All Tables

Table 1: Log of the observations of the South field. They were taken on January, $1{\rm st}$ 1997, under proposal number 6437, PI Robert P. Kirshner.
Table 2: Log of the observations of the West field. The proposal number is 6033, PI Jeremy Walsh.
Table 3: Spatial distribution of $\ensuremath {{E}({B}-{V})}$ colour excess as measured in the South field. In Col. 3 we report the measured rms of the $\ensuremath {{E}({B}-{V})}$ distribution, in Col. 4 the mean error on $\ensuremath {{E}({B}-{V})}$ resulting from the fitting procedure (see text), whereas Col. 5 lists the intrinsic reddening dispersion, computed as the quadratic difference of the first two quantities. The number of stars with direct extinction determination is shown in the last column.
Table 4: Distribution of $\ensuremath {{\rm H}\alpha }$ excess stars in different bins of uncertainty on the $\ensuremath {{\rm H}\alpha }$ color index m_F675W-m_F656N (see text and Fig. 8).
Table 5: Spatial distribution of different types of stars in the four chips of the South field. The Pre-Main Sequence stars included here are only those that can be identified individually, i.e. those with (m_F675W-m_F656N)>0.5. For typographical convenience we report the Poissonian uncertainty as the square root of the observed number of stars in each bin.
Table 6: Spatial distribution of different types of stars in the four chips of the West field. The Pre-Main Sequence stars included here are only those that can be identified individually, i.e. those with (m_F675W-m_F656N)>0.5.