The Askania-Zeiss Abrahão de Moraes meridian circle, operated at the
IAG/USP Valinhos Observatory (,
),
is a 0.19 m refractor instrument with a focal distance of 2.6 m.
A CCD detector Thomson 7895A with
pixel matrix and a pixel scale of /pixel
was used for the imaging (Paper I,
Viateau et al. 1999).
The observations are performed in a drift-scanning mode.
So the integration time, for a declination ,
is given by

(1) |

The optimal magnitude interval for the observations is , while the typical accuracy in the positions and magnitudes for a single measurement of a given night is shown in Fig. 1 of Paper I.

The filter we have used in this and other observational programmes is somewhat wider than the standard Johnson filter ; allowing a larger coverage towards the infrared band in order to maximize the number of objects by taking advantage of the better quantum efficiency of the CCD in that region. Figure 2 of Paper I shows the response of the Valinhos filter together with the standard Johnson filter . The correlation between the filters, the method used for our programme and the limitations are described in Paper I. In the present work we have used the differences of magnitudes of the stars with respect to a standard reference set, as described in the next section.

The employed data reduction method requires a first
step, where the sky background is subtracted by a linear polynomial fitted to
each pixel column. Objects are identified when 3 consecutive pixels with a
confidence level are detected, where
is the standard deviation of the mean count rate in each
column. A two-dimensional Gaussian surface is fitted to the flux distribution of
the objects, to
obtain the *x* and *y* coordinates of the centroid, the flux and
respective errors (Paper I,
Viateau et al. 1999).
In the following step, the celestial positions and magnitudes are
calculated by solving a system (Eqs. (3-5) in Paper I) with respect
to reference stars (Sect. 4).
For our variability analysis we take these results, i.e.,
those obtained in the classical way, night-by-night.

After this process, the system is again solved in an iterative process, now for all stars detected in the field, by a global reduction, using the field overlap constraint among all observation nights (Eichhorn 1960; Benevides-Soares & Teixeira 1992 and Teixeira et al. 1992). At each step of iteration, the system is solved by least squares (Benevides-Soares & Teixeira; Teixeira et al. 1992). The process converges in a few iterations (typically less than 10 steps). This method is applied to obtain the best values to the positions, as can be seen in Appendix B.

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