7 Catalogue

LT$\&$LPV ("Red'' variable stars) represent the bulk of the stars presented in this catalogue. Figures 6 and 7 show typical light curves detected with the corresponding finding charts. Amplitudes measured over 120 days can be as low as 0.1 mag up to several magnitudes, depending on the timescale, and brightness range. The limitations (in the photometry) due to the crowding are also illustrated. The error bars (estimated in Paper I) account for the level of photon noise and other residual errors, but they do not account for the effect of crowding on the star flux. For light curves with $\phi_{\rm c}/\phi_0\le 3$, error bars are underestimated with respect to the scatter along the variation. This explains why the amplitude of variations in blue can be smaller (or comparable) than in red for a few LT$\&$LPV: the crowding is more important in blue and larger amplitudes of variation are expected on dimmer stars. Hence, we do not attempt to extract information about the amplitude, but provide magnitude estimates at one epoch with the $\phi _{\rm c}/\phi _0$ ratio. For most of them, the timescale of the variation is much longer than the period of observation, and the periodicity will not be studied here.

Table 2 contains the following informations. Column 1: The position, at J2000.0 epoch, is incorporated into the name of each variable, in accordance with IAU convention (Dickel et al. 1987); Column 2: N/X/Y: chip number Nand position (X,Y) on the chip. There were 10 chips on the EROS-1 CCD camera. Column 3: the $\phi _{\rm c}/\phi _0$ ratio in blue and red; Column 4: the $B_{\rm EROS}$ and $R_{\rm EROS}$ magnitude estimate at epoch JD = 2448678.3; Column 5: the number of stars detected by DAO in the super-pixel at epoch JD = 2448678.3 in B/R; Columns 6 and 7: the $B_{\rm EROS}$ and $R_{\rm EROS}$ magnitudes (at the same epoch) of the closest stars as estimated by DAOPHOT. Figures in bracket (on a second line) provide the magnitude of another star detected in the super-pixel. Column 8: identification with the other databases, discussed in the text. The Harvard variable numbers are given, as well as variables (WBP) detected by Wood et al. (1985).

The finding charts in red are presented for each variable in Fig. 2. They correspond to the epoch for which the stellar magnitude and blending has been studied (JD = 2448678.3). Each chart is labelled with the name of the variable. A cross indicates the position at which the variable star has been detected.