selection does not cause the strong bias in the $\beta$ distribution except for the extremely faint and blue objects. In order to quantify and discuss the influence, we estimate the recovery fraction in section \[S4s2RF\].

![ Model spectra and important broad-band filters. In the top panel, the green, blue, and red solid lines represent the model spectrum at *z* $=$ 3, 4, and 5, respectively, which clearly show the Lyman and Balmer breaks. The length of the black horizontal line denotes the wavelength coverage of Subaru/*i’*, Subaru/*z’*, and UKIRT/*J* band filters which are used for calculating the UV slope $\beta$. In the bottom panel, we show the Subaru/*BVRi’z’* and UKIRT/*JHK* band filters from left to right. For the sake of clarity, the filter responses of UKIRT/*JHK* are multiplied by an arbitrary constant. []{data-label="fig4"}](Pic.speccomp5-multi.eps){width="80mm"}

Results {#S4Rslt}
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![ Observed UV slope $\beta$ vs. UV absolute magnitude at rest-frame 1500Å ($\beta$–$M_{\mathrm{UV}}$ relation). The UV absolute magnitude is calculated by integrating the flux of the best-fit SED model template from rest-frame 1450Å to 1550Å. The green filled circles represent the individual objects in the area of the SEDS (Spitzer field) and the blue filled squares represent the individual objects out of the area. 