All Tables

Table 1: Exposure times and number of exposures for the HDF-S LSB candidate sample observed with ESO 3.6 m telescope.
Table 2: Measurements for the emission lines of the LSB candidate sample. All entries which are marked with ^a were not used for the estimation of the mean redshift $\langle z\rangle$ and therefore also not for the estimation of the standard deviation $\sigma _z$ . All lines which were either influenced by night sky emission lines or which had only upper limits were also not used for the determination of the mean redshift. It was not possible to resolve the two component of the [S II]-doublet. Therefore [S II] was not used in order to estimate redshifts. The redshift of LSB J22324-60520 (marked with ^b) was estimated measuring the wavelength of the Ca II-K absorption line.
Table 3: Measured (e.g., $r_{\rm m}$ measured radii) and calculated parameters of the observed HDF-S galaxy sample. The parameters in Cols. 4, 5, 7, 8, 9 and 10 are calculated using Eqs. (1) to (10) (see also description in Sect. 3.1).
Table 4: List of the galaxies which were selected as LSB candidates using color-color diagrams. The last column marks whether the candidate, after analyzing the spectroscopic information, is a true LSB galaxy or not. The central surface brightness in Col. 6 is corrected against fading due to "Tolman-Dimming''.
Table 5: Results of the strong-line method, derived using the semi-empirical calibration described in McGaugh (1994) and de Naray et al. (2004). Columns 2 to 6 show the measured equivalent width (including errors) for the LSB galaxy sample). Columns 7 to 9 gives the logarithm of the emission line relations as used in the R₂₃ method, Col. 10 gives the oxygen abundances and the last column shows the oxygen abundance in terms of solar abundance. The values of log([N II]/[O II]) are derived using upper limits for the [N II] measurements. The metallicities are derived from the lower branch values for log([N II]/[O II]) < -1 and from the upper branch for log([N II]/[O II]) > -1.