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完整後設資料紀錄
DC 欄位 | 值 | 語言 |
---|---|---|
dc.contributor.advisor | 王名儒 | |
dc.contributor.author | Yeng-Ming Tzeng | en |
dc.contributor.author | 曾衍銘 | zh_TW |
dc.date.accessioned | 2021-06-13T03:29:01Z | - |
dc.date.available | 2006-08-31 | |
dc.date.copyright | 2006-07-31 | |
dc.date.issued | 2006 | |
dc.date.submitted | 2006-07-27 | |
dc.identifier.citation | [1] Neutrino Physics, Kai Zuber.
[2] Michael Disney Sci, Am. 26-31 (1998). [3] Gerald J.Fishman and Dieter H.Hartmann Sci. Am. 34-39 (1997). [4] Current Aspects of Neutrino Physics, David O. Caldwell. [5] Igor Sokalski [arXiv:hep-ex/0501004]. [6] F. Vannucci, NATO Advanced Research Workshop, Oujda, Marocco, (2000), hepph/0106061 [7] Z.Cao, M.A. Huang, P.Sokolsky and Y. Hu [arXiv:astro-ph/0501004] [8] S. Eidelman et al., Phys. Lett. 592, 1 (2004) [9] Estimation the Sensitivity of the Neutrino Telescope, Shiang-Rund Tsai, (2005). [10] Y.S. Velikzhanin et al., Design of a General Purpose Data Collection Module for the NuTel Telescope, Nuclear Instruments and Methods in Physics Research, A(552):477-488,2005. [11] Rudolf K. Bock, 9 April (1998). | |
dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/32038 | - |
dc.description.abstract | Neutrinos could play an important role in connecting several branches of particle astrophysics. Bottom-up theories propose that they may come from astronomical sources like Active Galactic Nuclei (AGN), Gamma Ray Burst (GRB), or Galactic Center (GC)etc. On the other hand, top-down theories like to suggest that ultra high energy cosmic rays (UHECR) are decay products of topological defects or heavy relic particles. However the goal of NuTel (neutrino telescope) is building a Cherenkov telescope to be installed on a mountain site for observing near horizontal air showers emerging from another mountain. The ultra-high-energy cosmic tau neutrinos is the primary source of such showers. The energy domain of NuTel for tau neutrinos spans from 1 PeV to 1EeV.
The rate of the expected neutrino signals is very low (0.5~1 events per year). The main background is the night sky background with a much higher flux (~2000 /m2/sr/ns). It is crucial that an e±cient trigger system is put in place to reduce the backgrounds to a reasonable level. This work is on the study of the triggering scheme of NuTel. The triggering scheme is loaded into Field Programmable Gate Arrays (FPGA) on the on line electronic boards for fast response and flexibility of algorithm change. It can be shown in simulations that the trigger schemes found in this study can effectively reduce the background rate while maximizing the acceptance (A(E=1PeV)=2.6 km2sr) to cosmic neutrinos of interest. | en |
dc.description.provenance | Made available in DSpace on 2021-06-13T03:29:01Z (GMT). No. of bitstreams: 1 ntu-95-R93222008-1.pdf: 2292722 bytes, checksum: a07f9c6be68d91adbe20f561100a07a1 (MD5) Previous issue date: 2006 | en |
dc.description.tableofcontents | 1 Introduction 1
1.1 Neutrino Physics . . . . . . . . . . . . . . . . . . . . . . . . . 1 1.2 Neutrino Telescope-Earth-Skimming Technique . . . . . . . . 2 1.3 Method . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3 2 Hardware 5 3 The FPGA Code of Trigger 9 3.1 DCM . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9 3.1.1 DCM Statement . . . . . . . . . . . . . . . . . . . . . 10 3.1.2 Introduction to FPGA . . . . . . . . . . . . . . . . . . 11 3.2 Trigger FPGA . . . . . . . . . . . . . . . . . . . . . . . . . . . 13 3.2.1 One cell logic . . . . . . . . . . . . . . . . . . . . . . . 14 3.2.2 Trigger request . . . . . . . . . . . . . . . . . . . . . . 15 3.2.3 Trigger decision . . . . . . . . . . . . . . . . . . . . . . 15 3.2.4 Trigger settings . . . . . . . . . . . . . . . . . . . . . . 23 3.2.5 Synchro slave/single/masterA/masterB . . . . . . . . . 25 4 Trigger Decision 27 4.1 Sample : background and signal . . . . . . . . . . . . . . . . . 29 4.1.1 Background . . . . . . . . . . . . . . . . . . . . . . . . 29 4.1.2 signal : Pion shower . . . . . . . . . . . . . . . . . . . 29 4.2 Trigger Schemes . . . . . . . . . . . . . . . . . . . . . . . . . . 31 4.2.1 Two Kinds of Thresholds . . . . . . . . . . . . . . . . . 31 4.2.2 Three kinds of Trigger Schemes . . . . . . . . . . . . . 33 4.3 VH trigger options . . . . . . . . . . . . . . . . . . . . . . . . 34 4.3.1 Equivalent photoelectron after preamplifier . . . . . . . 34 4.3.2 Simulation of trigger rate reduction logic for Single telescope . . . . . . . . . . . . . . . . . . . . . . . . . . 35 4.3.3 Single and two telescopes (timing coincidence) for VHtrigger . . . . . . . . . . . . . . . . . . . . . . . . . . . 37 4.3.4 Double clocks . . . . . . . . . . . . . . . . . . . . . . . 39 4.3.5 Double triggers . . . . . . . . . . . . . . . . . . . . . . 42 4.3.6 Summary . . . . . . . . . . . . . . . . . . . . . . . . . 44 4.4 Optimal threshold . . . . . . . . . . . . . . . . . . . . . . . . . 46 4.4.1 Decide the VHL threshold . . . . . . . . . . . . . . . . 47 4.4.2 Find the HL threshold range . . . . . . . . . . . . . . . 48 4.4.3 Decide the cluster threshold with the proper LL threshold 49 4.5 Different particles : Pion, Electron, and Proton . . . . . . . . 57 4.6 Acceptance . . . . . . . . . . . . . . . . . . . . . . . . . . . . 59 5 Conclusion 63 | |
dc.language.iso | en | |
dc.title | 微中子望眼鏡的觸發機制 | zh_TW |
dc.title | Triggering Scheme of the NuTel Experiment | en |
dc.type | Thesis | |
dc.date.schoolyear | 94-2 | |
dc.description.degree | 碩士 | |
dc.contributor.oralexamcommittee | 侯維恕,葉平,張寶棣,上野耕資 | |
dc.subject.keyword | 微中子望眼鏡,觸發機制,觸發, | zh_TW |
dc.subject.keyword | NuTel,neutrino telescope,trigger,trigger scheme,triggering scheme, | en |
dc.relation.page | 65 | |
dc.rights.note | 有償授權 | |
dc.date.accepted | 2006-07-28 | |
dc.contributor.author-college | 理學院 | zh_TW |
dc.contributor.author-dept | 物理研究所 | zh_TW |
顯示於系所單位: | 物理學系 |
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