高能天文現象可以被用來研究宇宙學以及搜尋地外文明，在此研究中，我們探討
了三個主題：一、六個伽瑪射線爆之宿主星系的遠紅外恆星形成率透過阿塔卡瑪大
型毫米及次毫米波陣列；二、黑洞外的戴森球；三、透過河外星系的電波噴流之自
行限縮哈伯常數和它的最小值。
伽瑪射線爆（Gamma-Ray Bursts; GRBs），可以被用來追蹤宇宙恆星形成歷史的
足跡，在此研究中，我們研究了ALMA遠紅外波段觀測六個GRB宿主星系，我們
使用光譜能量分布擬合 （Spectral energy distribution fitting）來研究宿主星系的物理量。我們的最佳擬合結果指出恆星質量多與以前的文獻研究中相符，而恆星形成率都與以前的文獻研究不一致。我們的研究顯示，為了正確的估計恆星形成率，透過
恆星形成加熱的冷塵埃的熱輻射，遠紅外觀測的重要性。
戴森球（Dyson Spheres），一種包圍恆星的球形結構，用來轉換恆星的輻射能量
用以維持先進文明的發展，是搜尋地外文明（Search for Extra-Terrestrial Intelligence;SETI）的主要目標之一，在此研究中，我們探討了建立一個戴森球在一個黑洞周圍是否為有效率的。最多的能量來自於吸積盤，達到105 L⊙，足夠去維持一個二型文明(1 L⊙)的發展。考慮戴森球輻射的廢棄熱，我們的研究顯示一個在銀河系中（距離我們10 kpc）圍繞著恆星級黑洞的戴森球，是能利用我們現有的望遠鏡和計畫如星系演化探測器紫外光搜索在 紫外光至中紅外(10nm − 40 𝜇m)的波段所偵測到。使
用SED fitting以及測量逕向速度的變化都能幫助我們確認可能的人造結構。
在此研究中，我們提出了一個不需模型也不需距離階梯的方法來限縮哈伯常數
（描繪宇宙現在的膨脹速率;𝐻0），由弗里德曼-勒梅特-羅伯遜-沃爾克度規和河外
星系噴流之自行的幾何關係可以導出哈伯常數的最小值（𝐻0,min）只需要三個變數
就能決定：宿主星系之紅移值、遠離和接近的自行角速度。我們提出利用科摩哥洛
夫-史密諾夫檢定(Kolmogorov-Smirnov test; K-S test)來檢定觀測和理論中的𝐻0,min分布是否吻合。我們的結果顯示在10%和5%的觀測誤差中，增加噴流之數量可以
讓𝐻0和冪律指數限縮至更小的誤差範圍。若減小觀測誤差可以讓𝐻0限縮至更小的
誤差範圍，並且可以讓𝐻0和譜指數的退化程度變好。

