Juno UVS: Predicted OCFB location at Ganymede from fitting the bright auroral ovals

The dataset provides predictions for the surface locations of the open-close-field line-boundary (OCFB) at Ganymede during Juno's flyby, as calculated in Duling et al. (2026) (Figure 2b).

The location of the OCFB is interpreted as the locations of the brightest auroral emissions at the northern and southern ovals. A third-order Fourier series with higher order extension is fitted to pixels of integrated OI 1356 Å and OI 1304 Å brightness >100 R, as observed with Juno UVS. The pixels are weigthed by their brightness value. Only longitudes that are well covered by the observation are considered, i.e. 140°>$\lambda$>-90° (north) and 130°>$\lambda$>-20° (south). For detailed fitting information see the description in Duling et al. (2026).

The fitting result is 
\begin{equation}
      \theta_\mathrm{OCFB,fit}(\lambda)=\sum_{i=0}^{3}A_i\sin\left(i\lambda+\Delta\lambda_i\right)+\sum_{i=10}^{12}A_i\sin\left(i\lambda+\Delta\lambda_i\right)
\end{equation}
with 

The coordinate system is based on body fixed IAU_Ganymede with latitude $\theta$ and western longitude $\lambda$, with 0° being the Jupiter-facing meridian.

The data file contains the following columns:
- western longitude $\lambda$ in degree
- fitted latitude $\theta_{\mathrm{OCFB,fit}}$ of the northern oval in degree
- fitted latitude $\theta_{\mathrm{OCFB,fit}}$ of the southern oval in degree

Longitudes that are not observed and not included in the fit are indicated by values of 0.0.