請用此 Handle URI 來引用此文件：
http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/48262完整後設資料紀錄
| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 王名儒,上野耕資 | |
| dc.contributor.author | Jun-Lin Li | en |
| dc.contributor.author | 李俊霖 | zh_TW |
| dc.date.accessioned | 2021-06-15T06:50:34Z | - |
| dc.date.available | 2011-02-25 | |
| dc.date.copyright | 2011-02-25 | |
| dc.date.issued | 2011 | |
| dc.date.submitted | 2011-02-16 | |
| dc.identifier.citation | [1] Neutrino Physics, Chapter 12, Kai Zuber, 2004.
[2] T.K. Gaisser and T. Stanev revised, Physics Letters B, Vol 592, 233, (2004) [3] D.B. Cline and F.W. Stecker [arXiv:astro-ph/0003459] [4] Teng-Chieh Kang, Optical System of Neutrino Telescope, p37, Figure 3.4 (2006) [5] [6] [7] [8] http://sales.hamamatsu.com/assets/pdf/parts_H/H8500C_ H8500D _TPMH1308E01.pdf [9] [11] Yuri Velikzhanin, URL (http://hep1.phya.ntu.edu.tw/DCM/) [10] Kun-Xian Huang , Front-End Readout System of Neutrino Telescope, p23, Figure 2.18 (2007) [12] [13] Schott BG3 Glass Filter Data URL (http://www.optical-filters .com/bg3.html) [14] GoogleEarth, URL(http://www.google.com/earth/index.html) | |
| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/48262 | - |
| dc.description.abstract | 在天文物理中，微中子因為其和宇宙間的物質交互作用很不容易發生，所以能提供很多宇宙間的訊息。例如，我們可以藉由偵測微中子而對超高能宇宙射線或是早期宇宙演化得到更深入的了解。這兩者都是相當有名的議題。
NuTel設計為觀察τ微中子所激起air showers所產生的Cherenkov 光的望遠鏡。我們感興趣的部份是10^15~10^18 ev (電子伏特) 之間的能量範圍。望遠鏡的尺寸是約二公尺。採用的是Earth-Skimming 法，而倘若Cherenkov光可以由山後被偵測到，νμ → ντ震盪就可以被證實。台大梅峰農場是我們國內的第一個觀測點。首次的野外實測在2009年夏天完成。 首次的野外測試測量夜間天空背景量。我們使用四個多陽極光電管對準山和夜空來證明系統運作。光通亮可以因此被估算出來。 | zh_TW |
| dc.description.abstract | In astrophysics, neutrinos provide important information from cosmos due to its interaction among matters along its passage in the universe can hardly occur. We can know more about the origins of UHECR and the early cosmos evolution via neutrino detectors.
NuTel is a telescope designed to observe the Cherenkov light from air showers aroused by τ neutrinos. We are interested in the energy range between 1015~1018ev since this energy range is not covered by the conventional neutrino detectors or UHECR detectors. The size of NuTel is about 2 meter in diameter. Earth-skimming Method is used and if the Chrenkov light can be detected from behind a mountain, the oscillation of νμ → ντ can be proved. Mei-Fong farm of National Taiwan University is our first domestic site. The first field test took place in the summer of 2009. We measured the night sky background in this field test. We used four MAPMTs and choose moonless nights to determine the incident photon flux behind the mountain. | en |
| dc.description.provenance | Made available in DSpace on 2021-06-15T06:50:34Z (GMT). No. of bitstreams: 1 ntu-100-R94244009-1.pdf: 14140001 bytes, checksum: bcf1ab2ff3afa571d6397f94f9030274 (MD5) Previous issue date: 2011 | en |
| dc.description.tableofcontents | Content
1 Introduction 1.1 Physics................................1 1.2 Principle of Telescope Design..........3 2 Apparatus 2.1 Optics.................................4 2.2 Electronics............................7 2.2.1 MAPMT................................7 2.2.2 Pre-amp..............................9 2.2.3 DAQ.................................10 2.2.4 Off-line analysis...................13 3 Second Telescope 3.1 Telescope Pair........................14 3.2 Design & Manufacture..................16 3.3 Parameter Changed.....................22 4 Calibration 4.1 Linear Guide with Laser...............25 4.2 BG3 filter............................32 4.3 ND filter.............................38 5 Modification 5.1 Light Collector.......................39 5.1.1 Honeycomb...........................39 5.1.2 Outer Shell.........................40 5.1.3 Coating.............................41 5.2 2x2-MAPMT Case........................43 5.3 Cover.................................46 6 Field Test 6.1 Candidate Site........................49 Lulin lodge & Lulin Hut...................49 Kwan Young................................52 Mei Fong farm.............................54 Gwan Shan.................................56 6.2 Plan of Transfer......................60 6.2.1 Transportation (Mirror Box).........62 6.2.2 Lens Box............................67 6.3 Observatory Construction..............67 6.3.1 Site Building.......................67 6.3.2 Telescope Assembling................74 6.3.3 Mechanical Calibration in Optics....78 6.3.4 Electronics Setup...................85 7 Calculation.............................93 Reference................................ 97 | |
| dc.language.iso | en | |
| dc.subject | 契倫可夫光 | zh_TW |
| dc.subject | 微中子 | zh_TW |
| dc.subject | 天文物理 | zh_TW |
| dc.subject | 夜間天空背景量 | zh_TW |
| dc.subject | Astrophysics | en |
| dc.subject | cherenkov light | en |
| dc.subject | nightsky background | en |
| dc.subject | Neutrinos | en |
| dc.title | 微中子望遠鏡整合與夜間天空背景量測量 | zh_TW |
| dc.title | Integration of Neutrino Telescope and Night Sky Background Measurement | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 99-1 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 熊怡 | |
| dc.subject.keyword | 微中子,天文物理,夜間天空背景量,契倫可夫光, | zh_TW |
| dc.subject.keyword | Neutrinos,Astrophysics,nightsky background,cherenkov light, | en |
| dc.relation.page | 97 | |
| dc.rights.note | 有償授權 | |
| dc.date.accepted | 2011-02-16 | |
| 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 | |
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