The jet and arc molecular clouds toward Westerlund 2, RCW 49, and HESS J1023-575; ¹²CO and ¹³CO (J = 2-1 and J = 1-0) observations with NANTEN2 and Mopra telescope
| dc.contributor.author | Furukawa, N. | |
| dc.contributor.author | Rowell, G. | |
| dc.contributor.organisation | Institute for Photonics & Advanced Sensing (IPAS) | |
| dc.date.issued | 2014 | |
| dc.description | Extent: 20 p. | |
| dc.description.abstract | We have made new CO observations of two molecular clouds, which we call "jet" and "arc" clouds, toward the stellar cluster Westerlund 2 and the TeV γ-ray source HESS J1023–575. The jet cloud shows a linear structure from the position of Westerlund 2 on the east. In addition, we have found a new counter jet cloud on the west. The arc cloud shows a crescent shape in the west of HESS J1023–575. A sign of star formation is found at the edge of the jet cloud and gives a constraint on the age of the jet cloud to be ~Myr. An analysis with the multi CO transitions gives temperature as high as 20 K in a few places of the jet cloud, suggesting that some additional heating may be operating locally. The new TeV γ-ray images by H.E.S.S. correspond to the jet and arc clouds spatially better than the giant molecular clouds associated with Westerlund 2. We suggest that the jet and arc clouds are not physically linked with Westerlund 2 but are located at a greater distance around 7.5 kpc. A microquasar with long-term activity may be able to offer a possible engine to form the jet and arc clouds and to produce the TeV γ-rays, although none of the known microquasars have a Myr age or steady TeV γ-rays. Alternatively, an anisotropic supernova explosion which occurred ~Myr ago may be able to form the jet and arc clouds, whereas the TeV γ-ray emission requires a microquasar formed after the explosion. | |
| dc.description.statementofresponsibility | A. Ohama, T. Fukuda, K. Torii, T. Hayakawa, H. Sano, T. Okuda, H. Yamamoto, N. Moribe, A. Mizuno, H. Maezawa, T. Onishi, A. Kawamura, N. Mizuno, J. R. Dawson, T. M. Dame, Y. Yonekura, F. Aharonian, E. de Oña Wilhelmi, G. P. Rowell, R. Matsumoto, Y. Asahina, and Y. Fukui | |
| dc.identifier.citation | The Astrophysical Journal: an international review of astronomy and astronomical physics, 2014; 781(2):1-20 | |
| dc.identifier.doi | 10.1088/0004-637X/781/2/70 | |
| dc.identifier.issn | 1538-4357 | |
| dc.identifier.issn | 1538-4357 | |
| dc.identifier.orcid | Rowell, G. [0000-0002-9516-1581] | |
| dc.identifier.uri | http://hdl.handle.net/2440/82900 | |
| dc.language.iso | en | |
| dc.publisher | American Astronomical Society | |
| dc.relation.grant | ARC | |
| dc.rights | ©2014.The American Astronomical Society. All rights reserved. | |
| dc.source.uri | https://doi.org/10.1088/0004-637x/781/2/70 | |
| dc.subject | ISM: clouds | |
| dc.subject | ISM: individual objects (jet and arc molecular clouds, HESS J1023-575) | |
| dc.subject | stars: individual (Westerlund 2) | |
| dc.title | The jet and arc molecular clouds toward Westerlund 2, RCW 49, and HESS J1023-575; ¹²CO and ¹³CO (J = 2-1 and J = 1-0) observations with NANTEN2 and Mopra telescope | |
| dc.title.alternative | The jet and arc molecular clouds toward Westerlund 2, RCW 49, and HESS J1023-575; (12)CO and (13)CO (J = 2-1 and J = 1-0) observations with NANTEN2 and Mopra telescope | |
| dc.type | Journal article | |
| pubs.publication-status | Published |