Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/103026
Citations | ||
Scopus | Web of Science® | Altmetric |
---|---|---|
?
|
?
|
Full metadata record
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Abramowski, A. | - |
dc.contributor.author | Aharonian, F. | - |
dc.contributor.author | Ait Benkhali, F. | - |
dc.contributor.author | Akhperjanian, A. | - |
dc.contributor.author | Angüner, E. | - |
dc.contributor.author | Backes, M. | - |
dc.contributor.author | Balzer, A. | - |
dc.contributor.author | Becherini, Y. | - |
dc.contributor.author | Becker Tjus, J. | - |
dc.contributor.author | Berge, D. | - |
dc.contributor.author | Bernhard, S. | - |
dc.contributor.author | Bernlöhr, K. | - |
dc.contributor.author | Birsin, E. | - |
dc.contributor.author | Blackwell, R. | - |
dc.contributor.author | Böttcher, M. | - |
dc.contributor.author | Boisson, C. | - |
dc.contributor.author | Bolmont, J. | - |
dc.contributor.author | Bordas, P. | - |
dc.contributor.author | Bregeon, J. | - |
dc.contributor.author | Brun, F. | - |
dc.contributor.author | et al. | - |
dc.date.issued | 2015 | - |
dc.identifier.citation | Astronomy and Astrophysics: a European journal, 2015; 577:A131-1-A131-6 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.issn | 1432-0746 | - |
dc.identifier.uri | http://hdl.handle.net/2440/103026 | - |
dc.description.abstract | Re-observations with the HESS telescope array of the very high-energy (VHE) source HESS J1018–589A that is coincident with the Fermi- LAT γ-ray binary 1FGL J1018.6–5856 have resulted in a source detection significance of more than 9σ and the detection of variability (χ2/ν of 238.3/155) in the emitted γ-ray flux. This variability confirms the association of HESS J1018–589A with the high-energy γ-ray binary detected by Fermi-LAT and also confirms the point-like source as a new VHE binary system. The spectrum of HESS J1018–589A is best fit with a power-law function with photon index ⌈ = 2:20 ± 0:14stat 0:2sys. Emission is detected up to ∼20 TeV. The mean differential flux level is (2:9 ± 0:4) x 10⁻¹³ TeV⁻¹ cm⁻² s⁻¹ at 1 TeV, equivalent to ∼1% of the flux from the Crab Nebula at the same energy. Variability is clearly detected in the night-by-night light curve. When folded on the orbital period of 16.58 days, the rebinned light curve peaks in phase with the observed X-ray and high-energy phaseograms. The fit of the HESS phaseogram to a constant flux provides evidence of periodicity at the level of Nσ > 3σ. The shape of the VHE phaseogram and measured spectrum suggest a low-inclination, low-eccentricity system with a modest impact from VHE Υ-ray absorption due to pair production (ζ≲1 at 300 GeV). | - |
dc.description.statementofresponsibility | A. Abramowski ... J. Lau ... G. Rowell ... F. Voisin ... et al. (The H.E.S.S. Collaboration) | - |
dc.language.iso | en | - |
dc.publisher | EDP Sciences | - |
dc.rights | © ESO 2015. Article published by EDP Sciences | - |
dc.source.uri | http://dx.doi.org/10.1051/0004-6361/201525699 | - |
dc.title | Discovery of variable VHE γ -ray emission from the binary system 1FGL J1018.6-5856 | - |
dc.title.alternative | Discovery of variable VHE gamma -ray emission from the binary system 1FGL J1018.6-5856 | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1051/0004-6361/201525699 | - |
pubs.publication-status | Published | - |
Appears in Collections: | Aurora harvest 7 Chemistry and Physics publications |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
hdl_103026.pdf | Published version | 586.01 kB | Adobe PDF | View/Open |
Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.