Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/112108
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DC Field | Value | Language |
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dc.contributor.author | Abdalla, H. | - |
dc.contributor.author | Abramowski, A. | - |
dc.contributor.author | Aharonian, F. | - |
dc.contributor.author | Benkhali, F. | - |
dc.contributor.author | Angüner, E. | - |
dc.contributor.author | Arakawa, M. | - |
dc.contributor.author | Armand, C. | - |
dc.contributor.author | Arrieta, M. | - |
dc.contributor.author | Backes, M. | - |
dc.contributor.author | Balzer, A. | - |
dc.contributor.author | Barnard, M. | - |
dc.contributor.author | Becherini, Y. | - |
dc.contributor.author | Tjus, J. | - |
dc.contributor.author | Berge, D. | - |
dc.contributor.author | Bernhard, S. | - |
dc.contributor.author | Bernlöhr, K. | - |
dc.contributor.author | Blackwell, R. | - |
dc.contributor.author | Böttcher, M. | - |
dc.contributor.author | Boisson, C. | - |
dc.contributor.author | Bolmont, J. | - |
dc.contributor.author | et al. | - |
dc.date.issued | 2018 | - |
dc.identifier.citation | Astronomy and Astrophysics: a European journal, 2018; 612:A13-1-A13-8 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.issn | 1432-0746 | - |
dc.identifier.uri | http://hdl.handle.net/2440/112108 | - |
dc.description.abstract | The H.E.S.S. Collaboration has discovered a new very high energy (VHE, E > 0.1 TeV) γ-ray source, HESS J1741−302, located in the Galactic plane. Despite several attempts to constrain its nature, no plausible counterpart has been found so far at X-ray and MeV/GeV γ-ray energies, and the source remains unidentified. An analysis of 145-h of observations of HESS J1741−302 at VHEs has revealed a steady and relatively weak TeV source (~1% of the Crab Nebula flux), with a spectral index of Γ = 2.3 ± 0.2stat ± 0.2sys, extending to energies up to 10 TeV without any clear signature of a cut-off. In a hadronic scenario, such a spectrum implies an object with particle acceleration up to energies of several hundred TeV. Contrary to most H.E.S.S. unidentified sources, the angular size of HESS J1741−302 is compatible with the H.E.S.S. point spread function at VHEs, with an extension constrained to be below 0.068° at a 99% confidence level. The γ-ray emission detected by H.E.S.S. can be explained both within a hadronic scenario, due to collisions of protons with energies of hundreds of TeV with dense molecular clouds, and in a leptonic scenario, as a relic pulsar wind nebula, possibly powered by the middle-aged (20 kyr) pulsar PSR B1737−30. A binary scenario, related to the compact radio source 1LC 358.266+0.038 found to be spatially coincident with the best fit position of HESS J1741−302, is also envisaged. | - |
dc.description.statementofresponsibility | H. Abdalla … R. Blackwell … P. de Wilt … J. Hawkes … J. Lau … N. Maxted … G. Rowell … F. Voisin … et al. [The H.E.S.S. Collaboration] | - |
dc.language.iso | en | - |
dc.publisher | EDP Sciences | - |
dc.rights | © ESO 2018 | - |
dc.source.uri | http://dx.doi.org/10.1051/0004-6361/201730581 | - |
dc.subject | Gamma rays: ISM; gamma rays: general; cosmic rays; ISM: clouds | - |
dc.title | HESS J1741-302: a hidden accelerator in the Galactic plane | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1051/0004-6361/201730581 | - |
dc.relation.grant | ARC | - |
dc.relation.grant | CNRS-IN2P3 | - |
pubs.publication-status | Published | - |
Appears in Collections: | Aurora harvest 8 IPAS publications Physics publications |
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File | Description | Size | Format | |
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hdl_112108.pdf | Published version | 1.19 MB | Adobe PDF | View/Open |
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