The high resolution spectroscopy is a fundamental tool for the study of the structure, geometry and velocity fields of the external atmospheric envelopes of stellar systems. In the framework of many observing programmes we have collected high resolution spectra of many emission line objects belonging to different stellar categories, and some results have beeen published on particular stars and projects (e.g. Rossi et al. 1988; Rossi et al. 1991; Altamore et al. 1992; Muratorio et al. 1992; Viotti et al. 1992, 1994), but the quantity of information that can be extracted from a single spectrum is often much wider than that used for a given project. For this reason we reanalysed from a different point of view some old spectra of ours, to which new ones have been added.
In this paper we present the results of the study of the profiles
of particular lines of some emission line stars, which can be considered
as interesting members of different stellar categories: EZ CMa (WN5),
Cas (B0IVe), HD 200775 (Herbig Be), HR 8752 (G0Ia+),
AG Dra and CH Cyg (symbiotic stars), KQ Pup (VV Cep-type variable),
and R Aqr (Mira-type symbiotic star).
The observations were collected in December 1990 and January 1995
within a project of a high resolution study of peculiar,
emission line stars developed with the Aurélie spectrograph of the 1.52 m
telescope of the Observatoire de Haute Provence (OHP),
with special attention to the Balmer and He I lines,
and to the 1 
m region which includes the peculiar Fe II 1.00 m line.
The 1990 observations of AG Dra, CH Cyg and R Aqr were also
made within the RIASS campaign of coordinated ROSAT and IUE observations
of symbiotic stars (Viotti et al. 1994).
As for comparison we collected the spectra of a few additional objects:
Aqr (B1Vpe), 
CMi (B8Ve),
Ori (B8Ia), UMa (A0V),
Boo (K2IIIp), Tau (K5III), 
Aur (K4Ib-II),
VV Cep (M2Ia),
Ori (M2Iab), and Cep (M2Ia), some of which are shown in
this paper.
For long term monitored stars we compare the Aurélie observations with previous
high resolution spectrograms obtained at ESO CAT-CES.
All the reduced spectrograms and their list are available on request to CR or RV.