A Wildly Flickering Jet in the Black Hole X-Ray Binary MAXI J1535-571

Tutkimustuotos: Lehtiartikkelivertaisarvioitu


  • Maria Cristina Baglio
  • David M. Russell
  • Piergiorgio Casella
  • Hind Al Noori
  • Aisha Al Yazeedi
  • Tomaso Belloni
  • David A.H. Buckley
  • Marion Cadolle Bel
  • Chiara Ceccobello
  • Stephane Corbel
  • Francesco Coti Zelati
  • Maria Díaz Trigo
  • Rob P. Fender
  • Elena Gallo
  • Poshak Gandhi
  • Jeroen Homan
  • Fraser Lewis
  • Thomas J. Maccarone
  • Julien Malzac
  • Sera Markoff
  • James C.A. Miller-Jones
  • Kieran O'Brien
  • Thomas D. Russell
  • Payaswini Saikia
  • Tariq Shahbaz
  • Greg R. Sivakoff
  • Roberto Soria
  • Vincenzo Testa
  • Alexandra J. Tetarenko
  • Mario E. Van Den Ancker
  • Federico M. Vincentelli


  • NYU Abu Dhabi
  • Osservatorio Astronomico di Brera
  • Osservatorio Astronomico Roma
  • South African Astronomical Observatory
  • SIXT Leasing SE
  • Chalmers University of Technology
  • CEA
  • Observatoire de Paris
  • Autonomous University of Barcelona
  • Institute of Space Studies of Catalonia
  • European Southern Observatory
  • University of Oxford
  • University of Michigan, Ann Arbor
  • University of Southampton
  • Eureka Scientific Inc
  • SRON Netherlands Institute for Space Research
  • University of Turku
  • Cardiff University
  • Liverpool John Moores University
  • Texas Tech University
  • IRAP
  • University of Amsterdam
  • Curtin University of Technology
  • Durham University
  • Instituto Astrofisico de Canarias
  • University of La Laguna
  • University of Alberta
  • University of Chinese Academy of Sciences
  • University of Sydney
  • East Asian Observatory
  • University of Insubria


We report on the results of optical, near-infrared (NIR), and mid-infrared observations of the black hole X-ray binary candidate (BHB) MAXI J1535-571 during its 2017/2018 outburst. During the first part of the outburst (MJD 58004-58012), the source shows an optical-NIR spectrum that is consistent with an optically thin synchrotron power law from a jet. After MJD 58015, however, the source faded considerably, the drop in flux being much more evident at lower frequencies. Before the fading, we measure a dereddened flux density of 100 mJy in the mid-infrared, making MAXI J1535-571 one of the brightest mid-infrared BHBs known so far. A significant softening of the X-ray spectrum is evident contemporaneous with the infrared fade. We interpret it as being due to the suppression of the jet emission, similar to the accretion-ejection coupling seen in other BHBs. However, MAXI J1535-571 did not transition smoothly to the soft state, instead showing X-ray hardness deviations associated with infrared flaring. We also present the first mid-IR variability study of a BHB on minute timescales, with a fractional rms variability of the light curves of ∼15%-22%, which is similar to that expected from the internal shock jet model, and much higher than the optical fractional rms (≲7%). These results represent an excellent case of multiwavelength jet spectral timing and demonstrate how rich, multiwavelength time-resolved data of X-ray binaries over accretion state transitions can help in refining models of the disk-jet connection and jet launching in these systems.


JulkaisuAstrophysical Journal
TilaJulkaistu - 10 marraskuuta 2018
OKM-julkaisutyyppiA1 Julkaistu artikkeli, soviteltu

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