Discovery by the Hinode EUV Spectrometer (EIS) of persistent plasma upflows from Active Region (AR) peripheries raised the possibility that these flows may contribute to the slow solar wind. We have sought to clarify this suggestion by establishing the origin of the upflows and by use of magnetic field extrapolations to identify the open outflow paths. Through plasma composition measurements for the upflows at the AR sites followed by later comparison with plasma properties arriving at the ACE spacecraft at L1, we obtained evidence for upflow plasma contribution to the slow solar wind. Data were analysed for two solar rotations - CR 2065 in January. 2008 and CR 2064 in December 2007. End-to-end studies were performed for two quite different magnetic field configurations involving two active regions for which EIS measurements of AR upflow plasma composition, indicating a strong low-FIP element enhancement were compared with the solar wind composition at L1. Results will be described for these two configurations with a discussion of how the ACE plasma measurements were related to the upflow observations by the use of a back-mapping technique. The future application of Solar Orbiter remote sensing and in-situ observations to configurations of this type will then be discussed.