Gas and dust obscured AGN in the early universe is an important population which could represent an early violent formation/growth phase of SMBHs and their host spheroidal components. A recent study utilizing the wide and deep (5.3 deg2, ∼50 ks) X-ray survey catalog (XMM-SERVS; Chen+18) shows that 76−3+4% of high-z luminous AGN (z>2, logLX (erg s−1)>44.5) are obscured (logNH (cm−2)>22), and the obscured fraction is increasing with increasing redshift (see Vijarnwannaluk+22). Therefore, it is possible that many luminous AGN are so obscured that they could be undetectable even in the hard X-ray band (i.e., heavily obscured AGN) at high-redshift (z>3) and the contribution of such population to over all SMBHs growth rate at the redshifts. Thus, we conducted a search for heavily obscured z>3 luminous AGN focusing on an AGN feature in the NIR-MIR band on the SED, and conducted a SED fitting analysis for the selected candidates. In this program, we propose the spectroscopic follow-up observation for selected AGN candidates.
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