Authors: Bin Zhuang (University of New Hampshire), Noé Lugaz (University of New Hampshire), Brian E. Wood (Naval Research Laboratory), Carlos R. Braga (Applied Physics Laboratory, Johns Hopkins University), Manuela Temmer (University of Graz), Tingyu Gou (Harvard-Smithsonian Center for Astrophysics), Phillip Hess (Naval Research Laboratory), Shaheda Begum Shaik (George Mason University, Naval Research Laboratory), Cecilia Mac Cormack (NASA Goddard Space Flight Center, The Catholic University of America), and Xialei Li (Auburn University)

Coronal mass ejections (CMEs) are large-scale eruptions of plasma and magnetic field from the Sun, often associated with solar prominences that consist of cool and dense material. Understanding the location and evolution of the prominence relative to the CME structure is important for the CME initiation and evolution through the heliosphere. Combining remote sensing observations of extreme-ultraviolet images, and white-light coronagraphs and heliospheric imagers (HIs) obtained from SDO, SOHO, STEREO-A, and Solar Orbiter, we present an analysis of the continuous tracking from the corona into interplanetary space of the substructures of a CME associated with a prominence that erupted on 2022 September 23. The prominence is found to remain bright and compact during CME propagation for more than three days. We investigate the kinematic evolution of the CME substructures as the CME propagated to around 0.5 au. We find that for the first about 0.28 au, both the CME front and prominence propagated coherently, indicating that the prominence appeared to be tied to the CME magnetic structure. Within 0.28 au, the increase in the radial size between the CME front and prominence follows a power-law distribution with an index of 0.78. We further discuss the prominence location relative to the CME structure, for example, whether it is positioned near the CME rear.