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The discovery that exoplanetary systems are common has posed the overarching question of how closely they resemble the Solar System. Although we have learned of many cases with dramatic differences comma this perspective may be more a product of selection effects than of the general population. Systems where we can achieve au (or even sub-au) resolution hold the keys to understanding exoplanetary system structure at the necessary scale. At 7.7 parsecs comma Vega enables one of the highest spatial resolution imaging opportunities of all exoplanetary systems. For example comma its Kuiper-belt analog ring located at virgul 120 au is at an angular separation of 16.9.. comma while its Asteroid-belt analog is at virgul 12 au (corresponding to 1.6..). Giant and ice-giant planets will also likely be outward of 30 au (virgul 4..) from the central star. At these angular distances comma the STIS coronagraph has excellent imaging contrast. Furthermore comma the luminous host star provides ample flux at optical wavelengths for the dust and planetary bodies in the system to scatter. Despite these attributes comma the Vega disk has never been imaged with HST comma and attempts to image its planets in scattered light integrated only deep enough to detect planets with radii above 3.6 R_Jupiter (at which sizes gas giants are not expected to exist). We propose a single heritage HST program that will provide a deep and complete characterization of the Vega debris and planetary system. Our program is designed to image the disk components and any Jupiter analogs outward of 30 au comma assuming conservative albedo values. Our HST observations will complement JWST GTO Cycle 1 observations of the system with NIRCam and MIRI and existing ALMA observations.