這份論文的第一部分是關於"利用Subaru/Hyper Suprime-Cam深光學數據計算北黃道極(NEP)區寬場的光學紅移"。

在21世紀初期，AKARI太空紅外線望遠鏡利用其獨特的9波段濾鏡在北黃道極區寬埸(NEPW; 5.4 deg^2)進行了深度的中紅外波段的觀測，這個觀測時間更佔了AKARI整個觀測壽命裡的十分之一。多波段濾鏡的特性是其他有名的紅外線望遠鏡如: NASA的Spitzer和WISE 太空望遠鏡(只有4波段濾鏡)所比不上的。
但是，AKARI NEPW卻欠缺了深度的可見光波段的數據，這連帶影響了光學紅移的計算。

近幾年，我們用8公尺的SUBARU光學望遠鏡的Hyper Suprime-Cam (HSC)相機觀測並得到了5個寬帶波段的濾鏡(g, r, i, z, and Y)，除此之外，我們更把從可見光到次毫米，不同波段的數據合併成一個目錄。利用這個目錄的數據，我們可以利用能量譜分佈的擬合(SED fitting)計算新的光學紅移。

我們總共用了26個不同波段的濾鏡，我們利用2026個0 < z < 5的已知光譜紅移值作比較，分析我們計算的光學紅移準確度。
在z < 1.5，我們達到了σ_{Δ[z/(1+z)]} = 0.053 的權重光學紅移準確度和11.3%的離群值 (離群值的定義是|Δz|/(1 + z_s) > 0.15)。

這份論文的第二部分是關於"利用SHELLQs揭示z~6類星體的宿主星系"。

天文學家總是對最高紅移的類星體（QSO）的宿主星系感興趣；它們為我們提供了一個可以研究與宇宙中最早出現的黑洞中最亮的星爆活動星系核（AGN）相關的物理學的機會。

在此，我們會報告一個圍繞在疊合QSO圖像外的光學擴展結構的量測訊號。我們堆疊了的46張Subaru/HSC高紅移QSO圖像（z_median = 6.13）。這些QSO主要由Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs)識別。我們仔細地從圖像中減去了使用附近恆星所構造的點擴散函數(PSF)。在減去PSF之後，z波段中的擴展結構延伸了超過1.49角秒的半光度半徑（R_e = 9.3kpc）。這個宿主星系可能是一個正在形成的巨大星系，並與一個超大質量黑洞交互作用。這個結果仍是初步的，我們將來會再做更一步的分析。

This thesis is composed of two parts. The first part is "Photometric Redshifts in the North Ecliptic Pole Wide Field based on a Deep Optical Survey with Hyper Suprime-Cam". The AKARI space infrared telescope has performed near- to mid-infrared (MIR) observations on the North Ecliptic Pole Wide (NEPW) field (5.4 deg^2) devoting a large amount of time. AKARI took advantage of its continuous nine photometric bands, compared with NASA's Spitzer and WISE space telescopes, which had only four filters with a wide gap in the MIR.
The AKARI NEPW field lacked deep and homogeneous optical data, limiting the use of nearly half of the IR sources for extra-galactic studies owing to the absence of photometric redshifts (photo-zs).
To remedy this, we have recently obtained deep optical imaging over the NEPW field with 5 bands (g, r, i, z, and Y) of the Hyper Suprime-Camera (HSC) on the Subaru 8m telescope. We optically identify AKARI-IR sources along with supplementary Spitzer and WISE data as well as pre-existing optical data. In this work, we derive new photo-zs using a Χ^2 template-fitting method code (Le Phare) and reliable photometry from 26 selected filters including HSC, AKARI, CFHT, Maidanak, KPNO, Spitzer and WISE data. We take 2026 spectroscopic redshifts (spec-z) from all available spectroscopic surveys over the NEPW to calibrate and assess the accuracy of the photo-zs. At z < 1.5, we achieve a weighted photo-z dispersion of σ_{Δ[z/(1+z)]} = 0.053 with η = 11.3% catastrophic errors.

The second part is "Unveiling quasar host galaxies and their Lyα emission at z$\sim$6 by SHELLQs". Host galaxies of high redshift quasars (QSOs) are of interest; they provide us with a valuable opportunity to investigate the physics relevant to the starburst-active galactic nuclei (AGN) connection at the earliest epoch of the Universe, with the most luminous black holes.
Here we report an optical detection of an extended structure around a stacked QSO image. We have stacked 46 high-z (z_median = 6.13) QSOs images by Subaru/HSC. These QSOs are mainly identified by the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). We have carefully subtracted a PSF constructed using nearby stars from the images. After the PSF (QSO) subtraction, a structure in the z-band extends for more than 4" on the sky (R_e = 11kpc). The host may be a forming giant galaxy, co-evolving with a supermassive black hole. More analysis will be carried out in the future.

Abstract--------------iii
摘要--------------iv
Acknowledgements--------------v
List of Figures--------------viii
List of Tables--------------xi
I. Introduction--------------3
II. Photometric Redshifts of North Ecliptic Pole Wide Field based on Deep Optical Survey using Hyper Suprime-Cam (submitted to MNRAS, 2020)--------------9
1. THE DATASETS--------------11
1.1. Optical Identification of the AKARI Sources--------------11
1.2. Spectroscopic Data--------------12
1.3. Ancillary Near- to Mid-IR Data--------------13
1.4. Data Selection--------------15
2. Photo-z with SED template fitting--------------25
2.1. Comparison of different template models--------------25
2.2. Comparison of different filter combinations--------------27
2.3. Star/Galaxy Classification--------------27
2.4. Best parameters for photo-z accuracy--------------30
3. Photo-z with SED template fitting37
4. Discussion--------------39
4.1. Photo-z of AGNs--------------39
4.2. Feasibility of Machine Learning photo-z--------------40
4.2.1. Galaxy classification in the NEPW field--------------41
4.3. Comparison of photo-z accuracy with other work--------------41
III. Unveiling QSO host galaxies and their Lyα emission at z∼6 by SHELLQs--------------43
1. QSO sample--------------45
1.1. SHELLQs--------------45
1.2. SDSS--------------45
1.3. CFHQS--------------45
1.4. Sample selection--------------47
2. Method492.1. QSO stacking--------------49
2.2. Point Spread Function (PSF)--------------49
3. Result513.1. PSF subtraction--------------51
3.1.1. Sérsic fit--------------51
IV. Conclusion55V. APPENDIX711. Summary of source detection and photometry from different sources--------------73
2. Summary of definitions of depths for different catalogs753. Response to the panelists’ questions--------------77
3.1. The outlier fraction of the photo-z is 11.3% at z < 1.5. This sounds quite bad. Could you comment on this?--------------77
3.2. Why the photo-z computed by RF was quantized?--------------77
3.3. You did not use AGN templates for the computation of photo-z. Is this catalog still available for AGN research?--------------79
3.4. How robust can you say that this is a host galaxy, not e.g., outflows--------------79

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