Discovery of Molecular and Atomic Clouds Associated with the Magellanic 
Superbubble 30 Doradus C

Sano, H.; Yamane, Y.; Voisin, F.; Fujii, K.; Yoshiike, S.; Inaba, T.; Tsuge, K.; Babazaki, Y.; Mitsuishi, I.; Yang, R.; Aharonian, F. A.; Rowell, G.; Filipovic, M. D.; Mizuno, N.; Tachihara, K.; Kawamura, A.; Onishi, T.; Fukui, Y.

doi:10.3847/1538-4357/aa73e0

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Discovery of Molecular and Atomic Clouds Associated with the Magellanic Superbubble 30 Doradus C

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Aharonian, F. A.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Citation

Sano, H., Yamane, Y., Voisin, F., Fujii, K., Yoshiike, S., Inaba, T., et al. (2017). Discovery of Molecular and Atomic Clouds Associated with the Magellanic Superbubble 30 Doradus C. Astrophysical Journal, 843(1): 61. doi:10.3847/1538-4357/aa73e0.

Cite as: https://hdl.handle.net/21.11116/0000-0000-CE19-D

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 gamma- ray distribution may spatially match the total interstellar proton column density as well as the non-thermal X-rays. If the hadronic gamma-ray is dominant, the total energy of the cosmic-ray protons is at least similar to 1.2 x 10(50) erg with the estimated mean interstellar proton density similar to 60 cm(-3). In addition, the gamma-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.