ deg$^2$), spatial resolution, low sky-background,and depth also make Euclid an excellent space observatory for the study of thelow surface brightness Universe. Scientific exploitation of the extended lowsurface brightness structures requires dedicated calibration procedures yet tobe tested.  We investigate the capabilities of Euclid to detect extended low surfacebrightness structure by identifying and quantifying sky background sources andstray-light contamination. We test the feasibility of generating skyflat-fields to reduce large-scale residual gradients in order to reveal theextended emission of galaxies observed in the Euclid Survey.  We simulate a realistic set of Euclid/VIS observations, taking into accountboth instrumental and astronomical sources of contamination, including cosmicrays, stray-light, zodiacal light, ISM, and the CIB, while simulating theeffects of the presence of background sources in the FOV.  We demonstrate that a combination of calibration lamps, sky flats andself-calibration would enable recovery of emission at a limiting surfacebrightness magnitude of $\mu=29.5^{+0.08}_{-0.27} $ mag arcsec$^{-2}$($3\sigma$, $10\times10$ arcsec$^2$) in the Wide Survey, reaching regions 2magnitudes deeper in the Deep Surveys.  Euclid/VIS has the potential to be an excellent low surface brightnessobservatory. Covering the gap between pixel-to-pixel calibration lamp flats andself-calibration observations for large scales, the application of skyflat-fielding will enhance the sensitivity of the VIS detector at scales oflarger than 1 degree, up to the size of the FOV, enabling Euclid to detectextended surface brightness structures below $\mu=31$ mag arcsec$^{-2}$ andbeyond.

Euclid preparation: XVI. Exploring the ultra low-surface brightness Universe with Euclid/VIS