This paper presents scanning Perot-Fabry observations of ionized gas in 11
elliptical and lenticular galaxies. We show monochromatic and velocity maps
for each object. Using the model developed by de Zeeuw and Franx in 1989,
we could give informations about the geometrical aspect of the triaxial
ellipsoid such as viewing angles and axis ratios. But this calculation gives
interesting results (narrow possible viewing angles regions) only if gas and
stars major axis are not aligned, if not regions are too wide to give any
valuable information. Three galaxies of our sample show a
complex system of
double gaseous components: NGC 708, NGC 1052 and NGC 7332. The presence of
such multiple components addresses the question of gas origin and fate. This
implies an external origin of the gas, at least for a part of the gas
content. One scenario is to imagine that the galaxy had several encounters
during his life. The case of NGC 708 is certainly the most interesting,
because one component is aligned with the stars and the other is decoupled.
In that case the cooling flow hypothesis can not explain the presence of
such gaseous components. On another hand two objects, NGC 404 and NGC 2974
show a perfect agreement between gas and stars which can be candidates for
internal origin.
Monochromatic maps give us the possibility to have
ionized gas masses. The range of the masses is between 
and 
, which is few in comparison with the total mass of the
galaxy estimated from the maximal gas velocity (cf. Table 5 (click here)). As
Buson et al.
(1993) analysis, our sample shows that H
luminosity is 10 to 100
times larger than the spectroscopic survey from Phillips et al. (1986). It
can mean that galaxies gas content is simply larger or that a higher
fraction of gas has been ionized. The gas distribution is also quite
different between galaxies.
In a forcoming paper we will discuss more deeply the
interpretation we can give for galaxy shape and orientation of elliptical
galaxies.
Acknowledgements
We wish to thank the Local Allocation Time Committee of the Special Astrophysical Observatory (Russia) as well as Drs. V. Afanasiev, A. Burenkov, S. Dodonov, V. Vlasiuk and Mr S. Drabek who helped us efficiently and built partially a local CIGALE instrument indispensable for the observations. We also want to thank M. Marcelin for his help in the writing of this article.