After its discovery, Helene was observed in 1980-81 (Reitsema 1981) and from 1981 to 1985 by Veillet (Oberti et al. 1989). In total, there are 233 published positions of this satellite. Some observations made in 1992 and 1994 are informed by Rodhe & Pascu (1993, 1994).

An analytical theory for the motion of Helene was presented by Oberti (1990). After 1995 a numerical integration of this longitude: , latitude: and altitude: 1 872 m. The plates are the same used in our observations of the large satellites of Saturn. All plates were hypersensitized and the exposure times have varied from 8 to 12 minutes. No filters or masks on the plates were used. For some details about the observations see Paper I.

The images of the satellite, the stars and the other satellites of Saturn were digitized with the PDS 1010A of the Observatório Nacional-Brazil. For the images scans a square slit with 20 m of side was used. To find the center of these images, the ASTROL routines package (Colas & Serrau 1993) was employed and to determine each center, a two-dimensional Gaussian fitting on a small circular area around the image in which the background was removed by a second-degree polynomial, was used. The errors upon the centering procedure were smaller than 0 03 for Helene.

For the astrometric calibration we used the method presented in Paper I. The observed positions of Helene are referred to Titan in the reference system J2000. In Paper I, it can be seen that the positions of the large satellites of Saturn have errors smaller than 0 2 when their positions are compared with TASS1.7 (Vienne & Duriez 1998). Therefore, it is considered that the errors induced by the reduction procedure are smaller than 0 2. In Table 1, our positions of Helene related to Titan are presented.

The theoretical positions for Helene and Titan were provided by Jacobson from JPL (Jacobson 1999). We inspected all our plates of the Saturnian system (Paper I) in order to identify images of any faint image in the regions around the Dione's Lagrangian points. We found only 32 measurable objects in these plates.

To select the images of Helene from the 32 candidates measured,
we compared these observed positions with the
theoretical one. We can observe in a plot (Fig. 1) where the
axes are the
and
that there is a cluster of
points in the neighbohood of the origin, while the other points
are spread over the plot. We considered only the positions
belonging to the central cluster. These positions of the candidates
to Helene images were also compared with the positions of stars
(with *B* and *R* magnitudes smaller than 20) from the USNO A2.0 Catalog
(Monet et al. 1998) in the same field, in order to insure that
they are not stellar.

The residuals for our observed positions of Helene compared with
theoretical positions have
,
,
and
.
In Fig. 2 the histogram for the residuals
*x* and *y*, is presented. It can be noted that the standard deviation
in the *x* direction is larger than for the *y* direction. This is due to
guiding problems.

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