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Starbursting galaxies present the best laboratory to study the CGM since they are likely undergoing strong accretion events which trigger intense star formation-driven outflows. However comma very few observations exist that have directly imaged their CGM and quantified the fine-scale substructure. Recent ultra-deep Keck-KCWI observations have mapped optical emission lines in the CGM to a distance of over 30 kpc from IRAS08 comma a nearby starbursting galaxy with evidence for an ongoing accretion event. These KCWI observations contain bright emission line knots with sizes of order hundreds of parsecs and no evidence of stellar continuum comma implying a lack of stars. The properties of these emission knots are consistent with cool comma condensing clouds in recent simulations. However comma the sizes from KCWI are near the seeing limit comma and the continuum measurement is hampered by sky subtraction uncertainties. We aim to use HST to zoom in on this substructure in the CGM of IRAS08 and test hypotheses explaining the sub-kiloparsec features. We propose for 5 orbits of WFC3-UVIS to obtain the Halpha+CORCHETE_OPENNIICORCHETE_CLOSE (F665N) and broad-band starlight (F467M and F775W) to measure the sizes and fluxes of the CGM emission knots. These data will allow us to differentiate between three possible scenarios giving rise to these knots comma including the cool condensing clouds predicted in high resolution simulations comma external HII regions comma and dwarf galaxies. These observations are part of a larger program to directly image the optical emission lines of the CGM in starbursting galaxies. This HST imaging will therefore be a Rosetta Stone for interpreting future data as we move into the new era of direct imaging of the CGM.