both the SXDS and UDS-UKIDSS fields (see figure \[fig1\]: the overlapped region is filled by yellow slanting lines) because we need both optical and NIR photometry for estimating the UV slope $\beta$ value of *z* $\sim$ 4 galaxies. The information of the imaging data is summarized in table \[tab1\].

![ Field map of imaging data used in our analysis. The blue solid line show the sky coverage of the SXDS field; the green dot-dash line represent the sky coverage observed with Subaru/updated-*z’*; The red dash line represents the sky coverage of the UDS-UKIDSS field; the black dotted line represents the sky coverage of the UDS-CANDELS field; and the brown two-dot-dash line represents the sky coverage of the SEDS field. Our catalog consists of the objects within the area covered by all of the SXDS, updated-*z’*, and UDS field since we use the *i’*, *z’*, updated-*z’*, and *J* band photometry for estimating the UV slope $\beta$ value. This area is filled by the yellow slanting lines. []{data-label="fig1"}](Pic.Region_SXDS_new1812.eps){width="80mm"}

\[tab1\]

(1)@Furu08; (2)@Furu16; (3); (4)@Grog11; (5)@Koek11; (6)@Ash13;\
The values show the total magnitude where the completeness of the source detection is 50%.

 Sample selection and SED fitting  {#S2s2ss}
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From the photometric sample, we 