Journal Article10.3847/1538-4357/ad1a10
Chasing the Break: Tracing the Full Evolution of a Black Hole X-Ray Binary Jet with Multiwavelength Spectral Modeling
Constanza Echibur'u-Trujillo,Alexandra J. Tetarenko,Daryl Haggard,Thomas D. Russell,Karri I. I. Koljonen,Arash Bahramian,Jingyi Wang,Michael Kremer,Joe Bright,Piergiorgio Casella,D. M. Russell,Diego Altamirano,Maria Cristina Baglio,T. Belloni,Chiara Ceccobello,S. Corbel,Maria Diaz Trigo,Dipankar Maitra,Aldrin Gabuya,Elena Gallo,S. Heinz,J. Homan,Erin Kara,Elmar Körding,F. Lewis,Matteo Lucchini,Sera Markoff,S. Migliari,J. Miller-Jones,Jerome Rodriguez,Payaswini Saikia,Craig L. Sarazin,Tariq Shahbaz,Gregory R. Sivakoff,R. Soria,V. Testa,Bailey Tetarenko,Valeriu Tudose +37 more
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TL;DR: Multiwavelength spectral modeling of MAXI J1820+070 outburst reveals the evolution of the jet launching region and its connection to the accretion flow.
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Abstract:
Black hole (BH) X-ray binaries (XRBs) are ideal targets to study the connection between accretion inflow and jet outflow. Here we present quasi-simultaneous, multiwavelength observations of the Galactic BH system MAXI J1820+070, throughout its 2018–2019 outburst. Our data set includes coverage from the radio through X-ray bands from 17 different instruments/telescopes, and encompasses 19 epochs over a 7 month period, resulting in one of the most well-sampled multiwavelength data sets of a BH XRB outburst to date. With our data, we compile and model the broadband spectra of this source using a phenomenological model that includes emission from the jet, a companion star, and an accretion flow. This modeling allows us to track the evolution of the spectral break in the jet spectrum, a key observable that samples the jet launching region. We find that the spectral break location changes over at least ≈3 orders of magnitude in electromagnetic frequency over this period. Using these spectral break measurements, we link the full cycle of jet behavior, including the rising, quenching, and reignition, to the changing accretion flow properties as the source evolves through its different accretion states. Our analysis shows consistent jet behavior with other sources in similar phases of their outbursts, reinforcing the idea that jet quenching and recovery may be a global feature of BH XRB systems in outburst. Our results also provide valuable evidence supporting a close connection between the geometry of the inner accretion flow and the base of the jet.
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Citations
Swift J1727.8-1613 has the Largest Resolved Continuous Jet Ever Seen in an X-ray Binary
Callan M. Wood,J. Miller-Jones,Arash Bahramian,S. Tingay,Steve Prabu,T. D. Russell,P. Atri,F. Carotenuto,D. Altamirano,S. Motta,L. Hyland,Cormac Reynolds,Stuart Weston,Robert Fender,E. Koerding,Dipankar Maitra,Sera Markoff,Simone Migliari,D. Russell,Craig L. Sarazin,Gregory R. Sivakoff,R. Soria,Alexandra J. Tetarenko,Valeriu Tudose +23 more
- 20 May 2024
TL;DR: Researchers observe Swift J1727.8-1613, an X-ray binary, using the Very Long Baseline Array and Long Baseline Array, revealing a large, two-sided, resolved jet extending 110 AU, with a lower limit on the jet speed of 0.27c and upper limit on jet inclination of 74 degrees.
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The Delayed Radio Emission in the Black Hole X-Ray Binary MAXI J1348-630
Bei You,Shunhu Yang,Zhen Yan,Xinwu Cao,A. A. Zdziarski +4 more
TL;DR: Researchers analyze X-ray and radio observations of black hole binary MAXI J1348-630, finding a 3-day delay between radio and X-ray emission during the rising phase, indicating Comptonization originates from advection-dominated accretion flow rather than the jet.
