Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/38021
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DC Field | Value | Language |
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dc.contributor.author | Aharonian, F. | - |
dc.contributor.author | Akhperjanian, A. | - |
dc.contributor.author | Bazer-Bachi, A. | - |
dc.contributor.author | Beilicke, M. | - |
dc.contributor.author | Benbow, W. | - |
dc.contributor.author | Berge, D. | - |
dc.contributor.author | Bernlohr, K. | - |
dc.contributor.author | Boisson, C. | - |
dc.contributor.author | Bolz, O. | - |
dc.contributor.author | Borrel, V. | - |
dc.contributor.author | Braun, I. | - |
dc.contributor.author | Breitling, F. | - |
dc.contributor.author | Brown, A. | - |
dc.contributor.author | Buhler, R. | - |
dc.contributor.author | Busching, I. | - |
dc.contributor.author | Carrigan, S. | - |
dc.contributor.author | Chadwick, P. | - |
dc.contributor.author | Chounet, L. | - |
dc.contributor.author | Cornils, R. | - |
dc.contributor.author | Costamante, L. | - |
dc.contributor.author | et al. | - |
dc.date.issued | 2006 | - |
dc.identifier.citation | Astronomy and Astrophysics: a European journal, 2006; 448(2):L43-L47 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.issn | 1432-0746 | - |
dc.identifier.uri | http://hdl.handle.net/2440/38021 | - |
dc.description.abstract | The Vela supernova remnant (SNR) is a complex region containing a number of sources of non-thermal radiation. The inner section of this SNR, within 2 degrees of the pulsar PSR B0833-45, has been observed by the HESS γ-ray atmospheric Cherenkov detector in 2004 and 2005. A strong signal is seen from an extended region to the south of the pulsar, within an integration region of radius 0.8° around the position (α = 08h35 m00s, δ = -45°36′ J2000.0). The excess coincides with a region of hard X-ray emission seen by the ROSAT and ASCA satellites. The observed energy spectrum of the source between 550 GeV and 65 TeV is well fit by a power law function with photon index Γ = 1.45 ± 0.09stat ± 0.2sys and an exponential cutoff at an energy of 13.8 ± 2.3stat ± 4.1 sys TeV. The integral flux above 1 TeV is (1.28 ± 0.17 stat ± 0.38sys) × 10-11 cm -2 s-1. This result is the first clear measurement of a peak in the spectral energy distribution from a VHE γ-ray source, likely related to inverse Compton emission. A fit of an Inverse Compton model to the HESS spectral energy distribution gives a total energy in non-thermal electrons of ∼2 × 1045 erg between 5 TeV and 100 TeV, assuming a distance of 290 parsec to the pulsar. The best fit electron power law index is 2.0, with a spectral break at 67 TeV. © ESO 2006. | - |
dc.description.statementofresponsibility | F. A. Aharonian...G. P. Rowell...et al. | - |
dc.language.iso | en | - |
dc.publisher | E D P Sciences | - |
dc.rights | © The European Southern Observatory 2006 | - |
dc.source.uri | http://dx.doi.org/10.1051/0004-6361:200600014 | - |
dc.subject | ISM: plerions | - |
dc.subject | Gamma rays: observations | - |
dc.title | First detection of a VHE gamma-ray spectral maximum from a cosmic source: HESS discovery of the Vela X nebula | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1051/0004-6361:200600014 | - |
pubs.publication-status | Published | - |
dc.identifier.orcid | Rowell, G. [0000-0002-9516-1581] | - |
Appears in Collections: | Aurora harvest Physics publications |
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hdl_38021.pdf | Published version | 506.74 kB | Adobe PDF | View/Open |
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