Authors: Phillip Hess (NRL), Erika Palmerio (PSI), Robin Colaninno (NRL), Mark Linton (NRL), Volker Bothmer (Institut für Astrophysik und Geophysik, Georg-August-Universität, Göttingen, Germany)

Coronal mass ejections (CMEs) are the largest and most energetic transient feature in the solar corona and heliosphere. High resolution imagery for the WISPR instrument on board Parker Solar Probe and the SoloHI instrument on board Solar Orbiter offer higher resolution of these structures than has ever been possible in the past. Combining images from these instruments, which observe transient structures from well inside the heliosphere, with legacy imagers from 1 AU provides the most comprehensive data to determine both CME bulk speed characteristics and study small scale, substructural features. In this poster, we utilize data from both of these heliospheric images, as well as 1 AU coronagraphs and EUV images, to understand the nature of specific substructural features seen within the CME. We also compare these structures directly PSP in-situ observations to see if we can directly link density enhancements in the various data sets. Based on the data, and triangulation of the CME from the multiple viewpoints, all indications are that the remote sensing observations are dominated by features far away from PSP as it encounters the CME.