CaltechAUTHORS
  A Caltech Library Service

A rapidly changing jet orientation in the stellar-mass black-hole system V404 Cygni

Miller-Jones, James C. A. and Tetarenko, Alexandra J. and Sivakoff, Gregory R. and Middleton, Matthew J. and Altamirano, Diego and Anderson, Gemma E. and Belloni, Tomaso M. and Fender, Rob P. and Jonker, Peter G. and Körding, Elmar G. and Krimm, Hans A. and Maitra, Dipankar and Markoff, Sera and Migliari, Simone and Mooley, Kunal P. and Rupen, Michael P. and Russell, David M. and Russell, Thomas D. and Sarazin, Craig L. and Soria, Roberto and Tudose, Valeriu (2019) A rapidly changing jet orientation in the stellar-mass black-hole system V404 Cygni. Nature, 569 (7756). pp. 374-377. ISSN 0028-0836. https://resolver.caltech.edu/CaltechAUTHORS:20190506-094217685

[img] PDF - Accepted Version
See Usage Policy.

8Mb
[img] Video (MPEG) (Video showing the evolution of the jet morphology over four hours on 22 June 2015) - Supplemental Material
See Usage Policy.

7Mb
[img] MS Excel (Source Data Fig. 1) - Supplemental Material
See Usage Policy.

2637Kb
[img] MS Excel (Source Data Fig. 2) - Supplemental Material
See Usage Policy.

612b
[img] MS Excel (Source Data Fig. 3) - Supplemental Material
See Usage Policy.

10Kb
[img] MS Excel (Source Data Fig. 4) - Supplemental Material
See Usage Policy.

9Kb
[img] MS Excel (Source Data Extended Data Fig. 1) - Supplemental Material
See Usage Policy.

14Kb
[img] MS Excel (Source Data Extended Data Fig. 2) - Supplemental Material
See Usage Policy.

400b
[img] MS Excel (Source Data Extended Data Fig. 3) - Supplemental Material
See Usage Policy.

19Kb
[img] MS Excel (Source Data Extended Data Fig. 4) - Supplemental Material
See Usage Policy.

17Kb
[img] Image (JPEG) (Extended Data Fig. 1: Position angles of the jet components on 22 June 2015) - Supplemental Material
See Usage Policy.

79Kb
[img] Image (JPEG) (Extended Data Fig. 2: Best-fitting proper motions of the different components on 22 June 2015) - Supplemental Material
See Usage Policy.

27Kb
[img] Image (JPEG) (Extended Data Fig. 3: Motion of the observed components on 22 June 2015) - Supplemental Material
See Usage Policy.

104Kb
[img] Image (JPEG) (Extended Data Fig. 4: Light curves for the individual components as a function of time on 22 June 2015) - Supplemental Material
See Usage Policy.

94Kb
[img] Image (JPEG) (Extended Data Fig. 5: Slim-disk precession parameters) - Supplemental Material
See Usage Policy.

70Kb
[img] Image (JPEG) (Extended Data Table 1 VLBA observing log for the June 2015 outburst of V404 Cygni) - Supplemental Material
See Usage Policy.

88Kb
[img] Image (JPEG) (Extended Data Table 2 Measured position angles on the plane of the sky for the 8.4-GHz monitoring observations) - Supplemental Material
See Usage Policy.

25Kb
[img] Image (JPEG) (Extended Data Table 3 Measured component parameters for the observations of 22 June 2015) - Supplemental Material
See Usage Policy.

106Kb
[img] Image (JPEG) (Extended Data Table 4 Prior distributions for the parameters of the atmospheric jitter correction model) - Supplemental Material
See Usage Policy.

29Kb
[img] Image (JPEG) (Extended Data Table 5 Inferred physical parameters for our identified paired ejecta from 22 June 2015) - Supplemental Material
See Usage Policy.

57Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20190506-094217685

Abstract

Powerful relativistic jets are one of the main ways in which accreting black holes provide kinetic feedback to their surroundings. Jets launched from or redirected by the accretion flow that powers them are expected to be affected by the dynamics of the flow, which for accreting stellar-mass black holes has shown evidence for precession due to frame-dragging effects that occur when the black-hole spin axis is misaligned with the orbital plane of its companion star. Recently, theoretical simulations have suggested that the jets can exert an additional torque on the accretion flow, although the interplay between the dynamics of the accretion flow and the launching of the jets is not yet understood. Here we report a rapidly changing jet orientation—on a time scale of minutes to hours—in the black-hole X-ray binary V404 Cygni, detected with very-long-baseline interferometry during the peak of its 2015 outburst. We show that this changing jet orientation can be modelled as the Lense–Thirring precession of a vertically extended slim disk that arises from the super-Eddington accretion rate. Our findings suggest that the dynamics of the precessing inner accretion disk could play a role in either directly launching or redirecting the jets within the inner few hundred gravitational radii. Similar dynamics should be expected in any strongly accreting black hole whose spin is misaligned with the inflowing gas, both affecting the observational characteristics of the jets and distributing the black-hole feedback more uniformly over the surrounding environment.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1038/s41586-019-1152-0DOIArticle
https://rdcu.be/bAyv7PublisherFree ReadCube access
https://arxiv.org/abs/1906.05400arXivDiscussion Paper
ORCID:
AuthorORCID
Miller-Jones, James C. A.0000-0003-3124-2814
Tetarenko, Alexandra J.0000-0003-3906-4354
Sivakoff, Gregory R.0000-0001-6682-916X
Middleton, Matthew J.0000-0002-8183-2970
Altamirano, Diego0000-0002-3422-0074
Jonker, Peter G.0000-0001-5679-0695
Krimm, Hans A.0000-0003-4348-6058
Markoff, Sera0000-0001-9564-0876
Mooley, Kunal P.0000-0002-2557-5180
Russell, David M.0000-0002-3500-631X
Russell, Thomas D.0000-0001-6958-8891
Soria, Roberto0000-0002-4622-796X
Additional Information:© 2019 Springer Nature Publishing AG. Received 29 August 2018; Accepted 06 February 2019; Published 29 April 2019. Data availability: The raw VLBA data are publicly available from the NRAO archive (https://archive.nrao.edu/archive/advquery.jsp), under project codes BM421 and BS249. All software packages used in our analysis (AIPS, Difmap, CASA, UVMULTIFIT and EMCEE) are publicly available. The final calibrated images and uv-data are available from the corresponding author upon reasonable request. The data underlying the figures are available as csv or xlsx files, and the measured positions and flux densities of all VLBA components from 22 June 2015 are included with the MCMC fitting code (see below). Code availability: The MCMC fitting code is available at https://github.com/tetarenk/jet-jitter. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. J.C.A.M.-J. is the recipient of an Australian Research Council Future Fellowship (FT140101082) funded by the Australian Government. A.J.T. is supported by a Natural Sciences and Engineering Research Council of Canada (NSERC) Post-Graduate Doctoral Scholarship (PGSD2-490318-2016). A.J.T. and G.R.S. acknowledge support from NSERC Discovery Grants (RGPIN-402752-2011 and RGPIN-06569-2016). M.J.M. acknowledges support from a Science and Technology Facilities Council (STFC) Ernest Rutherford Fellowship. D.A. acknowledges support from the Royal Society. G.E.A. is the recipient of an Australian Research Council Discovery Early Career Researcher Award (project number DE180100346) funded by the Australian Government. T.M.B. acknowledges a financial contribution from the agreement ASI-INAF n.2017-14-H.0. P.G.J. acknowledges funding from the European Research Council under ERC Consolidator Grant agreement 647208. S. Markoff and T.D.R. acknowledge support from a Netherlands Organisation for Scientific Research (NWO) Veni Fellowship and Vici Grant, respectively. K.P.M. acknowledges support from the Oxford Centre for Astrophysical Surveys, which is funded through the Hintze Family Charitable Foundation. K.P.M. is currently a Jansky Fellow of the National Radio Astronomy Observatory. This work profited from discussions carried out during a meeting on multi-wavelength rapid variability organized at the International Space Science Institute (ISSI) Beijing by T.M.B. and D. Bhattacharya. The authors acknowledge the worldwide effort in observing this outburst, and the planning tools (created by T. Marsh and coordinated by C. Knigge) that enabled these observations. Author Contributions: J.C.A.M.-J. wrote the manuscript with input from all authors. J.C.A.M.-J. wrote the observing proposal BM421 with help from all authors. G.R.S. wrote the observing proposal BS249 with help from J.C.A.M.-.J., A.J.T., R.P.F., P.G.J., G.E.A. and K.P.M. J.C.A.M.-J. designed and processed the VLBA observations. A.J.T. performed the Monte Carlo modelling. J.C.A.M.-J., A.J.T. and G.R.S. analysed the data. M.J.M. led the development of the Lense–Thirring precession scenario, with help from S. Markoff. The authors declare no competing interests.
Funders:
Funding AgencyGrant Number
Associated Universities, Inc.UNSPECIFIED
Australian Research CouncilFT140101082
Natural Sciences and Engineering Research Council of Canada (NSERC)PGSD2-490318-2016
Natural Sciences and Engineering Research Council of Canada (NSERC)RGPIN-402752-2011
Natural Sciences and Engineering Research Council of Canada (NSERC)RGPIN-06569-2016
Science and Technology Facilities Council (STFC)UNSPECIFIED
Royal SocietyUNSPECIFIED
Australian Research CouncilDE180100346
Agenzia Spaziale Italiana (ASI)2017-14-H.0
European Research Council (ERC)647208
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
Oxford Centre for Astrophysical SurveysUNSPECIFIED
Hintze Family Charitable FoundationUNSPECIFIED
Jansky FellowshipUNSPECIFIED
National Radio Astronomy ObservatoryUNSPECIFIED
Subject Keywords:Compact astrophysical objects; High-energy astrophysics; Time-domain astronomy
Issue or Number:7756
Record Number:CaltechAUTHORS:20190506-094217685
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190506-094217685
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95243
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:06 May 2019 17:11
Last Modified:04 Jun 2020 21:33

Repository Staff Only: item control page