請用此 Handle URI 來引用此文件:
http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/43858
完整後設資料紀錄
DC 欄位 | 值 | 語言 |
---|---|---|
dc.contributor.advisor | 吳俊輝(Jiun-Huei Proty Wu) | |
dc.contributor.author | Yu-Wei Liao | en |
dc.contributor.author | 廖祐葳 | zh_TW |
dc.date.accessioned | 2021-06-15T02:30:46Z | - |
dc.date.available | 2009-12-31 | |
dc.date.copyright | 2009-08-19 | |
dc.date.issued | 2009 | |
dc.date.submitted | 2009-08-14 | |
dc.identifier.citation | Allen, S. W. 2000, MNRAS, 315, 269, arXiv:astro-ph/0002506
Allen, S. W., Ettori, S., & Fabian, A. C. 2001, MNRAS, 324, 877, arXiv:astroph/ 0008517 Anders, E., & Grevesse, N. 1989, Geochim. Cosmochim. Acta, 53, 197 Aurich, R., Lustig, S., & Steiner, F. 2006, MON.NOT.ROY.ASTRON.SOC., 369, 240 Aurich, R., Lustig, S., & Steiner, F. 2009, Hot pixel contamination in the CMB correlation function Barker, R. et al. 2006, MNRAS, 369, L1, arXiv:astro-ph/0509215 Benson, B. A., Church, S. E., Ade, P. A. R., Bock, J. J., Ganga, K. M., Henson, C. N., & Thompson, K. L. 2004, ApJ, 617, 829 Birkinshaw, M. 1999, Phys. Rep., 310, 97, arXiv:astro-ph/9808050 Bonamente, M., Joy, M., LaRoque, S. J., Carlstrom, J. E., Nagai, D., & Marrone, D. P. 2008, ApJ, 675, 106 Bonamente, M., Joy, M. K., LaRoque, S. J., Carlstrom, J. E., Reese, E. D., & Dawson, K. S. 2006, ApJ, 647, 25, arXiv:astro-ph/0512349 Cavaliere, A., & Fusco-Femiano, R. 1976, A & A, 49, 137 ——. 1978, A & A, 70, 677 Challinor, A. D., & Lasenby, A. N. 1998, ApJ, 499, 1 96 Chen, M.-T. et al. 2009, The Astrophysical Journal, 694, 1664 Cornish, N. J., Spergel, D. N., & Starkman, G. D. 1998, Classical and Quantum Gravity, 15, 2657 Cornish, N. J., Spergel, D. N., Starkman, G. D., & Komatsu, E. 2004, Phys, Rev. Lett., 92, 201302 Dunkley, J. et al. 2009, ApJS, 180, 306 Efstathiou, G. 2005, MON.NOT.ROY.ASTRON.SOC., 356, 1549 Fowler, J. W. 2004, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 5498, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, ed. C. M. Bradford, P. A. R. Ade, J. E. Aguirre, J. J. Bock, M. Dragovan, L. Duband, L. Earle, J. Glenn, H. Matsuhara, B. J. Naylor, H. T. Nguyen, M. Yun, & J. Zmuidzinas, 1 Gelman, A. 1996, in Markov Chain Monte Carlo in Practice (Chapman & Hall), 131 Gilks, W. R., Richardson, S., & Spiegelhalter, D. J. 1996, in Markov Chain Monte Carlo in Practice (Chapman & Hall), 1 Grego, L., Carlstrom, J. E., Reese, E. D., Holder, G. P., Holzapfel, W. L., Joy, M. K., Mohr, J. J., & Patel, S. 2001, ApJ, 552, 2 Hallman, E. J., Burns, J. O., Motl, P. M., & Norman, M. L. 2007, ApJ, 665, 911 Halverson, N. W. et al. 2008, ArXiv e-prints, 0807.4208 Hansen, S. H., Pastor, S., & Semikoz, D. V. 2002, ApJ Letter, 573, L69, arXiv:astroph/ 0205295 Hasting, W. K. 1970, Biometrika, 57, 97 Hincks, A. D. et al. 2009, ArXiv e-prints, 0907.0461 Hinshaw, G., Branday, A. J., Bennett, C. L., Gorski, K. M., Kogut, A., Lineweaver, C. H., Smoot, G. F., & Wright, E. L. 1996, ApJL, 464, L25 Hinshaw, G. et al. 2007, ApJ, 170, 288 Hinshaw, G. et al. 2003, ApJS, 148, 135 Ho, P. T. P. et al. 2009, ApJ, 694, 1610 Huang, C.