dc.contributor.author | Abramowski, A. | |
dc.contributor.author | Büsching, I. | |
dc.contributor.author | Davids, I.D. | |
dc.contributor.author | De Jager, O.C. | |
dc.contributor.author | Holleran, M. | |
dc.contributor.author | Venter, C. | |
dc.contributor.author | H.E.S.S. Collaboration | |
dc.date.accessioned | 2012-09-05T09:30:46Z | |
dc.date.available | 2012-09-05T09:30:46Z | |
dc.date.issued | 2011 | |
dc.identifier.citation | Büsching, I. et al. 2011. Detection of very-high-energy y-ray emission from the vicinity of PSR B1706-44 and G 343.1-2.3 with H.E.S.S. Astronomy & astrophysics, 528: Article no A143. [https://doi.org/10.1051/0004-6361/201015381] | en_US |
dc.identifier.issn | 0004-6361 | |
dc.identifier.issn | 1432-0746 (Online) | |
dc.identifier.uri | http://hdl.handle.net/10394/7234 | |
dc.identifier.uri | https://doi.org/10.1051/0004-6361/201015381 | |
dc.identifier.uri | https://www.aanda.org/articles/aa/abs/2011/04/aa15381-10/aa15381-10.html | |
dc.description.abstract | The γ-ray pulsar PSRB1706−44 and the adjacent supernova remnant (SNR) candidate G343.1−2.3 were observed by H.E.S.S. during a dedicated observation campaign in 2007. As a result of this observation campaign, a new source of very-high-energy (VHE; E > 100 GeV) γ-ray emission, H.E.S.S. J1708−443, was detected with a statistical significance of 7σ, although no significant point-like emission was detected at the position of the energetic pulsar itself. In this paper, the morphological and spectral analyses of the newly-discovered TeV source are presented. The centroid of H.E.S.S. J1708−443 is considerably offset from the pulsar and located near the apparent center of the SNR, at αJ2000 = 17h08m11s ± 17s and δJ2000 = −44◦20ʹ ± 4ʹ. The source is found to be significantly more extended than the H.E.S.S. point spread function (∼0.1◦), with an intrinsic Gaussian width of 0.29◦ ± 0.04◦. Its integral flux between 1 and 10 TeV is ∼3.8 × 10−12 ph cm−2 s−1, equivalent to 17% of the Crab Nebula flux in the same energy range. The measured energy spectrum is well-fit by a power law with a relatively hard photon index Γ = 2.0 ± 0.1stat ± 0.2sys. Additional multi-wavelength data, including 330 MHz VLA observations, were used to investigate the VHE γ-ray source’s possible associations with the pulsar wind nebula of PSRB1706−44 and/or with the complex radio structure of the partial shell-type SNR G343.1−2.3. | en_US |
dc.language.iso | en | en_US |
dc.publisher | EDP Sciences | en_US |
dc.subject | ISM: individual objects: G343.1-2.3 | en_US |
dc.subject | gamma rays: general | en_US |
dc.subject | pulslars: individual: PARB1706-44 | en_US |
dc.title | Detection of very-high-energy y-ray emission from the vicinity of PSR B1706-44 and G 343.1-2.3 with H.E.S.S. | en_US |
dc.type | Article | en_US |
dc.contributor.researchID | 13235176 - Büsching, Ingo | |
dc.contributor.researchID | 13146629 - Davids, Isak Delberth | |
dc.contributor.researchID | 10065857 - De Jager, Ocker Cornelis | |
dc.contributor.researchID | 12006653 - Venter, Christo | |
dc.contributor.researchID | 10859748 - Holleran, Mathew | |