The Be shell star zeta Tauri is a bright star with an extensive observational history, especially in the ProAm community. Attracted by this huge interest I have tried to record a spectrum of this famous star with my low budget, low resolution set up (50 spectra were stacked and processed with VSpec and RSpec).
I have compared the spectrum of zeta Tauri with the spectrum of beta Psc, which is an "ordinary" Be star:
The He I absorption lines (generated in the circumstellar disk ?) are well visible and distinguish this shell star from the Be star beta Psc.
To check, if the determination of the equivalent width would deliver meaningful data, I have compared the H alpha line with a high resolution line profile that was aquired at Dec. 20th by Bryssinck from the BeSS database (http://basebe.obspm.fr/basebe/):
In theory, the measured equivalent width should be independent from spectrometer dispersion but this is obviously not the case here. It would be interesting to see other low resolution spectra of zeta Tauri. Perhaps it is possible to follow the long term variability of the H alpha EW at least semi-quantitatively??