-W. L. et al. 2009, AMiBA: Scaling Relations Between the Integrated Compton-y and X-Ray Derived Temperature, Mass, and Luminosity Itoh, N., Kohyama, Y., & Nozawa, S. 1998, Apj, 502, 7, arXiv:astro-ph/9712289 Kaiser, N. 1986, MNRAS, 222, 323 Kaneko, T. 2006, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 6267, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Kneissl, R., Jones, M. E., Saunders, R., Eke, V. R., Lasenby, A. N., Grainge, K., & Cotter, G. 2001, MNRAS, 328, 783, arXiv:astro-ph/0103042 Koch, P. M. et al. 2009a, AMiBA 94 GHz SZE Observations: An Initial Measurement of H0 ——. 2009b, ApJ, 694, 1670, 0902.2335 Kompaneets, A. S. 1957, Soviet Phys. JETP, 4, 730 Kosowsky, A. 2003, New Astronomy Review, 47, 939, arXiv:astro-ph/0402234 Lachieze-Rey, M., & Luminet, J. 1995, Phys. Rept., 254, 135 Lancaster, K. et al. 2007, MNRAS, 378, 673, 0705.3336 ——. 2005, MNRAS, 359, 16, arXiv:astro-ph/0405582 LaRoque, S. J., Bonamente, M., Carlstrom, J. E., Joy, M. K., Nagai, D., Reese, E. D., & Dawson, K. S. 2006, ApJ, 652, 917, arXiv:astro-ph/0604039 LaRoque, S. J., Carlstrom, J. E., Reese, E. D., Holder, G. P., Holzapfel, W. L., Joy, M., & Grego, L. 2002, ArXiv Astrophysics e-prints, arXiv:astro-ph/0204134 Lehoucq, R., Weeks, J., Uzan, J.-P., Gausmann, E., & Luminet, J.-P. 2002, Class. Quant. Grav., 19, 4683 Levin, J. 2002, Phys. Rept., 365, 251 Levin, J., Scannapieco, E., & Silk, J. 1998, Phys. Rev. D, 58, 103516 Liao, Y.-W. et al. 2009, AMiBA: Sunyaev-Zel’dovich Effect Derived Properties and Scaling Relations of Massive Galaxy Clusters Lifshitz, E. M. 1946, J. Phys. USSR, 10, 16 Lin, K.-Y. et al. 2009, ApJ, 694, 1629 Liu, G.-C. et al. 2009, Contamination of Sunyaev-Zel’dovich Clusters in AMiBA Observations Metropolis, N., Rosenbluth, A. W., Rosenbluth, M. N., Teller, A. H., & Teller, E. 1953, J. Chem. Phys., 21, 1087 Mohr, J. J., Mathiesen, B., & Evrard, A. E. 1999, Astrophysics Journal, 517, 627, arXiv:astro-ph/9901281 Molnar, S. M. et al. 2009, CONSTRAINING INTRA-CLUSTER GAS MODELS WITH AMIBA13 Morandi, A., Ettori, S., & Moscardini, L. 2007, MNRAS, 379, 518 Muchovej, S. et al. 2007, Astrophysics Journal, 663, 708, arXiv:astro-ph/0610115 Navarro, J. F., Frenk, C. S., & White, S. D. M. 1997, Astrophysics Journal, 490, 493, arXiv:astro-ph/9611107 Nishioka, H. et al. 2009, ApJ, 694, 1637 Nolta, M. R. et al. 2009, ApJ, 180, 296 Nord, M. et al. 2009, ArXiv e-prints, 0902.2131 O’Dwyer, I. J. et al. 2004, ApJ, 617, L99 Page, L. et al. 2007, ApJ, 170, 335 Peebles, P. J. E., & Yu, J. T. 1970, ApJ, 162, 815 Phillips, N. G., & Kogut, A. 2006, ApJ, 645, 820 Press, W. H., Teukolsky, S. A., Vetterling, W. T., & Flannery, B. P. 1992, ”Numerical Recipes in C. The Art of Scientific Computing”’, 2nd edn. (Cambridge University Press) Reese, E. D., Carlstrom, J. E., Joy, M., Mohr, J. J., Grego, L., & Holzapfel, W. L. 2002, ApJ, 581, 53, arXiv:astro-ph/0205350 Riazuelo, A., Caillerie, S., Lachi`eze-Rey, M., Lehoucq, R., & Luminet, J.