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Discovery of variable VHE gamma-ray emission from the binary system 1FGL J1018.6-5856

MPS-Authors
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Aharonian,  F.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Ait Benkhali,  Faical
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Bernloehr,  K.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

/persons/resource/persons119022

Bordas Coma,  P.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Casanova,  S.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Chakraborty,  Nachiketa
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Deil,  C.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Domainko,  W
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Edwards,  Tanya
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Eger,  Peter
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Foerster,  A.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Hahn,  Joachim
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Hermann,  G.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Hillert,  Andreas
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Hinton,  J.A.
Division Prof. Dr. James A. Hinton, MPI for Nuclear Physics, Max Planck Society;

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Hofmann,  W.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Hofverberg,  P.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Lu,  Chia-Chun
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Marandon,  Vincent
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Marx,  Ramin
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Mitchell,  A.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Panter,  M.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Parsons,  R. D.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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de los Reyes,  R.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Rieger,  F.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Viana,  Aion
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Völk,  Heinrich J.
Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society;

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Weitzel,  Quirin
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Yang,  Ruizhi
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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1503.02711.pdf
(Preprint), 472KB

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Citation

H.E.S.S. Collaboration, Abramowski, A., Aharonian, F., Ait Benkhali, F., Akhperjanian, A. G., Angüner, E. O., et al. (2015). Discovery of variable VHE gamma-ray emission from the binary system 1FGL J1018.6-5856. Astronomy and Astrophysics, 577: A131. doi:10.1051/0004-6361/201525699.


Cite as: https://hdl.handle.net/11858/00-001M-0000-0027-7A1F-8
Abstract
Re-observations with the H.E.S.S. telescope array of the very-high-energy (VHE) source HESS J1018-589 A coincident with the Fermi-LAT $\gamma$-ray binary 1FGL J1018.6-5856 have resulted in a source detection significance of more than 9$\sigma$, and the detection of variability ($\chi^2$/$\nu$ of 238.3/155) in the emitted $\gamma$-ray flux. This variability confirms the association of HESS J1018-589 A with the high-energy $\gamma$-ray binary detected by Fermi-LAT, and also confirms the point-like source as a new very-high-energy binary system. The spectrum of HESS J1018-589 A is best fit with a power-law function with photon index $\Gamma = 2.20 \pm 0.14_{\rm stat} \pm 0.2_{\rm sys}$. Emission is detected up to ~20 TeV. The mean differential flux level is $(2.9 \pm 0.4)\times10^{-13}$ 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 lightcurve. When folded on the orbital period of 16.58 days, the rebinned lightcurve peaks in phase with the observed X-ray and high-energy phaseograms. The fit of the H.E.S.S. phaseogram to a constant flux provides evidence of periodicity at the level of 3$\sigma$. The shape of the VHE phaseogram and measured spectrum suggest a low inclination, low eccentricity system with a modest impact from VHE $\gamma$-ray absorption due to pair production ($\tau$ < 1 at 300 GeV).