All Tables

Table 1: Narrowband surveys for Ly $\alpha$ at z = 5.7.
Table 2: WFILAS fields, filter set exposure times and detection limits. The entries under each field heading list: (a) the total exposure time (ks), (b) the flux for a 2 $\sigma$ detection on 6 pixel diameter aperture ( $\mu$ Jy) and (c) the final seeing (''), in each filter.
Table 3: The median, first and last decile of background and seeing for the WFILAS narrowband imaging for all three fields combined. One pixel corresponds to 0 $.\!\!^{\prime\prime}$ 238.
Table 5: Parameters for the single component model to SGP_8884 before convolution with the instrumental profile. We also include the parameters for the single component and the two double component models of the previously confirmed LAE S11_5236 (Westra et al. 2005). These parameters differ slightly from Westra et al., since we have subsequently corrected the spectrum of S11_5236 for slit-losses.
Table 6: The candidate list of the WFILAS survey after the selection as described in Sect. 4. From left to right are the object name, the B, R, M₈₁₅, New A, N₈₁₇ and N₈₂₄ AB-magnitudes, line flux calculated from the narrowband magnitude in which the object was detected and line luminosity. For all measurements less than $2\sigma$ the $2\sigma$ upper limit has been given.
Table 7: Calculation of the Schechter function parameter L^* and luminosity density $\mathcal{L}$ according to Ajiki et al. (2003) for their sample, our complete sample and the combination of the two. For each sample the luminosity density has been derived from the sum of the candidate luminosities divided by the corresponding survey volume. Then Eq. (2) was solved for L^*, with given $\alpha$ and $\phi ^*$ from Ajiki et al. (2003). Finally, the entire luminosity function was integrated to give the final luminosity density.