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|Title:||Discovery of molecular and atomic clouds associated with the Magellanic superbubble 30 Doradus C|
|Citation:||The Astrophysical Journal: an international review of astronomy and astronomical physics, 2017; 843(1):61-1-61-7|
|Publisher:||IOP Publishing; American Astronomical Society|
|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.|
|Appears in Collections:||Aurora harvest 4|
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