Please use this identifier to cite or link to this item: http://hdl.handle.net/2440/120257
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Type: Journal article
Title: Discovery of molecular and atomic clouds associated with the Magellanic superbubble 30 Doradus C
Author: Sano, H.
Yamane, Y.
Voisin, F.
Fujii, K.
Yoshiike, S.
Inaba, T.
Tsuge, K.
Babazaki, Y.
Mitsuishi, I.
Yang, R.
Aharonian, F.
Rowell, G.
Filipović, M.
Mizuno, N.
Tachihara, K.
Kawamura, A.
Onishi, T.
Fukui, Y.
Citation: Astrophysical Journal, 2017; 843(1):61-1-61-7
Publisher: IOP Publishing; American Astronomical Society
Issue Date: 2017
ISSN: 0004-637X
1538-4357
Statement of
Responsibility: 
H. Sano, Y. Yamane, F. Voisin, K. Fujii, S. Yoshiike, T. Inaba, K. Tsuge, Y. Babazaki, I. Mitsuishi, R. Yang, F. Aharonian, G. Rowell, M.D. Filipović, N. Mizuno, K. Tachihara, A. Kawamura, T. Onishi, and Y. Fukui
Abstract: We analyzed the 2.6 mm CO and 21 cm H i lines toward the Magellanic superbubble 30 Doradus C, in order to reveal the associated molecular and atomic gas. We uncovered five molecular clouds in a velocity range from 251 to 276 km s⁻¹ toward the western shell. The non-thermal X-rays are clearly enhanced around the molecular clouds on a parsec scale, suggesting possible evidence for magnetic field amplification via shock–cloud interaction. The thermal X-rays are brighter in the eastern shell, where there are no dense molecular or atomic clouds, opposite to the western shell. The TeV γ-ray distribution may spatially match the total interstellar proton column density as well as the non-thermal X-rays. If the hadronic γ-ray is dominant, the total energy of the cosmic-ray protons is at least ∼1.2 × 10⁵⁰ erg with the estimated mean interstellar proton density ~60 cm⁻³. In addition, the γ-ray flux associated with the molecular cloud (e.g., MC3) could be detected and resolved by the Cherenkov Telescope Array (CTA). This should permit CTA to probe the diffusion of cosmic-rays into the associated dense ISM.
Keywords: cosmic rays; gamma rays: ISM; ISM: bubbles; ISM: clouds; X-rays: individual (30 Doradus C)
Rights: © 2017. The American Astronomical Society. All rights reserved.
RMID: 0030072835
DOI: 10.3847/1538-4357/aa73e0
Appears in Collections:Physics publications

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