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Tracking the variable jets of V404 Cygni during its 2015 outburst

Tetarenko, A. J. and Sivakoff, G. R. and Miller-Jones, J. C. A. and Bremer, M. and Mooley, K. P. and Fender, R. P. and Rumsey, C. and Bahramian, A. and Altamirano, D. and Heinz, S. and Maitra, D. and Markoff, S. B. and Migliari, S. and Rupen, M. P. and Russell, D. M. and Russell, T. D. and Sarazin, C. L. (2019) Tracking the variable jets of V404 Cygni during its 2015 outburst. Monthly Notices of the Royal Astronomical Society, 482 (3). pp. 2950-2972. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20190415-091844811

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Abstract

We present multifrequency monitoring observations of the black hole X-ray binary V404 Cygni throughout its 2015 June outburst. Our data set includes radio and mm/sub-mm photometry, taken with the Karl G. Jansky Very Large Array, Arc-Minute MicroKelvin Imager Large Array, Sub-millimeter Array, James Clerk Maxwell Telescope, and the Northern Extended Millimetre Array, combined with publicly available infrared, optical, UV, and X-ray measurements. With these data, we report detailed diagnostics of the spectral and variability properties of the jet emission observed during different stages of this outburst. These diagnostics show that emission from discrete jet ejecta dominated the jet emission during the brightest stages of the outburst. We find that the ejecta became fainter, slower, less frequent, and less energetic, before the emission transitioned (over 1–2 d) to being dominated by a compact jet, as the outburst decayed towards quiescence. While the broad-band spectrum of this compact jet showed very little evolution throughout the outburst decay (with the optically thick to thin synchrotron jet spectral break residing in the near-infrared/optical bands; ∼2–5 × 10^(14) Hz), the emission still remained intermittently variable at mm/sub-mm frequencies. Additionally, we present a comparison between the radio jet emission throughout the 2015 and previous 1989 outbursts, confirming that the radio emission in the 2015 outburst decayed significantly faster than in 1989. Lastly, we detail our sub-mm observations taken during the 2015 December mini-outburst of V404 Cygni, which demonstrate that, similar to the main outburst, the source was likely launching jet ejecta during this short period of renewed activity.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/sty2853DOIArticle
https://academic.oup.com/mnras/article/482/3/2950/5142704PublisherArticle
ORCID:
AuthorORCID
Tetarenko, A. J.0000-0003-3906-4354
Sivakoff, G. R.0000-0001-6682-916X
Miller-Jones, J. C. A.0000-0003-3124-2814
Mooley, K. P.0000-0002-2557-5180
Bahramian, A.0000-0003-2506-6041
Altamirano, D.0000-0002-3422-0074
Heinz, S.0000-0002-8433-8652
Markoff, S. B.0000-0001-9564-0876
Russell, D. M.0000-0002-3500-631X
Russell, T. D.0000-0001-6958-8891
Additional Information:© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2018 October 12. Received 2018 October 10; in original form 2018 June 8. Published: 23 October 2018. The authors thank the anonymous referee for constructive feedback that improved the manuscript. We wish to sincerely thank all the National Radio Astronomy Observatory, SMA, JCMT, and IRAM NOEMA staff that supported us during this observing campaign. The authors also offer a special thanks to the IRAM NOEMA Director, Karl-Fredrich Schuster, for granting our NOEMA DDT request. AJT thanks Craig Heinke and Bailey Tetarenko for useful discussions on accretion disc contributions in broad-band spectra of X-ray binaries. AJT is supported by an Natural Sciences and Engineering Research Council of Canada (NSERC) Post-Graduate Doctoral Scholarship (PGSD2-490318-2016). AJT and GRS are supported by NSERC Discovery Grants. JCAMJ is the recipient of an Australian Research Council Future Fellowship (FT140101082). SBM acknowledges support from VICI grant Nr. 639.043.513/520, funded by the Netherlands Organisation for Scientific Research (NWO). TDR acknowledges support from the NWO Veni Fellowship, grant number 639.041.646. DA acknowledges support from the Royal Society. This work is based on observations carried out under project numbers S15DE and D15AB with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the engineers and staff of the Mullard Radio Astronomy Observatory for maintenance and operation of AMI, which is supported by the Universities of Cambridge and Oxford. The AMI telescope acknowledges support from the European Research Council under grant ERC-2012-StG-307215 LODESTONE. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica. The JCMT is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan; Academia Sinica Institute of Astronomy and Astrophysics; the Korea Astronomy and Space Science Institute; the Operation, Maintenance and Upgrading Fund for Astronomical Telescopes and Facility Instruments, budgeted from the Ministry of Finance (MoF) of China and administrated by the Chinese Academy of Sciences (CAS), as well as the National Key R&D Program of China (No. 2017YFA0402700). Additional funding support is provided by the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. The authors also wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research.
Funders:
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC)PGSD2-490318-2016
Australian Research CouncilFT140101082
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)639.043.513/520
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)639.041.646
Royal SocietyUNSPECIFIED
Institut National des Sciences de l'Univers (INSU)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Max Planck SocietyUNSPECIFIED
Instituto Geográfico Nacional (IGN)UNSPECIFIED
Associated Universities, Inc.UNSPECIFIED
European Research Council (ERC)307215
Smithsonian InstitutionUNSPECIFIED
Academia SinicaUNSPECIFIED
National Key Research and Development Program of China2017YFA0402700
Science and Technology Facilities Council (STFC)UNSPECIFIED
Subject Keywords:black hole physics – stars: individual (V404 Cygni, GS 2023+338) – ISM: jets and outflows – radio continuum: stars – submillimetre: stars –X-rays: binaries
Issue or Number:3
Record Number:CaltechAUTHORS:20190415-091844811
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190415-091844811
Official Citation:A J Tetarenko, G R Sivakoff, J C A Miller-Jones, M Bremer, K P Mooley, R P Fender, C Rumsey, A Bahramian, D Altamirano, S Heinz, D Maitra, S B Markoff, S Migliari, M P Rupen, D M Russell, T D Russell, C L Sarazin, Tracking the variable jets of V404 Cygni during its 2015 outburst, Monthly Notices of the Royal Astronomical Society, Volume 482, Issue 3, January 2019, Pages 2950–2972, https://doi.org/10.1093/mnras/sty2853
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:94700
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:16 Apr 2019 23:31
Last Modified:09 Mar 2020 13:18

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