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    On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249

    91355.pdf (1.071Mb)
    Access Status
    Open access
    Authors
    Bassi, T.
    Malzac, J.
    Del Santo, M.
    Jourdain, E.
    Roques, J.P.
    D'Aì, A.
    Miller-Jones, James
    Belmont, R.
    Motta, S.E.
    Segreto, A.
    Testa, V.
    Casella, P.
    Date
    2020
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Bassi, T. and Malzac, J. and Del Santo, M. and Jourdain, E. and Roques, J.P. and D'Aì, A. and Miller-Jones, J.C.A. et al. 2020. On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249. Monthly Notices of the Royal Astronomical Society. 494 (1): pp. 571-583.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/staa739
    ISSN
    0035-8711
    Faculty
    Faculty of Science and Engineering
    School
    School of Elec Eng, Comp and Math Sci (EECMS)
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/FT140101082
    URI
    http://hdl.handle.net/20.500.11937/91531
    Collection
    • Curtin Research Publications
    Abstract

    The black hole transient GRS 1716−249 was monitored from the radio to the γ -ray band during its 2016-2017 outburst. This paper focuses on the spectral energy distribution (SED) obtained in 2017 February-March, when GRS 1716−249 was in a bright hard spectral state. The soft γ -ray data collected with the INTEGRAL/SPI telescope show the presence of a spectral component that is in excess of the thermal Comptonization emission. This component is usually interpreted as inverse Compton emission from a tiny fraction of non-thermal electrons in the X-ray corona. We find that hybrid thermal/non-thermal Comptonization models provide a good fit to the X-/γ -ray spectrum of GRS 1716−249. The best-fitting parameters are typical of the bright hard state spectra observed in other black hole X-ray binaries. Moreover, the magnetized hybrid Comptonization model BELM provides an upper limit on the intensity of the coronal magnetic field of about 106 G. Alternatively, this soft γ -ray emission could originate from synchrotron emission in the radio jet. In order to test this hypothesis, we fit the SED with the irradiated disc plus Comptonization model combined with the jet internal shock emission model ISHEM. We found that a jet with an electron distribution of p = 2.1 can reproduce the soft γ -ray emission of GRS 1716−249. However, if we introduce the expected cooling break around 10 keV, the jet model can no longer explain the observed soft γ -ray emission, unless the index of the electron energy distribution is significantly harder (p < 2).

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