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Interstellar gas towards the TeV γ-ray sources HESS J1640-465 and HESS J1641-463

dc.contributorSchool of Physical Sciences, University of Adelaide, Adelaide, SA 5005, Australia
dc.contributorSchool of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Armagh Observatory and Planetarium, College Hill, Armagh, BT61 9DG, Northern Ireland, UK
dc.contributorDepartment of Physics, University of Nagoya, Furo-cho, Chikusa-ku, Nagoya, 464-8601, Japan
dc.contributorMax-Planck-Institut für Kernphysik, PO Box 103980, D-69029 Heidelberg, Germany; Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland; National Research Nuclear University (MEPHI), 115409, Moscow, Russia
dc.contributorDESY, D-15738 Zeuthen, Germany
dc.contributorGRAPPA, Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, NL-1098 XH Amsterdam, the Netherlands
dc.contributorMax-Planck-Institut für Kernphysik, PO Box 103980, D-69029 Heidelberg, Germany; Instytut Fizyki Ja¸drowej PAN, ul. Radzikowskiego 152, PL-31-342 Krakow, Poland
dc.contributor.authorLau, J. C.
dc.contributor.authorRowell, G.
dc.contributor.authorBurton, M. G.
dc.contributor.authorFukui, Y.
dc.contributor.authorAharonian, F. A.
dc.contributor.authorOya, I.
dc.contributor.authorVink, J.
dc.contributor.authorOhm, S.
dc.contributor.authorCasanova, S.
dc.date.accessioned2024-02-21T11:03:27Z
dc.date.available2024-02-21T11:03:27Z
dc.date.issued2017-01-01T00:00:00Z
dc.identifier.doi10.1093/mnras/stw2692
dc.identifier.doi10.48550/arXiv.1610.05444
dc.identifier.other2016arXiv161005444L
dc.identifier.otherastro-ph.HE
dc.identifier.other10.48550/arXiv.1610.05444
dc.identifier.otherarXiv:1610.05444
dc.identifier.other2017MNRAS.464.3757L
dc.identifier.other10.1093/mnras/stw2692
dc.identifier.other2016arXiv161005444L
dc.identifier.other-
dc.identifier.urihttp://hdl.handle.net/20.500.14302/1842
dc.description.abstractWe present a detailed analysis of the interstellar medium towards the tera electron volt (TeV) γ-ray sources HESS J1640-465 and HESS J1641-463 using results from the Mopra Southern Galactic Plane CO Survey and from a Mopra 7 mm-wavelength study. The γ-ray sources are positionally coincident with two supernova remnants (SNRs) G338.3-0.0 and G338.5+0.1, respectively. A bright complex of H II regions connect the two SNRs and TeV objects. Observations in the CO(1-0) transition lines reveal substantial amounts of diffuse gas positionally coincident with the γ-ray sources at multiple velocities along the line of sight, while 7 mm observations in CS, SiO, HC<SUB>3</SUB>N and CH<SUB>3</SUB>OH transition lines reveal regions of dense, shocked gas. Archival H I data from the Southern Galactic Plane Survey was used to account for the diffuse atomic gas. Physical parameters of the gas towards the TeV sources were calculated from the data. We find that for a hadronic origin for the γ-ray emission, the cosmic ray enhancement rates are ∼10<SUP>3</SUP> and 10<SUP>2</SUP> times the local solar value for HESS J1640-465 and HESS J1641-463, respectively.
dc.publisherMonthly Notices of the Royal Astronomical Society
dc.titleInterstellar gas towards the TeV γ-ray sources HESS J1640-465 and HESS J1641-463
dc.typearticle
dc.source.journalMNRAS
dc.source.journalMNRAS.464
dc.source.volume464
refterms.dateFOA2024-02-21T11:03:27Z
dc.identifier.bibcode2017MNRAS.464.3757L


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