fans from 2022 (top panel) and 2016 (bottom panel). The red, lime, yellow, and white arrows are the same annotations as Figures 3 through 8. The concentric rings denote cometocentric distance, in units of kilometres. The purple dashed line corresponds to active region between -10◦to -30◦S. The orange dashed line corresponds to -40◦to -50◦S. The yellow dashed line corresponds to -60◦to -80◦S. The cyan line is the South Pole of 67P. Binning is 1×1.]

One advantage of Laplacian filtering in Boehnhardt et al. (2024) is the detection of very dim and sharp structures in the coma, generally beyond what division by azimuthal median can achieve. Such sensitivity allowed the detection and correlation of related fans. Instrumental artefacts, such as the cross-hatching pattern seen in several maps, prohibit us from using Laplacian filtering on our dataset. These related fans are associated with continuous ejection of material from an active source on the nucleus as it rotates, producing a conical distribution of material around the projected rotational axis. The detected fan features in Biver et al. (2023); Boehnhardt et al. (2024); Ivanova et al. (in prep.) all correspond to the sides of this ejection cone, and therefore should be mirrored about the sky-projected rotation axis. Although Boehnhardt et al. (2024) and Ivanova et al. (in prep.) find evidence of mirrored fans pre-perihelion, we do not. We do find strong evidence post-perihelion for this behaviour between Fans C and E, as they are approximately equidistant from the South Pole of 67P. Therefore, we posit that Fans C and E originate from the same active source on the nucleus, which is likely the source ϕ=-50◦to ϕ=-58◦S reported in the aforementioned works. Fans D and F likely represent one component of a mirrored fan, however, we were not able to retrieve their complementary structures robustly in our CWT maps or Voigt fits, therefore limiting the speculation to their origin and sublimation latitude. Despite this, Fan D is closer to the South Pole of 67P, thus implying a higher sublimation latitude, likely on par with –70◦S to –80◦S, reported in Biver et al. (2019) and Boehnhardt et al. (2024). Fan F is further from the South Pole, likely correlating to the -10◦ to -30◦S sublimation zones found in both their and our work. We do not observe evidence of mirrored fans in our gas maps, however, we note a strong correlation between the pre-perihelion northern NH2 structure and Fan A. We also find a significant post-perihelion relationship between all gas species and dust fans, though disentangling the post-perihelion interactions remains challenging. Boehnhardt et al. (2024) similarly reported a pre-perihelion dust structure with clockwise curvature originating from northern regions of 67P, identifying a source at ϕ = 40◦N. This latitude is approximately 40◦south of the active region proposed in our study, a discrepancy we attribute to our limited sensitivity to mirrored fans, which reduced the precision of latitude conversions. Despite this limitation, our Fan A and NH2 structure align well with the eastern component of the mirrored fan described in Boehnhardt et al. (2024), possibly indicating a shared activity source for dust particles and NH2 around ϕ = 40◦N. Further correlations can 38 be drawn to in-situ findings by Biver et al.