Please use this identifier to cite or link to this item: http://hdl.handle.net/2440/120257
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dc.contributor.authorSano, H.en
dc.contributor.authorYamane, Y.en
dc.contributor.authorVoisin, F.en
dc.contributor.authorFujii, K.en
dc.contributor.authorYoshiike, S.en
dc.contributor.authorInaba, T.en
dc.contributor.authorTsuge, K.en
dc.contributor.authorBabazaki, Y.en
dc.contributor.authorMitsuishi, I.en
dc.contributor.authorYang, R.en
dc.contributor.authorAharonian, F.en
dc.contributor.authorRowell, G.en
dc.contributor.authorFilipović, M.en
dc.contributor.authorMizuno, N.en
dc.contributor.authorTachihara, K.en
dc.contributor.authorKawamura, A.en
dc.contributor.authorOnishi, T.en
dc.contributor.authorFukui, Y.en
dc.date.issued2017en
dc.identifier.citationAstrophysical Journal, 2017; 843(1):61-1-61-7en
dc.identifier.issn0004-637Xen
dc.identifier.issn1538-4357en
dc.identifier.urihttp://hdl.handle.net/2440/120257-
dc.description.abstractWe 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.en
dc.description.statementofresponsibilityH. 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. Fukuien
dc.language.isoenen
dc.publisherIOP Publishing; American Astronomical Societyen
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectcosmic rays; gamma rays: ISM; ISM: bubbles; ISM: clouds; X-rays: individual (30 Doradus C)en
dc.titleDiscovery of molecular and atomic clouds associated with the Magellanic superbubble 30 Doradus Cen
dc.typeJournal articleen
dc.identifier.rmid0030072835en
dc.identifier.doi10.3847/1538-4357/aa73e0en
dc.identifier.pubid362178-
pubs.library.collectionPhysics publicationsen
pubs.library.teamDS14en
pubs.verification-statusVerifieden
pubs.publication-statusPublisheden
dc.identifier.orcidRowell, G. [0000-0002-9516-1581]en
Appears in Collections:Physics publications

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