Letter

An elevation of 0.1 light-seconds for the optical jet base in an accreting Galactic black hole system

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Accepted:
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Abstract

Relativistic plasma jets are observed in many systems that host accreting black holes. According to theory, coiled magnetic fields close to the black hole accelerate and collimate the plasma, leading to a jet being launched1,2,3. Isolating emission from this acceleration and collimation zone is key to measuring its size and understanding jet formation physics. But this is challenging because emission from the jet base cannot easily be disentangled from other accreting components. Here, we show that rapid optical flux variations from an accreting Galactic black-hole binary are delayed with respect to X-rays radiated from close to the black hole by about 0.1 seconds, and that this delayed signal appears together with a brightening radio jet. The origin of these subsecond optical variations has hitherto been controversial4,5,6,7,8. Not only does our work strongly support a jet origin for the optical variations but it also sets a characteristic elevation of 103 Schwarzschild radii for the main inner optical emission zone above the black hole9, constraining both internal shock10 and magnetohydrodynamic11 models. Similarities with blazars12,13 suggest that jet structure and launching physics could potentially be unified under mass-invariant models. Two of the best-studied jetted black-hole binaries show very similar optical lags8,14,15, so this size scale may be a defining feature of such systems.

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Acknowledgements

This research has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA), as well as the High Energy Astrophysics Science Archive Research Center. P.G. thanks the Science and Technology Facilities Council (STFC) for support (grant reference ST/J003697/2). ULTRACAM and V.S.D. are supported by STFC grant ST/M001350/1. P.G. thanks C.B. Markwardt, C.M. Boon, A.B. Hill, M. Fiocchi, K. Forster, A. Zoghbi and T. Muñoz-Darias for help and discussions. J.C. acknowledges financial support from the Spanish Ministry of Economy, Industry and Competitiveness (MINECO) under the 2015 Severo Ochoa Program MINECO SEV-2015-0548, and to the Leverhulme Trust through grant VP2-2015-04. T.R.M. acknowledges STFC (ST/L000733/1). J.M. acknowledges financial support from the French National Research Agency (CHAOS project ANR-12-BS05-0009), and D.A. thanks the Royal Society. S.M. acknowledges support from Netherlands Organisation for Scientific Research (NWO) VICI grant no. 639.043.513. We thank P. Wallace for use of his SLA C library. P.A.C. is grateful to the Leverhulme Trust for the award of a Leverhulme Emeritus Fellowship. Part of this research was supported by the UK-India UKIERI/UGC Thematic Partnership grants UGC 2014-15/02 and IND/CONT/E/14-15/355. This work profited from discussions carried out during a meeting organized at the International Space Science Institute (ISSI) Beijing by T. Belloni andD. Bhattacharya.

Author information

Affiliations

  1. Department of Physics and Astronomy, University of Southampton, Southampton, SO17 3RT, UK

    • P. Gandhi
    • , D. Altamirano
    • , P. A. Charles
    •  & C. Knigge
  2. INAF-Osservatorio Astronomico di Cagliari, via della Scienza 5, I-09047, Selargius, Italy

    • M. Bachetti
  3. Department of Physics and Astronomy, University of Sheffield, Sheffield, S3 7RH, UK

    • V. S. Dhillon
    • , L. K. Hardy
    •  & S. P. Littlefair
  4. Instituto de Astrofisica de Canarias, 38205 La Laguna, Santa Cruz de Tenerife, Spain

    • V. S. Dhillon
    •  & J. Casares
  5. Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK

    • R. P. Fender
    • , K. Mooley
    • , J. Casares
    •  & P. A. Charles
  6. Cahill Center for Astrophysics, California Institute of Technology, 1216 East California Boulevard, Pasadena, CA, 91125, USA

    • F. A. Harrison
  7. IRAP, Université de toulouse, CNRS, UPS, CNES, Toulouse, France

    • J. Malzac
  8. Anton Pannekoek Institute for Astronomy, University of Amsterdam, 1098 XH, Amsterdam, The Netherlands

    • S. Markoff
    •  & C. Ceccobello
  9. Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK

    • T. R. Marsh
  10. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Mail Stop 169-221, Pasadena, CA, 91109, USA

    • D. Stern
  11. Space Sciences Laboratory, University of California, 7 Gauss Way, Berkeley, CA, 94720-7450, USA

    • J. A. Tomsick
  12. Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK

    • D. J. Walton
  13. INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monteporzio Catone, Italy

    • P. Casella
    •  & F. Vincentelli
  14. DiSAT, Universitá degli Studi dell’Insubria, Via Valleggio 11, I–22100, Como, Italy

    • F. Vincentelli
  15. INAF—Osservatorio Astronomico di Brera Merate, via E. Bianchi 46, I-23807, Merate, Italy

    • F. Vincentelli
  16. Departmento de Astrofísica Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain

    • J. Casares
  17. ISDC, Department of Astronomy, University of Geneva, Chemin d’Ecogia 16, CH-1290, Versoix, Switzerland

    • C. Ferrigno
  18. Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Tower Drive, Baton Rouge, LA, 70803, USA

    • R. I. Hynes
  19. ESA/ESTEC, Keplerlaan 1, 2201, AZ, Noordwijk, The Netherlands

    • E. Kuulkers
  20. Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune, 411007, India

    • M. Pahari
  21. European Southern Observatory, K. Schwarzschild-Strasse 2, D-85748, Garching bei München, Germany

    • F. Rahoui
  22. New York University Abu Dhabi, PO Box 129188, Abu Dhabi, United Arab Emirates

    • D. M. Russell
  23. Department of Physics, University of Alberta, CCIS 4-183, Edmonton, AB T6G 2E1, Canada

    • A. W. Shaw

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Contributions

P.G. wrote the ULTRACAM proposal, analysed the data and wrote the paper. The ULTRACAM observations were coordinated and carried out by L.K.H., S.P.L., V.S.D. and T.R.M. The X-ray observations were proposed by D.J.W., coordinated by D.S., J.A.T. and F.A.H., and the timing data analysed by M.B. Radio data were obtained and analysed by R.P.F. and K.M. INTEGRAL data were arranged by E.K. The remaining authors provided insight into jet physics constraints (S.M., J.M., C.C.), cross-correlation analyses (P.C., R.I.H., C.K., C.F., M.P., F.V.) and placing the source in context (D.A., J.C., P.A.C., D.M.R., F.R., A.W.S.). All authors read and commented on multiple versions of the manuscript.

Competing interests

The authors declare no competing financial interests.

Corresponding author

Correspondence to P. Gandhi.

Electronic supplementary material

  1. Supplementary Information

    5 supplementary figures, 7 sections, 47 references