than in the 15 May sighting. Fan A extended linearly to around ρ=10000 km, within ±10◦of the 2015/2016 northern pole solution (still ϕ ≃80◦N). Outside of ρ=10000 km, the fan curved significantly in the anti-sunward direction and continued to contribute to the diffuse northern component of the tail (see middle panel of Figure 4). After 31 Au16 gust 2021, Fan A was increasingly hard to detect due to the very tight FoV (∼ 10000×10000 km by 30 September)

and its diminished apparent brightness and contrast to other dust structures in the FoV. During the pre-perihelion period, an additional dust coma structure became evident. A bright and wide dust feature was seen from 18 August onwards. If we assume this structure was comprised of a single active component, it had an opening angle of ∼90◦, with a projected position angle of around 90-100◦from RFN (equatorial latitudes, ϕ ≃0◦to -10◦S). By 21 August, the structure was asymmetrical about the 18 August position measurement, which indicated it is not likely comprised of a single jet or fan, but rather a conglomerate of multiple features projected atop one another. The main component of this structure emanated to the South, hereafter designated Fan B, and extended linearly to beyond ρ=5000 km before it gently curved in the anti-sunward direction (see middle panel of Figure 4, or panels (II.) and (III.) of Figure 3. Fan B was the feature with the most contrast in the dust coma besides the dust tail. From 21 August to 30 September, Fan B increased in contrast, extended to beyond ρ=10000 km in radial extent, and remained fixed at a position angle of 140◦±5◦from RFN (ϕ ≃-35◦S). During this period, the tail remained fixed around 270◦from North, in the anti-sunward direction, and also increased in contrast to the rest of the coma. We note that this increase in contrast and apparent growth of structures is likely due to the decreasing geocentric distance, and thus increasing SNR, rather than actual growth and brightness increases in-system. Post-perihelion, our view of the comet had undergone a change in orbital plane angle from +2◦to -6◦and phase angle change from 46◦to 13◦, which significantly changed the Earth-based perception of the comet dust morphology. From 11 January to 09 March 2022, a large and wide dust structure persisted in the southern half of the dust maps, roughly along the sky-projected South Pole position angle of 67P. No prominent dust features were present in the North throughout this period. The southern dust structure exhibited finer substructure, from which we were able to fit four Voigt models and extract position angles for the first 3 epochs, presented in Table 2. We checked our retrieved position angles by computing the CWT of the fitted profile, seen in Figure C.14 in Appendix section Appendix C. We could not extract measurements of the substructure by 09 March because the cometary dust tail overlapped with the southern structures and the geocentric distance had increased by a factor of 2, which diminished the quality, contrast, and distinctiveness of the features. From East to West, we fitted four dust struc17

[Table: Table 2: Position Angles of Post-perihelion Dust Fans]

|  | Table 2: Position Angles of Post-perihelion Dust Fans |
| --- | --- |
| Fan | Position Angle (◦) Latitude ϕ (◦, S) σPA (◦) |