Investigating the disc–jet coupling in accreting compact objects using the black hole candidate Swift J1753.5−0127

Authors

  • P. Soleri,

    Corresponding author
    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
    2. Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands
      E-mail: soleri@astro.rug.nl
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  • R. Fender,

    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
    2. School of Physics and Astronomy, University of Southampton, Hampshire SO17 1BJ
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  • V. Tudose,

    1. Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, the Netherlands
    2. Astronomical Institute of the Romanian Academy, Cutitul de Argint 5, RO-040557 Bucharest, Romania
    3. Research Center for Atomic Physics and Astrophysics, Atomistilor 405, RO-077125 Bucharest, Romania
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  • D. Maitra,

    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
    2. Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USA
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  • M. Bell,

    1. School of Physics and Astronomy, University of Southampton, Hampshire SO17 1BJ
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  • M. Linares,

    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
    2. Kavli Institute for Astrophysics and Space Research, Massachussetts Institute of Technology, Cambridge, MA 02139, USA
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  • D. Altamirano,

    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
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  • R. Wijnands,

    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
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  • T. Belloni,

    1. INAF-Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate (LC), Italy
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  • P. Casella,

    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
    2. School of Physics and Astronomy, University of Southampton, Hampshire SO17 1BJ
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  • J. C. A. Miller-Jones,

    1. NRAO Headquarters, 520 Edgemont Road, Charlottesville, VA 22903, USA
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  • T. Muxlow,

    1. Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester M13 9PL
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  • M. Klein-Wolt,

    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
    2. Altran B.V., Hendrik Walaart Sacrestraat 405, 1117 BM Schiphol-Oost, the Netherlands
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  • M. Garrett,

    1. Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, the Netherlands
    2. Leiden Observatory, University of Leiden, PO Box 9513, 2300 RA Leiden, the Netherlands
    3. Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia
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  • M. van der Klis

    1. Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
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E-mail: soleri@astro.rug.nl

ABSTRACT

In studies of accreting black holes in binary systems, empirical relations have been proposed to quantify the coupling between accretion processes and ejection mechanisms. These processes are probed, respectively, by means of X-ray and radio/optical–infrared observations. The relations predict, given certain accretion conditions, the expected energy output in the form of a jet. We investigated this coupling by studying the black hole candidate Swift J1753.5−0127, via multiwavelength-coordinated observations over a period of ∼4 yr. We present the results of our campaign showing that, all along the outburst, the source features a jet that is fainter than expected from the empirical correlation between the radio and the X-ray luminosities in a hard spectral state. Because the jet is so weak in this system the near-infrared emission is, unusually for this state and luminosity, dominated by thermal emission from the accretion disc. We briefly discuss the importance and the implications of a precise determination of both the slope and the normalization of the correlations, listing some possible parameters that broad-band jet models should take into account to explain the population of sources characterized by a dim jet. We also investigate whether our data can give any hint on the nature of the compact object in the system, since its mass has not been dynamically measured.

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