All Tables

Table 1: Details of the CFDF images used in this study. For the 03 hr and 14 hr fields, we list the $3\sigma$ detection limit inside an aperture of 3'' for images convolved to the worst seeing (i.e. 1.3'' for 03 hr and 1.4'' for 14 hr). For the 22 hr field, we list the $3\sigma$ detection limit inside an aperture of 4'' for un-convolved images.
Table 2: Differential number counts, N, and surface density, n (in arcmin^-2), of Lyman-break galaxies in the CFDF fields, for a range of I_AB-selected slices. The mean surface density, labelled CFDF, is also given. Errors in the surface density measurements for each individual field are computed using Poisson counting statistics; field-to-field variance is used to estimate the error in the mean.
Table 3: Observed and simulated surface densities of objects (in arcmin^-2) recovered using the selection box (Eq. (1)), based on simulations described in Sect. 3.3 and observations in the CFDF-14 hr field. We also estimate the fraction of Lyman-break galaxies (LBG) recovered using this selection box from the total galaxy population in this redshift range. Additionally, we present the fraction of contaminants within this selection box by interlopers (lower-redshift galaxies) outside our redshift range (2.9<z<3.4) and by interlopers with z<2 and by stars.
Table 4: Comparison for different redshift ranges between objects falling within Steidel et al.'s selection box and objects selected in Steidel et al.'s box which also lie within the CFDF selection box (Eq. (1)) for I_AB<24.5.
Table 5: The amplitude of ${\omega (\theta )}$ at 1 degree, ${A_\omega }$ , the slope $\delta$ and the comoving correlation length r₀ (in h^-1 Mpc), for each field and for different magnitude limited samples considered in this paper. r₀ measurements are computed for three standard cosmological models. To derive r₀ we assume a top-hat redshift distribution centred at $\overline z = 3.2$ and the best fitted value of the slope. Result marked as CFDF mean are computed from the mean over all three fields. The error bars shown correspond to Poisson error bars. An extra systematic errorbar arising from our uncertainty in the underlying redshift range of our Lyman-break sources of $\pm 0.2$ for the entire faint samples and of $\pm 0.4$ for the bright sample should be added. (Our principal results are highlighted in bold.)
Table 6: Bias for each field and for each magnitude limited sample considered in this paper, for $\overline z = 3.2$ and for the best fitting value of the slope. The result marked as "CFDF mean'' is computed from the mean over all three fields. The error bars shown correspond to Poisson error bars. To account for our uncertainty in the underlying redshift distribution of our Lyman-break sources, an extra systematic error of $\pm 0.1$ for the whole and faint samples and of $\pm 0.2$ for the bright sample should be added.