本資料は、掲載誌(URI)等のリンク先にある学位授与機関のWebサイトやCiNii Dissertationsから、本文を自由に閲覧できる場合があります。
博士論文
国立国会図書館館内限定公開
収録元データベースで確認する
国立国会図書館デジタルコレクション
デジタルデータあり
公開元のウェブサイトで確認する
DOI[10.24561/00019581]のデータに遷移します
Study of the shell-type astronomical object HESSJ1912+101 with the MAGIC telescopes
- 国立国会図書館永続的識別子
- info:ndljp/pid/12313434
国立国会図書館での利用に関する注記
資料に関する注記
一般注記:
- type:textCosmic rays (CRs) were discovered by Victor Hess in 1912, however the origin is not fully understood yet. CRs mainly consists of protons, and...
書店で探す
障害者向け資料で読む
全国の図書館の所蔵
国立国会図書館以外の全国の図書館の所蔵状況を表示します。
所蔵のある図書館から取寄せることが可能かなど、資料の利用方法は、ご自身が利用されるお近くの図書館へご相談ください
書店で探す
障害者向け資料で読む
書誌情報
この資料の詳細や典拠(同じ主題の資料を指すキーワード、著者名)等を確認できます。
デジタル
- 資料種別
- 博士論文
- 著者・編者
- 永吉, 勤
- 著者標目
- 出版年月日等
- 2021
- 出版年(W3CDTF)
- 2021
- 並列タイトル等
- MAGIC望遠鏡を用いたシェル型構造天体HESS J1912+101の研究
- タイトル(掲載誌)
- 博士論文(埼玉大学大学院理工学研究科(博士後期課程))
- 授与機関名
- 埼玉大学
- 授与年月日
- 2021-03-25
- 授与年月日(W3CDTF)
- 2021-03-25
- 報告番号
- 乙第262号
- 学位
- 博士(理学)
- 博論授与番号
- 乙第262号
- 本文の言語コード
- eng
- 対象利用者
- 一般
- 一般注記
- type:textCosmic rays (CRs) were discovered by Victor Hess in 1912, however the origin is not fully understood yet. CRs mainly consists of protons, and the spectrum over 12 order of magnitude is well described by a power-law functions with three break points. CRs below the first break point, which is so-called knee ~ 10¹⁵∙⁵ eV is considered to be supplied in our Galaxy, therefore they are called Galactic Cosmic Rays (GCRs). The most possible object to supply GCRs is Supernova Remnant (SNR) because of a point view of the energy budget. In order to observe the protons at SNRs, the gamma-ray via π0 decay process (100 MeV to 100 TeV) is the only channel. In addition, young SNRs (several hundred years old), which is considered the most efficient phase to accelerate CRs, are known to have very bright Very High Energy (VHE; 100 GeV to 100 TeV) gamma ray emission. Therefore VHE gamma-rays can be called the best wavelength to study GCRs. A dozen of VHE gamma-ray SNRs have been discovered so far, and they are well studied in other wavelengths too. However, SNRs have not been concluded as the origin of GCRs. This is mainly caused by the difficulty to estimate the contribution from the leptonic interactions.HESS J1912+101 is one of the new SNRs which H.E.S.S. telescopes newly identified by performing the systematic SNR search based on a shell-like morphology. The new SNRs are discovered by only VHE gamma-rays. It indicates such SNRs have less synchrotron emission produced by electrons, therefore it can be considered that the contribution from the leptonic interactions to their gamma-ray emission is less.We performed a deep observation campaign with the MAGIC telescopes during the period of 2016-2017 collecting 87 hrs of good-quality data. The obtained morphology is parameterized by 2D likelihood fitting and the results are consistent with the H.E.S.S. result within 2σ level. Connecting the TeV and GeV emission, we could extend the spectrum to lower energies by three orders of magnitude and reveal a power-law with a hard spectral index 2.12 and a cutoff above 10 TeV. The HESS J1912+101 spectrum is well explained by the one-zone hadronic model with the proton index of 2.21 and the proton cutoff energy of > 100TeV. The results indicate that HESS J1912+101 is the young SNR and the gamma-ray emission is produced by the hadronic interactions based on the popular particle acceleration model; diffusive shock acceleration.Abstract iii1 Introduction 12 Review of cosmic rays and very high energy astrophysics 3 2.1 Cosmic rays . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3 2.1.1 Historical background of Cosmic Rays . . . . . . . . . . . . . . . . 3 2.1.2 Properties of cosmic rays . . . . . . . . . . . . . . . . . . . . . . . 3 2.1.3 Acceleration mechanisms of cosmic rays . . . . . . . . . . . . . . 7 2.1.4 The origin of galactic cosmic rays . . . . . . . . . . . . . . . . . . . 10 2.2 Gamma Rays . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11 2.2.1 Production of gamma rays . . . . . . . . . . . . . . . . . . . . . . 11 2.2.2 Comparison of gamma-ray production channels . . . . . . . . . . 14 2.3 Very high energy gamma-ray astronomy . . . . . . . . . . . . . . . . . . . 15 2.4 Cherenkov techniques . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17 2.4.1 Extensive air showrs . . . . . . . . . . . . . . . . . . . . . . . . . . 17 2.4.2 Cherenkov radiation . . . . . . . . . . . . . . . . . . . . . . . . . . 20 2.4.3 Imaging atmospheric Cherenkov telescope . . . . . . . . . . . . . 22 2.4.4 Recent telescopes and CTA . . . . . . . . . . . . . . . . . . . . . . 263 Proton accelerators 29 3.1 Supernova remnants . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29 3.1.1 Evolution of SNRs . . . . . . . . . . . . . . . . . . . . . . . . . . . 29 3.1.2 Gamma-ray emission from SNRs . . . . . . . . . . . . . . . . . . . 