Authors: Nathalia Alzate (GSFC/ADNET), Huw Morgan (Aberystwyth U.), Daniel Seaton (SwRI), Barbara Thompson (NASA GSFC), Teresa Nieves-Chinchilla (NASA GSFC) and Simone Di Matteo (NASA GSFC/Catholic U.)

Understanding the Sun/Corona/Heliosphere system requires effectively establishing a link between in situ measurements and remote observations by characterizing structure and plasma properties of the inner corona.  Further, we need to resolve the line-of-sight limitations of coronagraph and EUV observations to properly identify the location of structures and their temporal density changes.  Our advanced image processing techniques can reveal structures (on various timescales) in both EUV and visible-light data providing continuous tracking of brightness enhancements from the coronal base out to the radial extended corona.  Additionally, the uninterrupted field of view enables profiling the likely non-radial trajectory of outflows within streamers.  Our most recent work using STEREO/COR1 and GOES-R/SUVI has proven crucial in linking the low to high corona and has facilitated the interpretation of PSP data.  Further, our time-dependent rotational tomography of coronal data yields empirically derived coronal density distribution directly comparable to PSP measurements at perihelion.  We present our current work that combines PSP data with RS EUV/WL observations of the corona, via the use of coronal rotational tomography from SOHO/LASCO and STEREO/COR2 observations, which provides the capabilities to reconstruct features in the solar wind and subsequently study the evolution between EUV/WL and in situ of the plasma flows that give rise to them.