Spectral sequence of SN 2019oys during re-brightening. A handful of the spectra listed in Table 1 are shown, and here on a logarithmic scale to highlight the bright narrow emission lines. Phases in rest-frame days are provided for each spectrum. A spectrum of the Type IIn SN 2015ip is shown for comparison (in red). This spectrum is from Stritzinger et al. (2012) taken at 138 days past discovery. Basically all high excitation coronal lines seen in SN 2005ip are also detected in SN 2019oys, a main difference being that our SN do not display the broad Hα line from hydrogen-rich ejecta. The spectra are normalized and offset for clarity.