30 3.1.3 Hadronic versus leptonic . . . . . . . . . . . . . . . . . . . . . . . 32 3.1.4 TeV shell-type SNR candidates . . . . . . . . . . . . . . . . . . . . 35 3.2 Other accelerators . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38 3.2.1 Galactic center diffuse emission . . . . . . . . . . . . . . . . . . . . 38 3.2.2 Unidentified galactic sources . . . . . . . . . . . . . . . . . . . . . 404 MAGIC 45 4.1 MAGIC system . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 45 4.1.1 Structure, reflector and drive system . . . . . . . . . . . . . . . . . 45 4.1.2 Observation mode . . . . . . . . . . . . . . . . . . . . . . . . . . . 48 4.2 Analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 49 4.2.1 Raw level data calibration, image cleaning and stereo parameters 49 4.2.2 Data selection . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 49 4.2.3 Event reconstructions . . . . . . . . . . . . . . . . . . . . . . . . . 50 4.2.4 High level analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . 52 4.2.5 Extended source analysis . . . . . . . . . . . . . . . . . . . . . . . 57 4.3 Performance of the MAGIC system . . . . . . . . . . . . . . . . . . . . . . 61 5 The observation of HESSJ1912+101 with the MAGIC telescopes 65 5.1 Previous observations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 65 5.1.1 X-ray sources . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 65 5.1.2 Radio continuum emission . . . . . . . . . . . . . . . . . . . . . . 66 5.1.3 Radio pulsars . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 66 5.1.4 Atomic and molecular gas density and infrared emission . . . . . 67 5.1.5 GeV emission . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 68 5.2 Strategy of the MAGIC observation . . . . . . . . . . . . . . . . . . . . . . 69 5.3 Observations and data reduction . . . . . . . . . . . . . . . . . . . . . . . 71 5.4 Analysis and results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 77 5.4.1 Gamma-ray detection . . . . . . . . . . . . . . . . . . . . . . . . . 77 5.4.2 Morphology analysis . . . . . . . . . . . . . . . . . . . . . . . . . . 79 5.4.3 Spectrum analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . 86 5.4.4 Systematic uncertainties and cross calibration . . . . . . . . . . . 956 Interpretation and discussion 101 6.1 Fermi-LAT analsysis for HESS J1912+101 as an extended source . . . . . 101 6.1.1 The Fermi-LAT . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 101 6.1.2 Fermi-LAT morphology . . . . . . . . . . . . . . . . . . . . . . . . 104 6.1.3 Spectrum in Fermi-LAT energy range . . . . . . . . . . . . . . . . 106 6.2 Summary of the HESS J1912+101 observations . . . . . . . . . . . . . . . 107 6.2.1 The HESS J1912+101 morphology . . . . . . . . . . . . . . . . . . 107 6.2.2 The HESS J1912+101 SED . . . . . . . . . . . . . . . . . . . . . . . 108 6.3 The particle population in HESS J1912+101 region . . . . . . . . . . . . . 110 6.3.1 Leptonic model . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 110 6.3.2 Hadronic model . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 114 6.4 The nature of HESS J1912+101 . . . . . . . . . . . . . . . . . . . . . . . . . 121 6.4.1 SNR scenario . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 121 6.4.2 Other scenario . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 121 6.5 The index and SNR population . . . . . . . . . . . . . . . . . . . . . . . . 1227 Conclusion 127A The non-thermal emission from Kepler’s supernova remnant 129 A.1 Observations and data reduction . . . . . . . . . . . . . . . . . . . . . . . 130 A.2 Spectral analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 131 A.2.1 Hard X-ray spectrum with the HXD-PIN . . . . . . . . . . . . . . 131 A.2.2 Broad-band X-ray spectra with the XIS and HXD-PIN . . . . . . . 134 A.3 Discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 135B Observation dates of HESSJ1912+101 143 B.1 Cycle period XI . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 143 B.2 Cycle period XII . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 144 C Crab Nebula cross-check analysis 147 C.1 The data set . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 147 C.2 θ2 plots . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 147 C.3 Skymaps . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 147 C.4 Spectrum energy density . . . . . . . . . . . . . . . . . . . . . . . . . . . . 150 Acknowledgements 153指導教員 : 寺田幸功
- DOI
- 10.24561/00019581
- 国立国会図書館永続的識別子
- info:ndljp/pid/12313434
- コレクション(共通)
- コレクション(障害者向け資料:レベル1)
- コレクション(個別)
- 国立国会図書館デジタルコレクション > デジタル化資料 > 博士論文
- 収集根拠
- 博士論文(自動収集)
- 受理日(W3CDTF)
- 2022-08-08T06:02:54+09:00
- 作成日(W3CDTF)
- 2022-06-15
- 記録形式(IMT)
- application/pdf
- オンライン閲覧公開範囲
- 国立国会図書館内限定公開
- デジタル化資料送信
- 図書館・個人送信対象外
- 遠隔複写可否(NDL)
- 可
- 連携機関・データベース
- 国立国会図書館 : 国立国会図書館デジタルコレクション