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|Title:||Interstellar gas toward the Magellanic supernova remnants|
|Citation:||AIP Conference Proceedings, 2017 / Aharonian, F., Hofmann, W., Rieger, F. (ed./s), vol.1792, pp.040038-1-040038-6|
|Series/Report no.:||AIP Conference Proceedings|
|Conference Name:||6th International Meeting on High Energy Gamma-Ray Astronomy 2016 (11 Jul 2016 - 15 Jul 2016 : Heidelberg, Germany)|
|Hidetoshi Sano, Kosuke Fujii, Yumiko Yamane, Tetsuta Inaba, Satoshi Yoshiike, Tatsuya Fukuda, Fabien Voisin, Gavin Rowell and Yasuo Fukui|
|Abstract:||We present new CO observations toward 25 supernova remnants (SNRs) residing with the Large Magellanic Cloud, including the TeV γ-ray sources N132D and 30 Doradus C. Our observations revealed that∼90% of the SNRs were detected by 12CO(J = 1–0) line emission with a 3σ level or higher. At least ten of them were shown to have CO clouds that have a good spatial correspondence with thermal/non-thermal X-rays; this indicates that shock-cloud interactions may have occurred. The molecular gases associated with N132D showed a high intensity ratio of 12CO J = 3–2 / 1–0 > 0.8, indicates that shock-heating occurred. We also found five molecular clouds and three Hi clouds associated with 30 Doradus C, which showed either complimentary or similar distributions to the non-thermal X-ray filaments in a 10 pc scale. The interstellar proton density of 30 Doradus C was estimated to be ∼ 60 cm−3, which corresponded to the total energy of the cosmic-ray protons being at least∼1.2×1050 erg.|
|Description:||Conference: High energy gamma-ray astronomy: 6th International Meeting on High Energy Gamma-ray Astronomy.|
|Rights:||Copyright status unknown|
|Appears in Collections:||Physics publications|
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