The EROS-1 experiment (Arnaud et al. 1994a,b) was motivated by the study of dark compact objects in the dark halo of our Galaxy and contributed to show that the so-called brown dwarves could not be a significant component of the dark matter (Renault et al. 1997).
This dataset, treated in Paper I, is composed of some 1000 images per CCD and per colour spread over 120 days. Only 10 CCD fields were available in 91-92, so we restrict our analysis to this field of 0.25 deg2.
The data are then arranged in super-pixel light curves, and an empiric seeing correction is then applied to each light curve. The limitations of this technique reside in the conversion of pixel fluxes in magnitudes, which can be done efficiently with kernel convolution techniques developed by Tomaney Crotts (1996) and Alard (1998). Due the large filters of the EROS database and the short baseline (120 days) available with this data set, we choose to postpone this step to the next paper, which will produce periods with 3-years light curves together with a cross-identification with the DENIS photometry. In this paper, we provide a magnitude estimate for one epoch, together with an indication of blending, and put the emphasis on the selection procedure and the cross-identification with other catalogues.
The light curves we use in the following to select variable stars
correspond to the super-pixel flux
measured at different
|(0) Starting point after||excision|
|(1) Min( , )|
|(3) Clusters identification|
|Min( , )|
|> 4||999 (0.05%)|
|> 10||544 (0.03%)|
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