mirage

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. 

Boloka/Manakin Repository

Show simple item record

dc.contributor.author Davids, Isak Delberth
dc.contributor.author Holleran, Mathew
dc.contributor.author Venter, Christo
dc.contributor.author Büsching, Ingo
dc.contributor.author De Jager, Ocker Cornelis
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(A143):1-12. [http://www.aanda.org] en_US
dc.identifier.issn 0004-6361
dc.identifier.issn 1432-0746 (Online)
dc.identifier.uri http://hdl.handle.net/10394/7234
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.description.uri http://dx.doi.org/10.1051/0004-6361/201015381
dc.description.uri http://www.aanda.org/index.php?option=com_article&access=standard&Itemid=129&url=/articles/aa/abs/2011/04/aa15381-10/aa15381-10.html
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


Files in this item

This item appears in the following Collection(s)

Show simple item record

Search the NWU Repository


Advanced Search

Browse

My Account

Statistics