All Tables

Table 1: Location, median seeing and field of view (in sq. degree) of the 3 CFHTLS fields studied here.
Table 2: Galaxy contamination of the D1 field cross-identified with the VVDS field as a function of i' magnitude and r'-i' colour. The common area is $\sim$ 0.4 sq degree.
Table 3: Positions and MEGACAM photometry of late type dwarfs or high redshift quasars.
Table 4: Number of stars in the D1 field for i' < 21 and in different intervals of r'-i'. Column 1 indicates the middle of the interval of width 0.2, "tot'' means the total of the 3 interval considered, that is 1.5< r'-i'<2.1. Columns 2 to 17 give the model counts for each of the tested LF while column 18 contains the observed counts. Models are described by two parameters: on the first line of the column heading the value of the mass of changing slope is indicated, the second line gives the value of $\alpha$ (see Eq. (1)). The column values include, in the first line, the number of stars in the colour interval, the second line gives the difference between the data and simulated counts in number of sigmas, assuming that the noise is dominated by the Poisson statistics (see text). Model with values between -3 and +3 are considered as acceptable in the colour bin.
Table 5: Same as Table 4 but for field D2.
Table 6: Same as Table 4 but for field D3.