High energy phenomenon can be leveraged to study cosmology and the Search for Extra-Terrestrial Intelligence (SETI). We studied three perspectives in this thesis: (i) Far-infrared star-formation rates of six GRB host galaxies with ALMA, (ii) A Dyson Sphere around a black hole, and (iii) Constraining the Hubble constant and its lower limit from the proper motion of extragalactic radio jets.
Gamma-Ray Bursts (GRBs) can be a promising tracer of cosmic star-formation rate history (CSFRH). In order to reveal the CSFRH using GRBs, it is important to understand whether they are biased tracers. In this work, we report ALMA far-infrared (FIR) observations of six 𝑧 ∼ 2 IR-bright GRB host galaxies.Spectral energy distribution (SED) fitting analyses were performed to investigate physical properties of host galaxies. While derived stellar masses of three host galaxies are mostly consistent with those in previous studies, interestingly the value of star-formation rates (SFRs) of all six GRB hosts are inconsistent with previous studies. Our results indicate the importance of rest-frame FIR observations to correctly estimate SFRs by covering thermal emission from cold dust heated by star formation. A Dyson Sphere, a spherical structure that surrounds a star and transports its radiative energy outward as an energy source for an advanced civilisation, is one of the main targets
of SETI. In this study, we discuss whether building a Dyson Sphere around a black hole is effective. The largest luminosity can be collected from an accretion disk, reaching 10^5 L⊙, enough to maintain a Type II civilisation4 × 10^26 W(1 L⊙). Considering the emission from a Dyson Sphere, our results show that the Dyson Sphere around a stellar-mass black hole in the Milky Way (10 kpc away from us) is detectable in the ultraviolet to mid-infrared(10nm − 40 𝜇m) wavelengths via the waste heat radiation using current telescopes such as Galaxy Evolution Explorer Ultraviolet Sky Surveys. Performing model fitting to
observed spectral energy distributions and measuring the variability of radial velocity may help us to identify these possible artificial structures.
We propose a model-free and distance-free method to constrain 𝐻0, a measurement to describe the expansion rate of the Universe in the current era. Combining Friedman-Lemaître-Robertson-Walker cosmology with geometrical relation of the proper motion of extragalactic jets, the lower limit (𝐻0,min) of 𝐻0 can be determined using only three cosmology-free observables: the redshifts of the host galaxies, as well as the approaching and receding angular velocities of radio jets. We perform K-S tests between the simulated samples as theoretical distributions with different 𝐻0 and spectral index of velocity distribution
of jets and mock observational data. Our result suggests increasing sample sizes leads to tighter constraints on both spectral index and the Hubble constant at moderate accuracy (i.e., 10% and 5%) while at 1% accuracy, increasing sample sizes leads to tighter constraints on spectral index more. Improving accuracy results in better constraints in the Hubble constant compared with the spectral index in all cases but it also alleviates the degeneracy.

Abstract . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . iii
摘要 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . iv
Acknowledgements . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . v
List of Figures . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . viii
List of Tables . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . xi
I. Far-infrared star-formation rates of six GRB host galaxies with
ALMA 3
1. Introduction 5
2. Sample 9
2.1. GRB080207 host . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9
2.2. GRB060814 host . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 10
2.3. GRB070306 host . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 10
2.4. GRB081221 host . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11
2.5. GRB071021 host . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12
2.6. GRB050915A host . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12
3. Data 13
4. SED Modelling and results 21
5. Discussion 27
5.1. Group A (Radio detected hosts) . . . . . . . . . . . . . . . . . . . . . . . 27
5.1.1. GRB080207 host galaxy . . . . . . . . . . . . . . . . . . . . . . . 27
5.1.2. GRB060814 host galaxy . . . . . . . . . . . . . . . . . . . . . . . 29
5.1.3. GRB070306 host galaxy . . . . . . . . . . . . . . . . . . . . . . . 30
5.2. Group B (Radio non-detected hosts) . . . . . . . . . . . . . . . . . . . . . 30
5.2.1. GRB081221 host galaxy . . . . . . . . . . . . . . . . . . . . . . . 30
5.2.2. GRB071021 host galaxy . . . . . . . . . . . . . . . . . . . . . . . 31
5.2.3. GRB050915A host galaxy . . . . . . . . . . . . . . . . . . . . . . 31
6. Summary of the part 37
II. A Dyson Sphere around a black hole 39
1. Introduction 41
2. Energy source 45
2.1. Cosmic Microwave Background . . . . . . . . . . . . . . . . . . . . . . . 45
2.2. Hawking radiation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 46
2.3. Accretion disk . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 47
2.4. Bondi Accretion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 48
2.5. Corona . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 50
2.6. Relativistic jets . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 51
3. Dyson Sphere 53
3.1. Possible Type and Location . . . . . . . . . . . . . . . . . . . . . . . . . . 53
3.2. Efficiency . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 55
3.3. Detectablility . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 56
4. Summary of the part 65
III. Constraining the Hubble constant and its lower limit from the
proper motion of extragalactic radio jets 67
1. Introduction 69
2. Methodology 71
3. Results and Discussion 75
4. Summary of the part 83
IV. Conclusion 85
V. APPENDIX 113

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