Please use this identifier to cite or link to this item: https://hdl.handle.net/2440/112350
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dc.contributor.authorFukui, Y.-
dc.contributor.authorSano, H.-
dc.contributor.authorSato, J.-
dc.contributor.authorOkamoto, R.-
dc.contributor.authorFukuda, T.-
dc.contributor.authorYoshiike, S.-
dc.contributor.authorHayashi, K.-
dc.contributor.authorTorii, K.-
dc.contributor.authorHayakawa, T.-
dc.contributor.authorRowell, G.-
dc.contributor.authorFilipović, M.-
dc.contributor.authorMaxted, N.-
dc.contributor.authorMcclure-Griffiths, N.-
dc.contributor.authorKawamura, A.-
dc.contributor.authorYamamoto, H.-
dc.contributor.authorOkuda, T.-
dc.contributor.authorMizuno, N.-
dc.contributor.authorTachihara, K.-
dc.contributor.authorOnishi, T.-
dc.contributor.authorMizuno, A.-
dc.contributor.authoret al.-
dc.date.issued2017-
dc.identifier.citationThe Astrophysical Journal: an international review of astronomy and astronomical physics, 2017; 850(1):71-1-71-19-
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357-
dc.identifier.urihttp://hdl.handle.net/2440/112350-
dc.description.abstractWe present a new analysis of the interstellar protons toward the TeV γ-ray SNR RX J0852.0−4622 (G266.2−1.2, Vela Jr.). We used the NANTEN2 12CO(J = 1–0) and Australia Telescope Compact Array and Parkes H i data sets in order to derive the molecular and atomic gas associated with the TeV γ-ray shell of the SNR. We find that atomic gas over a velocity range from V LSR = −4 to 50 km s−1 or 60 km s−1 is associated with the entire SNR, while molecular gas is associated with a limited portion of the SNR. The large velocity dispersion of the H i is ascribed to the expanding motion of a few H i shells overlapping toward the SNR but is not due to the Galactic rotation. The total masses of the associated H i and molecular gases are estimated to be $\sim 2.5\times {10}^{4}$ M ⊙ and ~103 M ⊙, respectively. A comparison with the High Energy Stereoscopic System TeV γ-rays indicates that the interstellar protons have an average density around 100 cm−3 and shows a good spatial correspondence with the TeV γ-rays. The total cosmic-ray proton energy is estimated to be ~1048 erg for the hadronic γ-ray production, which may still be an underestimate by a factor of a few due to a small filling factor of the SNR volume by the interstellar protons. This result presents a third case, after RX J1713.7−3946 and HESS J1731−347, of the good spatial correspondence between the TeV γ-rays and the interstellar protons, lending further support for a hadronic component in the γ-rays from young TeV γ-ray SNRs.-
dc.description.statementofresponsibilityY. Fukui, H. Sano, J. Sato, R. Okamoto, T. Fukuda ... Gavin P. Rowell ... et al.-
dc.language.isoen-
dc.publisherIOP Publishing-
dc.rights© 2017. The American Astronomical Society. All rights reserved.-
dc.source.urihttp://dx.doi.org/10.3847/1538-4357/aa9219-
dc.subjectCosmic rays-gamma rays: ISM-ISM: clouds-ISM: individual objects (RX J0852.0-4622)-ISM: supernova remnants-
dc.titleA detailed study of the interstellar protons toward the TeV γ-Ray SNR RX J0852.0-4622 (G266.2-1.2, Vela Jr.): the third case of the γ-Ray and ISM spatial correspondence-
dc.typeJournal article-
dc.identifier.doi10.3847/1538-4357/aa9219-
pubs.publication-statusPublished-
dc.identifier.orcidRowell, G. [0000-0002-9516-1581]-
Appears in Collections:Aurora harvest 8
Chemistry and Physics publications

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