Study of the shell-type astronomical object HESSJ1912+101 with the MAGIC telescopes

The cover of this title could differ from library to library.

Available in National Diet Library

Find on the publisher's website

国立国会図書館デジタルコレクション

Digital data available

Check on the publisher's website

DOI[10.24561/00019581]to the data of the same series

Study of the shell-type astronomical object HESSJ1912+101 with the MAGIC telescopes

Persistent ID (NDL): info:ndljp/pid/12313434

Material type: 博士論文

Author: 永吉, 勤

Publisher: 埼玉大学大学院理工学研究科

Publication date: 2021

Material Format: Digital

Capacity, size, etc.: -

Name of awarding university/degree: 埼玉大学,博士(理学)

View All

Notes on use at the National Diet Library

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。

Notes on use

Note (General)：: 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...

Search by Bookstore

Read this material in an accessible format.

View materials in accessible formats for people with print disabilities (1Type)

Holdings of Libraries in Japan

This page shows libraries in Japan other than the National Diet Library that hold the material.

List of Cooperating Institutions and Databases

Please contact your local library for information on how to use materials or whether it is possible to request materials from the holding libraries.

other

Saitama University Cyber Repository of Academic Resources
Digital
You can check the holdings of institutions and databases with which 学術機関リポジトリデータベース（IRDB）（機関リポジトリ） is linked at the site of 学術機関リポジトリデータベース（IRDB）（機関リポジトリ）.
Saitama University Cyber Repository of Academic Resources

Search by Bookstore

Read in Disability Resources

Other Services
- テキストデータ check it on 国立国会図書館デジタルコレクション

Bibliographic Record

You can check the details of this material, its authority (keywords that refer to materials on the same subject, author's name, etc.), etc.

Digital

Material Type: 博士論文
Title: Study of the shell-type astronomical object HESSJ1912+101 with the MAGIC telescopes
Author/Editor: 永吉, 勤
Author Heading: 永吉, 勤
Publication, Distribution, etc.: 埼玉大学大学院理工学研究科
Publication Date: 2021
Publication Date (W3CDTF): 2021
Alternative Title: MAGIC望遠鏡を用いたシェル型構造天体HESS J1912+101の研究
Periodical title: 博士論文（埼玉大学大学院理工学研究科（博士後期課程））
Degree grantor/type: 埼玉大学
Date Granted: 2021-03-25
Date Granted (W3CDTF): 2021-03-25
Dissertation Number: 乙第262号
Degree Type: 博士(理学)
Conferring No. (Dissertation): 乙第262号
Text Language Code: eng
Target Audience: 一般
Note (General): type:text
Cosmic 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
https://doi.org/10.24561/00019581
Persistent ID (NDL): info:ndljp/pid/12313434
https://dl.ndl.go.jp/pid/12313434
Collection: 障害者向け資料
Collection (Materials For Handicapped People:1): テキストデータ
Collection (particular): 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
https://dl.ndl.go.jp/collections/A00014
Acquisition Basis: 博士論文（自動収集）
Date Accepted (W3CDTF): 2022-08-08T06:02:54+09:00
Date Created (W3CDTF): 2022-06-15
Format (IMT): application/pdf
Access Restrictions: 国立国会図書館内限定公開
Service for the Digitized Contents Transmission Service: 図書館・個人送信対象外
Availability of remote photoduplication service: 可
Periodical Title (URI): http://dx.doi.org/10.24561/00019581
http://id.nii.ac.jp/1586/00019581/
Data Provider (Database): 国立国会図書館 : 国立国会図書館デジタルコレクション
https://dl.ndl.go.jp