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    GRS 1739-278 observed at very low luminosity with XMM-NEWTON and NuSTAR

    247225.pdf (393.7Kb)
    Access Status
    Open access
    Authors
    Fürst, F.
    Tomsick, J.
    Yamaoka, K.
    Dauser, T.
    Miller, J.
    Clavel, M.
    Corbel, S.
    Fabian, A.
    García, J.
    Harrison, F.
    Loh, A.
    Kaaret, P.
    Kalemci, E.
    Migliari, S.
    Miller-Jones, James
    Pottschmidt, K.
    Rahoui, F.
    Rodriguez, J.
    Stern, D.
    Stuhlinger, M.
    Walton, D.
    Wilms, J.
    Date
    2016
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Fürst, F. and Tomsick, J. and Yamaoka, K. and Dauser, T. and Miller, J. and Clavel, M. and Corbel, S. et al. 2016. GRS 1739-278 observed at very low luminosity with XMM-NEWTON and NuSTAR. Astrophysical Journal. 832 (2): pp. 1-7.
    Source Title
    Astrophysical Journal
    DOI
    10.3847/0004-637X/832/2/115
    ISSN
    0004-637X
    School
    Department of Physics and Astronomy
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/FT140101082
    URI
    http://hdl.handle.net/20.500.11937/10029
    Collection
    • Curtin Research Publications
    Abstract

    We present a detailed spectral analysis of XMM-Newton and NuSTAR observations of the accreting transient black hole GRS 1739−278 during a very faint low hard state at ∼0.02% of the Eddington luminosity (for a distance of 8.5 kpc and a mass of 10 M ). The broad-band X-ray spectrum between 0.5–60 keV can be welldescribed by a power law continuum with an exponential cutoff. The continuum is unusually hard for such a low luminosity, with a photon index of Γ = 1.39 ± 0.04. We find evidence for an additional reflection component from an optically thick accretion disk at the 98% likelihood level. The reflection fraction is low with Rrefl = 0.043+0.033 −0.023. In combination with measurements of the spin and inclination parameters made with NuSTAR during a brighter hard state by Miller and co-workers, we seek to constrain the accretion disk geometry. Depending on the assumed emissivity profile of the accretion disk, we find a truncation radius of 15–35 Rg (5–12 RISCO) at the 90% confiden

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