| Item type |
デフォルトアイテムタイプ_（フル）(1) |
| 公開日 |
2023-03-18 |
| タイトル |
|
|
タイトル |
Observations of the Large Magellanic Cloud with Fermi |
|
言語 |
en |
| 作成者 |
Fukazawa, Yasushi
Hanabata, Yoshitaka
Katagiri, Hideaki
Mizuno, Tsunefumi
Ohsugi, Takashi
Takahashi, Hiromitsu
|
| アクセス権 |
|
|
アクセス権 |
open access |
|
アクセス権URI |
http://purl.org/coar/access_right/c_abf2 |
| 権利情報 |
|
|
権利情報 |
Copyright (c) 2010 The European Southern Observatory |
| 主題 |
|
|
主題Scheme |
Other |
|
主題 |
acceleration of particles |
| 主題 |
|
|
主題Scheme |
Other |
|
主題 |
cosmic rays |
| 主題 |
|
|
主題Scheme |
Other |
|
主題 |
Magellanic Clouds |
| 主題 |
|
|
主題Scheme |
Other |
|
主題 |
gamma rays: galaxies |
| 主題 |
|
|
主題Scheme |
NDC |
|
主題 |
440 |
| 内容記述 |
|
|
内容記述 |
Context. The Large Magellanic Cloud (LMC) is to date the only normal external galaxy that has been detected in high-energy gamma rays. High-energy gamma rays trace particle acceleration processes and gamma-ray observations allow the nature and sites of acceleration to be studied. Aims. We characterise the distribution and sources of cosmic rays in the LMC from analysis of gamma-ray observations. Methods. We analyse 11 months of continuous sky-survey observations obtained with the Large Area Telescope aboard the Fermi Gamma-Ray Space Telescope and compare it to tracers of the interstellar medium and models of the gamma-ray sources in the LMC. Results. The LMC is detected at 33σ significance. The integrated >100 MeV photon flux of the LMC amounts to (2.6 ± 0.2) × 10-7 ph cm-2 s-1 which corresponds to an energy flux of (1.6 ± 0.1) × 10-10 erg cm-2 s-1, with additional systematic uncertainties of 16%. The analysis reveals the massive star forming region 30 Doradus as a bright source of gamma-ray emission in the LMC in addition to fainter emission regions found in the northern part of the galaxy. The gamma-ray emission from the LMC shows very little correlation with gas density and is rather correlated to tracers of massive star forming regions. The close confinement of gamma-ray emission to star forming regions suggests a relatively short GeV cosmic-ray proton diffusion length. Conclusions. The close correlation between cosmic-ray density and massive star tracers supports the idea that cosmic rays are accelerated in massive star forming regions as a result of the large amounts of kinetic energy that are input by the stellar winds and supernova explosions of massive stars into the interstellar medium. |
|
言語 |
en |
| 出版者 |
|
|
出版者 |
EDP Sciences S A |
| 言語 |
|
|
言語 |
eng |
| 資源タイプ |
|
|
資源タイプ識別子 |
http://purl.org/coar/resource_type/c_6501 |
|
資源タイプ |
journal article |
| 出版タイプ |
|
|
出版タイプ |
VoR |
|
出版タイプResource |
http://purl.org/coar/version/c_970fb48d4fbd8a85 |
| 関連情報 |
|
|
|
識別子タイプ |
DOI |
|
|
関連識別子 |
10.1051/0004-6361/200913474 |
| 関連情報 |
|
|
|
識別子タイプ |
DOI |
|
|
関連識別子 |
http://dx.doi.org/10.1051/0004-6361/200913474 |
| 収録物識別子 |
|
|
収録物識別子タイプ |
ISSN |
|
収録物識別子 |
0004-6361 |
| 収録物識別子 |
|
|
収録物識別子タイプ |
NCID |
|
収録物識別子 |
AA00553195 |
| 開始ページ |
|
|
開始ページ |
A7-1 |
| 書誌情報 |
Astronomy & Astrophysics
Astronomy & Astrophysics
巻 512,
p. A7-1-A7-15,
発行日 2010
|
| 旧ID |
31168 |
AstronAstrophys_512_A7.pdf (3.8 MB)
