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dc.contributor.authorAharonian, F.
dc.contributor.authorBüsching, I.
dc.contributor.authorDe Jager, O.C.
dc.contributor.authorHolleran, M.
dc.contributor.authorRaubenheimer, B.C.
dc.contributor.authorVenter, C.
dc.contributor.authorH.E.S.S. Collaboration
dc.date.accessioned2010-02-16T06:13:55Z
dc.date.available2010-02-16T06:13:55Z
dc.date.issued2008
dc.identifier.citationAharonian, F. et al. 2008. Discovery of very high energy gamma-ray emission coincident with molecular clouds in the W 28 (G6.4-0.1) field. Astronomy & astrophysics, 481(2):401-410. [http://www.aanda.org/]en
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746 (Online)
dc.identifier.urihttp://hdl.handle.net/10394/2833
dc.identifier.urihttp://dx.doi.org/10.1051/0004-6361:20077765
dc.identifier.urihttp://www.aanda.org/articles/aa/pdf/2008/14/aa7765-07.pdf
dc.description.abstractAims. Observations of shell-type supernova remnants (SNRs) in the GeV to multi-TeV γ-ray band, coupled with those at millimetre radio wavelengths, are motivated by the search for cosmic-ray accelerators in our Galaxy. The old-age mixed-morphology SNRW28 (distance ∼2 kpc) is a prime target due to its interaction with molecular clouds along its northeastern boundary and other clouds situated nearby. Methods. We observed theW28 field (for ∼40 h) at very high energy (VHE) γ-ray energies (E > 0.1 TeV) with the HESS. Cherenkov telescopes. A reanalysis of EGRET E > 100 MeV data was also undertaken. Results from the NANTEN 4 m telescope Galactic plane survey and other CO observations were used to study molecular clouds. Results. We have discovered VHE γ-ray emission (HESS J1801−233) coincident with the northeastern boundary of W 28 and a complex of sources (HESS J1800−240A, B and C) ∼0.5◦ south of W 28 in the Galactic disc. The EGRET source (GRO J1801−2320) is centred on HESS J1801−233 but may also be related to HESS J1800−240 given the large EGRET point spread function. The VHE differential photon spectra are well fit by pure power laws with indices Γ ∼ 2.3 to 2.7. The spectral indices of HESS J1800−240A, B, and C are consistent within statistical errors. All VHE sources are ∼10 in intrinsic radius except for HESS J1800−240C, which appears pointlike. The NANTEN 12CO(J = 1−0) data reveal molecular clouds positionally associating with the VHE emission, spanning a ∼15 km s−1 range in local standard of rest velocity. Conclusions. The VHE/molecular cloud association could indicate a hadronic origin for HESS J1801−233 and HESS J1800−240, and several cloud components in projection may contribute to the VHE emission. The clouds have components covering a broad velocity range encompassing the distance estimates forW28 (∼2 kpc) and extending up to ∼4 kpc. Assuming hadronic origin and distances of 2 and 4 kpc for cloud components, the required cosmic-ray density enhancement factors (with respect to the solar value) are in the range ∼10 to ∼30. If situated at 2 kpc distance, such cosmic-ray densities may be supplied by SNRs like W 28. Additionally and/or alternatively, particle acceleration may come from several catalogued SNRs and SNR candidates, the energetic ultra compact HII region W 28A2, and the HII regions M 8 and M 20, along with their associated open clusters. Further sub-mm observations would be recommended to probe in detail the dynamics of the molecular clouds at velocites >10 km s−1 and their possible connection to W 28
dc.language.isoenen
dc.publisherEDP Sciencesen
dc.titleDiscovery of very high energy gamma-ray emission coincident with molecular clouds in the W 28 (G6.4-0.1) fielden
dc.typeArticleen
dc.contributor.researchID10859748 - Holleran, Mathew
dc.contributor.researchID12006653 - Venter, Christo
dc.contributor.researchID10179240 - Raubenheimer, Barend Christoffel
dc.contributor.researchID10065857 - De Jager, Ocker Cornelis
dc.contributor.researchID13235176 - Büsching, Ingo


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