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Disc–jet coupling in the 2009 outburst of the black hole candidate H1743−322

Authors

  • J. C. A. Miller-Jones,

    Corresponding author
    1. International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth, WA 6845, Australia
    2. NRAO Headquarters, 520 Edgemont Road, Charlottesville, VA 22903, USA
      E-mail: james.miller-jones@curtin.edu.au
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  • G. R. Sivakoff,

    1. Department of Physics, University of Alberta, Room 238 CEB, Edmonton, AB T6G 2G7, Canada
    2. Department of Astronomy, University of Virginia, PO Box 400325, Charlottesville, VA 22904, USA
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  • D. Altamirano,

    1. Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, the Netherlands
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  • M. Coriat,

    1. Université Paris Diderot and Service d’Astrophysique, UMR AIM, CEA Saclay, F-91191 Gif-sur-Yvette, France
    2. School of Physics and Astronomy, University of Southampton, Highfield SO17 IBJ
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  • S. Corbel,

    1. Université Paris Diderot and Service d’Astrophysique, UMR AIM, CEA Saclay, F-91191 Gif-sur-Yvette, France
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  • V. Dhawan,

    1. NRAO Domenici Science Operations Center, 1003 Lopezville Road, Socorro, NM 87801, USA
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  • H. A. Krimm,

    1. NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
    2. USRA, 10211 Wincopin Circle, Suite 500, Columbia, MD 21044, USA
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  • R. A. Remillard,

    1. MIT Kavli Institute for Astrophysics and Space Research, Building 37, 70 Vassar Street, Cambridge, MA 02139, USA
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  • M. P. Rupen,

    1. NRAO Domenici Science Operations Center, 1003 Lopezville Road, Socorro, NM 87801, USA
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  • D. M. Russell,

    1. Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, the Netherlands
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  • R. P. Fender,

    1. Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, the Netherlands
    2. School of Physics and Astronomy, University of Southampton, Highfield SO17 IBJ
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  • S. Heinz,

    1. Astronomy Department, University of Wisconsin-Madison, 475 N. Charter Street, Madison, WI 53706, USA
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  • E. G. Körding,

    1. Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands
    2. Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, the Netherlands
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  • D. Maitra,

    1. Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA
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  • S. Markoff,

    1. Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, the Netherlands
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  • S. Migliari,

    1. Departament d’Astronomia i Meteorologia, Institut de Ciènces del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain
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  • C. L. Sarazin,

    1. Department of Astronomy, University of Virginia, PO Box 400325, Charlottesville, VA 22904, USA
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  • V. Tudose

    1. Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, the Netherlands
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E-mail: james.miller-jones@curtin.edu.au

ABSTRACT

We present an intensive radio and X-ray monitoring campaign on the 2009 outburst of the Galactic black hole candidate X-ray binary H1743−322. With the high angular resolution of the Very Long Baseline Array, we resolve the jet ejection event and measure the proper motions of the jet ejecta relative to the position of the compact core jets detected at the beginning of the outburst. This allows us to accurately couple the moment when the jet ejection event occurred with X-ray spectral and timing signatures. We find that X-ray timing signatures are the best diagnostic of the jet ejection event in this outburst, which occurred as the X-ray variability began to decrease and the Type C quasi-periodic oscillations disappeared from the X-ray power density spectrum. However, this sequence of events does not appear to be replicated in all black hole X-ray binary outbursts, even within an individual source. In our observations of H1743−322, the ejection was contemporaneous with a quenching of the radio emission, prior to the start of the major radio flare. This contradicts previous assumptions that the onset of the radio flare marks the moment of ejection. The jet speed appears to vary between outbursts, with a possible positive correlation with outburst luminosity. The compact core radio jet reactivated on transition to the hard intermediate state at the end of the outburst, and not when the source reached the low hard spectral state. Comparison with the known near-infrared behaviour of the compact jets suggests a gradual evolution of the compact jet power over a few days near the beginning and end of an outburst.

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