活耀星系核(AGN)與其宿主星系之間的互動本質仍是一個未解之謎。因此,進行活耀星系核的普查對於其研究是非常有價值的一步。然而,大多數的活耀星系核皆被其環境遮蔽住,圍繞在中心超大質量黑洞的塵埃圓環阻擋了紫外線與可見光波段的輻射。由於被遮擋的輻射能在中紅外線波段重新釋出,中紅外線波段的探測在鑑定屏蔽活耀星系核的工作中顯現出重要性。詹姆斯·韋伯太空望遠鏡(James Webb Space Telescope,JWST)具有高靈敏性,可以比先前的太空望遠鏡發現更多黯淡的目標。在這篇論文中,我們透過光譜能量分布(Spectral energy distribution, SED)研究在JWST早期發布宇宙演化科學調查(CEERS)中的活耀星系核候選目標。我們確定了42個候選目標,其中有30個為混合星系(0.2 ≤ f_{AGN,IR} < 0.5);12個為活耀星系核(f_{AGN,IR} ≥ 0.5)。我們報告活耀星系核貢獻與活耀星系核數量比值分別與紅移與總紅外線光度的函數之間的關係,由於樣本數量不足,與先前研究報告的上升趨勢結果相比並不明顯。我們也將先前用極亮紅外星系(ULIRGs, L_{TIR} ≥ 10^12L_{⊙})做出的結果延伸至更黯淡的星系,凸顯了JWST的力量。

The nature of the interaction between active galactic nuclei (AGNs) and their host galaxies remains an unsolved question. Therefore, conducting an AGN census is valuable to AGN research. Nevertheless, a significant fraction of AGNs are obscured by their environment, which blocks UV and optical emissions due to the dusty torus surrounding the central supermassive black hole (SMBH). To overcome this challenge, mid-infrared (IR) surveys have emerged as a valuable tool for identifying obscured AGNs, as the obscured light is re-emitted in this range. With its high sensitivity, the James Webb Space Telescope (JWST) uncovered more fainter objects than previous telescopes. By applying the SED fitting, this work investigates AGN candidates in JWST Cosmic Evolution Early Release Science (CEERS) fields. We identified 42 candidates, 30 of them are classified as composites (0.2 ≤ f_{AGN,IR} < 0.5), and 12 of them are AGNs (f_{AGN,IR} ≥ 0.5). We report the AGN luminosity contributions and AGN number fractions as a function of redshift and total infrared luminosity, showing that previously reported increasing relations are not apparent in our sample due to the sample size. We also extend the previous results on ultra-luminous infrared galaxies (ULIRGs, L_{TIR} ≥ 10^12L_{⊙}) to less luminous AGNs, highlighting the power of JWST.

Abstract (Chinese) I
Acknowledgements (Chinese) II
Abstract IV
Acknowledgements V
Contents VII
List of Figures IX
List of Tables X

1 Introduction 1

2 Data and analysis 5
2.1 MIR observations in CEERS and merged catalogue with CANDELS-
EGS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5
2.2 CIGALE SED fittings . . . . . . . . . . . . . . . . . . . . . . . . . 7
2.3 Sample selections . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12

3 Results and discussions 14
3.1 The uncertainties of SED fittings . . . . . . . . . . . . . . . . . . . 14
3.2 Source distribution . . . . . . . . . . . . . . . . . . . . . . . . . . . 18
3.3 AGN contribution . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19
3.4 AGN number fraction . . . . . . . . . . . . . . . . . . . . . . . . . . 23
3.5 X-ray-selected AGNs . . . . . . . . . . . . . . . . . . . . . . . . . . 26
3.6 Colour-colour selections . . . . . . . . . . . . . . . . . . . . . . . . 28

4 Summary 32

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