Sun-to-PSP connectivity maps for the first (October–November 2018), second (March–April 2019), and fourth (January–February 2020) encounters (top, middle, and bottom row, respectively). Connectivity is computed by projecting the solar wind speed measured at PSP backwards to the surface of the Sun, considering the most likely Parker spiral, accounting for solar wind travel time and connecting to coronal field reconstructions based on magnetograms corresponding to the expected solar wind release times. The left panels display Carrington maps of EUV emission (SDO/AIA 193Å) overlaid with the most probable footpoints (solar wind source positions, coloured circles) at the surface of the Sun for the dates indicated, and the centroid of the connectivity probability distribution at 5 R_⊙ (coloured stars). The cyan line indicates the trajectories of the 2.5 R_⊙ connectivity point. The coloured dotted lines are visual aids to connect source-surface to surface positions (but do not trace the actual field-line trajectories). Date labels indicate in situ solar wind measurement times. The right panels show similar maps of white light emission at 5 R_⊙ (SoHO/LASCO C3), overlaid with similar markers (at 5 R_⊙). The red dashed line represents the neutral line (base of the HCS) obtained from PFSS extrapolation of ADAPT/GONG maps. PSP spent a significant fraction of its first passages sampling solar wind streams that developed at the vicinity of predominantly azimuthally aligned CH–streamer boundaries, and that propagated through the heliospheric plasma sheet (in close proximity to the HCS, within the bright streamer belt region).