Comparison between the spectra of SN 2009E, SN 1987A, and models a2 and a4 around the time of maximum brightness. We also overplot model X (used to model the low energy Type II-P SN 2008bk; Lisakov et al. 2017) to show that a lower energy than used for model a2 is needed to explain the very narrow Hα. All spectra are normalized and shifted vertically for visibility. Observations were corrected for redshift but not for reddening.