1 Introduction

Although the HIPPARCOS system will make remarkable achievements, there are many things to do after HIPPARCOS (Clauzet et al. 1990; Kovalevsky 1991), such as: the improvement of fundamental reference systems of stars, the extension of fundamental catalogue to faint stars, the maintenance of the HIPPARCOS reference system, the extension of HIPPARCOS catalogue.

The automatized photoelectric astrolabe (here-after ASPHO) at the "Observatoire du Calern" (OCA, $\phi$ = $+43^{\rm o}44^{\hbox{$^\prime$}} 55.011^{\hbox{$^{\prime\prime}$}}$; $\lambda$ = $-0^{\rm h}27^{\rm m}42.44^{\rm s}$, Calern, Caussols, France) observed two years at two zenith distances ($30^{\rm o}$ and $45^{\rm o}$) which turns it able to determine absolute declinations of stars (Martin & Leister 1997). One must note that automatization not only gave to ASPHO a real impersonality, but also a very much improved output, particularly during the long winter nights.

After July 1993, the pillar made in concret was replaced by a crude metalic pillar. Thus, the thermal problems in the ASPHO were diminished and was possible to put an elevator to the mercury basin. This made possible the observations at $30^{\rm o}$ and $45^{\rm o}$ zenithal distances.

The stars are arranged in two different observational programmes (ASPHOI and ASPHOII), in 11 groups of fixed composition with the best azimuth repartition.

In the period 1993-1996, 41648 stars transits were observed in the declination zone $-2^{\rm o}$ to $88^{\rm o}$. The catalogues composition are 169 stars at ASPHOI ($30^{\rm o}$) and 180 at ASPHOII ($45^{\rm o}$)having a total of 349 stars.

In this total was included 84 stars at almost maxima digression condition and 62 that were common at the two catalogues.

With this set of data it was possible to determine 185 absolute declinations ($\delta _{\rm abs}$). Our method allows to obtain the declination corrections of all stars.

In this paper we consider all the programme stars in the global reduction method (Martin et al. 1996; Martin & Leister 1997). We accomplished the global reduction due the small number of common stars in the catalogues observed at two zenith distances.

Despite the fact that the number of stars is small, this method allowed a better evaluation of the observational set. We obtained a better definition of the errors involved in the process and a global definition of the colour and magnitude equations; furthermore we were able to get directly the equator correction ($\eta$) and the declination correction ($\Delta\delta$).