  The star EZ Peg, long ago classified as cataclysmic variable, has been shown
to be a chromospherically active binary system of the RS CVn-type. In this
paper we have analysed, using the spectral subtraction technique, simultaneous
spectroscopic observations of the H_alpha, H_beta, Na I D_{1} and D_{2}, He I
D_{3}, Mg I b triplet, Ca II H & K, and Ca II infrared triplet lines. We have
found that the hot component is the active star of the system, showing strong
emission in the H_alpha, Ca II H & K, H_epsilon, and Ca II IRT lines, and a
strong filling-in of the H_beta line, however the Na I D_{1} and D_{2} and Mg I
b triplet lines do not present filled-in. The He I D_{3} could present a total
filling-in due to microflaring. The observed variations (in different epochs
and with the orbital phase) of the different activity indicators, formed at
different height in the chromosphere, are correlated. Very broad wings have
been found in the subtracted profiles of H_alpha and Ca II IRT lambda 8498 and
lambda 8662 lines. These profiles are well matched using a two-component
Gaussian fit (narrow and broad) and the broad component could be interpreted as
arising from microflaring. The higher luminosity class of the hot component,
that our spectra seem to indicate, could explain why the hot component is the
active star of the system.
