One of the main high level scientific questions of the Solar Orbiter mission is how the Sun creates and controls the heliosphere. A deeper understanding of the origin of the Slow Solar Wind is essential to start tackling this question. With Solar Orbiter, it will be possible to observe the Sun with high spatio-temporal resolution using instruments with active region sized fields of view. Effective target selection is therefore essential for studies of the origin of the Solar Wind that is later measured in-situ. Here, we use in-situ particle measurements taken at L1 (ACE, WIND) to then simulate the trajectory and time taken by the plasma up to the point where it ceased to co-rotate with the Sun and started expanding radially. We can then use these estimates to identify the relevant images taken by remote sensing spacecraft (Hinode, SDO, STEREO). Photospheric observations are then used to constrain a coronal magnetic field model, and the magnetic field lines which are connected to the point at the source surface are tracked down to the solar surface. The variability in the measured intensity of the region around the footpoints will then be compared to the observed variability present in the in-situ datasets. This will enable us to correlate features observed at the Sun during their emission and the properties of the associated particle populations measured at L1.