The *B*, *V*, *R*, *i’*, *z’* band images are taken from the archived SXDS data [@Furu08]. The CCD of Subaru/Suprime-Cam is replaced with the new CCD of Hamamatsu Photonics in 2008, and the total response function improve especially at the longer wavelength. The Subaru/Suprime-Cam *z’* band images are taken after the replacement again, and we call the images the updated-*z’* band. The limiting magnitude of the updated-*z’* images is $\sim 0.5\>\mathrm{mag}$ deeper than the archived SXDS data [@Furu16]. The *J*, *H*, and *K* band images are taken from the UKIRT Deep Sky Survey (UKIDSS: [@Law07]) DR10, and the F125W and F160W band images are taken from the Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey (CANDELS: [@Grog11]; [@Koek11]). For the data from *B* to *K* band, we use 2”-diameter aperture magnitude measured by using the SExtractor[^1] ver.2.5.0 [@BeAr96]. The smaller PSF images are convolved with Gaussian kernels to be matched in FWHM of the stars (1”.0) with the original updated-*z’* band image. On the other hand the 3.6$\>\micron$ and 4.5$\>\micron$ photometry are taken from the Spitzer Extended Deep Survey (SEDS) catalog [@Ash13] and we apply aperture correction. Finally, we pick up the objects which are in the overlapped region covered by 