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  1. NTU Theses and Dissertations Repository
  2. 理學院
  3. 天文物理研究所
請用此 Handle URI 來引用此文件: http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/43858
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dc.contributor.advisor吳俊輝(Jiun-Huei Proty Wu)
dc.contributor.authorYu-Wei Liaoen
dc.contributor.author廖祐葳zh_TW
dc.date.accessioned2021-06-15T02:30:46Z-
dc.date.available2009-12-31
dc.date.copyright2009-08-19
dc.date.issued2009
dc.date.submitted2009-08-14
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dc.identifier.urihttp://tdr.lib.ntu.edu.tw/jspui/handle/123456789/43858-
dc.description.abstract在這篇論文當中, 我們研究兩種重要的宇宙微波背景輻射次級效應: 桑-濟效應與宇宙拓樸。在論文的第一部份, 我們利用李遠哲陣列所觀測到六個星系團造成的桑-濟效應, 推測這些星系團的電子溫度、質量、以及康普敦散射係數等物理性質。我們同時考慮了兩種星系團模型: 熱平衡貝它模型與普遍溫度模式貝它模型。我們對於星系團物理性質的推估,與其它研究團隊使用桑-濟效應與X 射線觀測資料所得結果相吻合。我們的結果顯示出只靠桑-濟效應的微波關測結果估計星系團性質是可能的。在第二部份, 我們模擬在六種可能的平坦有限宇宙拓樸當中, 宇宙微波背景輻射溫度與極化性的功率譜。我們將模擬所得之功率譜與威爾金森微波非均向性探測衛星的實際觀測結果做比較。我們的結果顯示威爾金森微波非均向性探測衛星的觀測結果有利於有限大小的宇宙拓樸模型。我們估計宇宙的大小大約是最後散射面半徑的1.14倍。同時我們也對於普朗克衛星觀測結果所可能對於宇宙拓樸估計做出的貢獻進行預測。zh_TW
dc.description.abstractIn this thesis we studied two important cosmic microwave background (CMB) secondary effects: Sunyaev-Zel’dovich effect (SZE) and cosmological topology. In the first part, we estimated electron temperature, mass, and integrated Compton Y of six galaxy clusters using SZE observation data obtained with the Y. T. Lee Array for Microwave Background Anisotropy (AMiBA). We modified an iterative method, based on isothermal beta-models, to derive these cluster properties. The non-isothermal universal temperature profile (UTP) beta-model was also considered. Our results are in good agreement with previous results deduced from other X-ray and SZE observations. Our results suggest that cluster properties may be measurable with SZE
observations alone. In the second part, we simulated CMB temperature and polarization power spectrum in universes with six compact and orientable non-trivial topologies with flat geometry. We also compared our simulated power spectrum with observation results from Wilkinson Microwave Anisotropy Probe (WMAP) to estimate the size of 3-torus topology. Our results suggest that the power spectrum
observed by WMAP favors the finite universe model with the size 1.14 times of the radius of last scattering surface. We also conducted a forecast of the ability of
upcoming PLANCK to constrain the topology of our Universe.
en
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Previous issue date: 2009
en
dc.description.tableofcontentsAcknowlegements i
摘要ii
Abstract iii
List of Tables vii
List of Figures viii
I Derivation of Galaxy Cluster Properties using AMiBA
SZE Observation 1
1 Introduction 2
1.1 Sunyaev-Zel’dovich Effect . . . . . . . . . . . . . . . . . . . . . . . . 2
1.2 Galaxy Cluster Properties . . . . . . . . . . . . . . . . . . . . . . . . 3
1.3 AMiBA Observation . . . . . . . . . . . . . . . . . . . . . . . . . . . 4
1.4 Contribution and Outline . . . . . . . . . . . . . . . . . . . . . . . . 5
2 Determination of Cluster Properties 7
2.1 AMiBA: Observation and Data Analysis . . . . . . . . . . . . . . . . 7
2.2 Isothermal -model . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9
2.3 Universal Temperature Profile -model . . . . . . . . . . . . . . . . . 12
2.4 Calculation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14
2.5 Comparing Between SZE and X-ray Derived Properties . . . . . . . . 17
3 Embedded Scaling Relations 30
3.1 Analytical formalism and Numerical analysis . . . . . . . . . . . . . . 30
3.2 Calculation of Scaling Relations . . . . . . . . . . . . . . . . . . . . . 34
4 Discussions, Conclusion, and Prospects 39
II Estimation of The Size of The Universe with a Finite
Flat Manifold Using WMAP Observation 42
5 Introduction 43
5.1 Cosmic Topology . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 43
5.2 CMB Power Spectrum . . . . . . . . . . . . . . . . . . . . . . . . . . 44
5.3 WMAP . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 46
5.4 Contribution and Outline . . . . . . . . . . . . . . . . . . . . . . . . 46
6 Calculation of CMB Power Spectrum in a Finite Universe 48
6.1 Acceptable Fourier Modes in Flat Compact Topologies . . . . . . . . 48
6.1.1 3-torus manifold . . . . . . . . . . . . . . . . . . . . . . . . . 48
6.1.2 Half turn torus . . . . . . . . . . . . . . . . . . . . . . . . . . 49
6.1.3 Quarter turn torus . . . . . . . . . . . . . . . . . . . . . . . . 50
6.1.4 Third turn torus . . . . . . . . . . . . . . . . . . . . . . . . . 50
6.1.5 Sixth turn torus . . . . . . . . . . . . . . . . . . . . . . . . . . 52
6.1.6 Hantzsche-Wendt manifold . . . . . . . . . . . . . . . . . . . . 52
6.2 CMB Power spectrum in non-trivial topology . . . . . . . . . . . . . 54
6.3 Modification of CMBFAST . . . . . . . . . . . . . . . . . . . . . . . . 58
7 Estimating Universe Size with CMB Observations 70
7.1 An Brief Introduction to Markov Chain Monte Carlo Method . . . . . 71
7.2 Markov chain Monte Carlo to Estimate the Cosmological Parameters 72
7.3 Forecast of PLANCK Capability to Determine the Cosmic Topology 77
8 Discussion, Conclusion, and Future Work 90
A Relativistic correction of Sunyaev-Zel’dovich effect 94
Bibliography 96
dc.language.isoen
dc.title以宇宙微波背景輻射觀測結果估計星系團性質與宇宙拓樸zh_TW
dc.titleEstimation of Galaxy Cluster Properties and Cosmic Topology Using Cosmic Microwave Background Observationsen
dc.typeThesis
dc.date.schoolyear97-2
dc.description.degree博士
dc.contributor.oralexamcommittee闕志鴻(Tzihong Chiueh),張祥光(Hsiang-Kuang Chang),黃崇源(Chorng-Yuan Hwang),劉國清(Guo-Chin Liu)
dc.subject.keyword宇宙微波背景輻射,桑濟效應,宇宙拓樸,星系團,zh_TW
dc.subject.keywordCosmic Microwave Background,Galaxy Cluster,Cosmic Topology,en
dc.relation.page101
dc.rights.note有償授權
dc.date.accepted2009-08-17
dc.contributor.author-college理學院zh_TW
dc.contributor.author-dept天文物理研究所zh_TW
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