The figure shows a fit to the ring events (red segments), with the other features the same as in Fig. 2. Those segments show the 1σ uncertainty intervals for the midtimes of the secondary events at Mount Agliale (Ag), Lajatico (L), San Marcello Pistoiese (SMP), Asiago (As), Wendelstein (W), Ondrejov (O), Konkoly (K) and Skalnate Pleso (S). No ring event could be detected from the Bavarian Public Observatory (in Munich) because of the low signal-to-noise ratio. The ring egresses at Wendelstein, Asiago, San Marcello Pistoiese and Lajatico are not observed because they are blocked by the main body. At Skalnate Pleso, the ring egress is not detected (despite the high signal-to-noise ratio of the data) either because the ring is not homogeneous or because its egress is lost in the readout time (marked here in green). The latter is the most likely explanation because the readout times of 5.5 s were long compared to the integration time of 10 s. Also, the green segment is very close to the positive Konkoly detection, making the hypothesis of an inhomogeneous ring unlikely. The two ellipses around Haumea delineate a 70-km-wide ring with an apparent opacity of 0.5 (grey area) and semi-major axis of that best simultaneously fits the secondary events of Fig. 1. The ring fit provides an opening angle B_ring = 13.8° ± 0.5° and a position angle for the apparent minor axis of the ring of P_ring = −74.3° ± 1.3°. This is aligned, to within error bars, with Haumea’s apparent minor axis P_limb = −76.3° ± 1.2° (Fig. 2). Moreover, the orbital pole position of Hi’iaka¹⁴ implies a sub-observer elevation of B_Hi’iaka = −15.7° above the orbit of Hi’iaka on 2017 January 21 and a superior conjunction occurring at a position angle of P_Hi’iaka = −73.6°. The fact that |B_ring| ≈ |B_Hi’iaka| and P_ring ≈ P_limb ≈ P_Hi’iaka strongly suggests that the ring and Hi’iaka both orbit in Haumea’s equatorial plane.