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https://hdl.handle.net/2440/102504
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dc.contributor.author | Voisin, F. | - |
dc.contributor.author | Rowell, G. | - |
dc.contributor.author | Burton, M. | - |
dc.contributor.author | Walsh, A. | - |
dc.contributor.author | Fukui, Y. | - |
dc.contributor.author | Aharonian, F. | - |
dc.date.issued | 2016 | - |
dc.identifier.citation | Monthly Notices of the Royal Astronomical Society, 2016; 458(3):2813-2835 | - |
dc.identifier.issn | 0035-8711 | - |
dc.identifier.issn | 1365-2966 | - |
dc.identifier.uri | http://hdl.handle.net/2440/102504 | - |
dc.description.abstract | HESS J1825−137 is a pulsar wind nebula (PWN) whose TeV emission extends across ∼1 deg. Its large asymmetric shape indicates that its progenitor supernova interacted with a molecular cloud located in the north of the PWN as detected by previous CO Galactic survey (e.g. Lemiere, Terrier & Djannati-Ataï). Here, we provide a detailed picture of the interstellar medium (ISM) towards the region north of HESS J1825−137, with the analysis of the dense molecular gas from our 7 and 12 mm Mopra survey and the more diffuse molecular gas from the Nanten CO(1–0) and GRS 13CO(1–0) surveys. Our focus is the possible association between HESS J1825−137 and the unidentified TeV source to the north, HESS J1826−130. We report several dense molecular regions whose kinematic distance matched the dispersion measured distance of the pulsar. Among them, the dense molecular gas located at (RA, Dec.) = (18h421h,−13 ∘.282) shows enhanced turbulence and we suggest that the velocity structure in this region may be explained by a cloud–cloud collision scenario. Furthermore, the presence of a H α rim may be the first evidence of the progenitor supernova remnant (SNR) of the pulsar PSR J1826−1334 as the distance between the H α rim and the TeV source matched with the predicted SNR radius RSNR ∼ 120 pc. From our ISM study, we identify a few plausible origins of the HESS J1826−130 emission, including the progenitor SNR of PSR J1826−1334 and the PWN G018.5−0.4 powered by PSR J1826−1256. A deeper TeV study however, is required to fully identify the origin of this mysterious TeV source. | - |
dc.description.statementofresponsibility | F. Voisin, G. Rowell, M. G. Burton, A. Walsh, Y. Fukui and F. Aharonian | - |
dc.language.iso | en | - |
dc.publisher | Oxford University Press | - |
dc.rights | © 2016 The Authors | - |
dc.source.uri | http://dx.doi.org/10.1093/mnras/stw473 | - |
dc.subject | Molecular data; pulsars; individual; PSR J1826−1334; ISM; clouds; cosmic rays; gamma-rays; ISM | - |
dc.title | ISM gas studies towards the TeV PWN HESS J1825-137 and northern region | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1093/mnras/stw473 | - |
pubs.publication-status | Published | - |
dc.identifier.orcid | Rowell, G. [0000-0002-9516-1581] | - |
Appears in Collections: | Aurora harvest 3 Physics publications |
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