1
Rapid far-infrared spectral timing of X-ray binaries with PRIMA
Alexandra J. Tetarenko,Poshak Gandhi,Devraj Pawar +2 more
Abstract: Abstract. The most powerful cosmic engines in our universe are fueled by compact objects. These objects accrete large amounts of material and eject matter in the form of jets. Recent groundbreaking discoveries of gravitational waves from merging compact objects and the direct imaging of the black hole shadows with the Event Horizon Telescope represent major steps forward in our understanding of such systems. However, there exists a large population of stellar-mass compact objects in our own Galaxy, present in X-ray binaries (XRBs), which provide better laboratories with which to study the processes of accretion and ejection. XRBs produce highly variable emissions on timescales ranging from milliseconds (for light-travel time in the region close to the compact object) to weeks (governing the mass-inflow process). Therefore, high-time resolution observations can be a powerful tool to study these systems. However, as XRBs emit across the electromagnetic spectrum, a suite of facilities is needed to take full advantage of these techniques. The PRIMA Observatory (PRobe far-Infrared Mission for Astrophysics) will provide unique access to a wavelength range that has not been sampled in XRBs, representing an exciting new possibility for characterizing rapid time-domain phenomena of XRBs (and potentially other transient sources) in the far-infrared regime.
Sub-second optical/near-infrared quasi-periodic oscillations from the black hole X-ray transient Swift J1727.8–1613
F. M. Vincentelli,T. Shahbaz,P. Casella,V. S. Dhillon,Paice J,D. Altamirano,N. Castro Segura,R. Fender,P Gandhi,S Littlefair,T. Maccarone,J. Malzac,K. O'Brien,D. M. Russell,A.J. Tetarenko,Phil Uttley,A. Veledina +16 more
Abstract: ABSTRACT We report on the detection of optical/near-infrared (O-IR) quasi-periodic oscillations (QPOs) from the black hole (BH) X-ray transient Swift J1727.8–1613. We obtained three X-ray and O-IR high-time-resolution observations of the source during its intermediate state (2023 September 9, 15, and 17) using NICER, HAWK-I@VLT, HIPERCAM@GTC, and ULTRACAM@NTT. We clearly detected a QPO in the X-ray and O-IR bands during all three epochs. The QPO evolved, drifting from 1.4 Hz in the first epoch, up to 2.2 Hz in the second, and finally reaching 4.2 Hz in the third epoch. These are among the highest O-IR QPO frequencies detected for a BH X-ray transient. During the first two epochs, the X-ray and O-IR emission are correlated, with an optical lag (compared to the X-rays) varying from +70 to 0 ms. Finally, during the third epoch, we measured, for the first time, a lag of the $z_s$ band with respect to the $g_s$ band at the QPO frequency ($\approx$ +10 ms). By estimating the variable O-IR SED we find that the emission is most likely non-thermal. Current state-of-the-art models can explain some of these properties, but neither the jet nor the hot flow model can easily explain the observed evolution of the QPOs. While this allowed us to put tight constraints on these components, more frequent coverage of the state transition with fast multiwavelength observations is still needed to fully understand the evolution of the disc/jet properties in BH low-mass X-ray binaries.
Evolution of accretion disk structure of the black hole X-ray binary MAXI J1820+070 during the rebrightening phase
Tomohiro Yoshitake,Megumi Shidatsu,Yoshihiro Ueda,Daisaku Nogami,Katsuhiro L Murata,Narikazu Higuchi,Keisuke Isogai,Hiroyuki Maehara,Shin Mineshige,Hitoshi Negoro,Nobuyuki Kawai,Yoichi Yatsu,Mahito Sasada,Ichiro Takahashi,Masafumi Niwano,Tomoki Saito,Masaki Takayama,Yumiko Oasa,Takuya Takarada,T. Shigeyoshi +19 more
TL;DR: Evolution of accretion disk structure of MAXI J1820+070 during the rebrightening phase shows the presence of both hot corona and cool disk structures.
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