-P. 2006, arXiv:astro-ph/0601433 Riazuelo, A., Weeks, J., Uzan, J.-P., Lehoucq, R., & Luminet, J.-P. 2004, Phys. Rev. D, 69, 103518 Robert, G. O. 1996, in Markov Chain Monte Carlo in Practice (Chapman & Hall), 45 Ruhl, J. et al. 2004, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 5498, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, ed. C. M. Bradford, P. A. R. Ade, J. E. Aguirre, J. J. Bock, M. Dragovan, L. Duband, L. Earle, J. Glenn, H. Matsuhara, B. J. Naylor, H. T. Nguyen, M. Yun, & J. Zmuidzinas, 11 Sanderson, A. J. R., & Ponman, T. J. 2003, MNRAS, 345, 1241, arXiv:astroph/ 0307457 Sazonov, S. Y., & Sunyaev, R. A. 1998, Apj, 508, 1 Scannapieco, E., Levin, J., & Silk, J. 1999, MNRAS, 303, 797, arXiv:astroph/ 9811226 Seljak, U., & Zaldarriaga, M. 1996, ApJ, 469, 437 Slosar, A., Seljak, U., & Makarov, A. 2004, Phys. Rev. D, 69, 123003 Spergel, D. N. et al. 2007, ApJ, 170, 377 Staniszewski, Z. et al. 2008, ArXiv e-prints, 0810.1578 Sunyaev, R. A., & Zeldovich, Y. B. 1972, Comments on Astrophysics and Space Physics, 4, 173 The Planck Collaboration. 2006, ArXiv Astrophysics e-prints, arXiv:astroph/ 0604069 Umetsu, K. et al. 2009, ApJ, 694, 1643, 0810.0969 Weeks, J., Luminet, J.-P., Riazuelo, A., & Lehoucq, R. 2004, MON.NOT.ROY.ASTRON.SOC., 352, 258 Wu, J.-H. P. et al. 2009, ApJ, 694, 1619 Zaldarriaga, M., & Seljak, U. 1997, Phys. Rev. D, 55, 1830 Zwart, J. T. L. et al. 2008, MNRAS, 391, 1545, 0807.2469 | |
dc.identifier.uri | http://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.abstract | In 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 |
dc.description.provenance | Made available in DSpace on 2021-06-15T02:30:46Z (GMT). No. of bitstreams: 1 ntu-98-D93244001-1.pdf: 3269421 bytes, checksum: 52159aa14d29af0a215170b341546b56 (MD5) Previous issue date: 2009 | en |
dc.description.tableofcontents | Acknowlegements 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.iso | en | |
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.title | Estimation of Galaxy Cluster Properties and Cosmic Topology Using Cosmic Microwave Background Observations | en |
dc.type | Thesis | |
dc.date.schoolyear | 97-2 | |
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.keyword | Cosmic Microwave Background,Galaxy Cluster,Cosmic Topology, | en |
dc.relation.page | 101 | |
dc.rights.note | 有償授權 | |
dc.date.accepted | 2009-08-17 | |
dc.contributor.author-college | 理學院 | zh_TW |
dc.contributor.author-dept | 天文物理研究所 | zh_TW |
顯示於系所單位: | 天文物理研究所 |
文件中的檔案:
檔案 | 大小 | 格式 | |
---|---|---|---|
ntu-98-1.pdf 目前未授權公開取用 | 3.19 MB | Adobe PDF |
系統中的文件,除了特別指名其著作權條款之外,均受到著作權保護,並且保留所有的權利。