other hand, the objects in the sub-sample (i) and (iii) are the potential LBGs at $3.5 \leq z_{phot} < 4.5$. We check the influence of the sub-sample (i) and (iii) on the UV slope $\beta$, the UV magnitude, and the other quantities, and consequently we confirm that the $\sim$ 300 objects excluded by the criteria (5) does not change our results and the criteria (5) is reasonable.

\[tab2\]

For the investigation of photometric redshift and stellar population, we use the Hyperz[^2] photometric redshift code ver.1.1 [@Bolz00] with the @Bruz03 templates[^3] (hereafter BC03) and the STARBURST99[^4] [@Leit99] templates (hereafter SB99). The BC03 templates are chosen as ”typical galaxy” models and constructed from five different star formation histories (SFHs), thirty age values, and three metallicity values with the Chabrier Initial Mass Function (IMF). The SB99 templates are adopted as ”young star-forming galaxy” models and constructed from two SFHs, thirty age values, four metallicity values, and two extreme nebular continuum cases with the Kroupa IMF. In the run of the Hyperz, the dust attenuation value, Av, is ranged from 0.0 to 3.0 with $\Delta \mathrm{Av} = 0.1$ assuming the @Calz00 attenuation law for dust extinction curve. The details of the parameters are summarized 