A broadband radio view of transient jet ejecta in the black hole candidate X-ray binary MAXI J1535-571
| Autor: | Natasha Hurley-Walker, Jai Verdhan Chauhan, Steve Croft, Arash Bahramian, S. W. Duchesne, D. L. Kaplan, Thomas D. Russell, Diego Altamirano, Roberto Soria, G. E. Anderson, Melanie Johnston-Hollitt, Marcin Sokolowski, Gregory R. Sivakoff, Steven Tingay, Chris Flynn, Vinay Gupta, Cathryn M. Trott, James Miller-Jones, Randall B. Wayth, A. Paduano, H. A. Krimm, Paul Hancock |
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| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics Jet (fluid) Astrophysics::High Energy Astrophysical Phenomena X-ray binary Astrophysics::Instrumentation and Methods for Astrophysics FOS: Physical sciences Astronomy and Astrophysics Murchison Widefield Array Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Radio spectrum law.invention Radio telescope Black hole Telescope 13. Climate action Space and Planetary Science law 0103 physical sciences 010306 general physics Molonglo Observatory Synthesis Telescope Astrophysics - High Energy Astrophysical Phenomena 010303 astronomy & astrophysics |
| Popis: | We present a broadband radio study of the transient jets ejected from the black hole candidate X-ray binary MAXI J1535-571, which underwent a prolonged outburst beginning on 2 September 2017. We monitored MAXI J1535-571 with the Murchison Widefield Array (MWA) at frequencies from 119 to 186 MHz over six epochs from 20 September to 14 October 2017. The source was quasi-simultaneously observed over the frequency range 0.84-19 GHz by UTMOST (the upgraded Molonglo Observatory Synthesis Telescope), the Australian Square Kilometre Array Pathfinder, the Australia Telescope Compact Array (ATCA), and the Australian Long Baseline Array (LBA). Using the LBA observations from 23 September 2017, we measured the source size to be $34\pm1$ mas. During the brightest radio flare on 21 September 2017, the source was detected down to 119 MHz by the MWA, and the radio spectrum indicates a turnover between 250 and 500 MHz, which is most likely due to synchrotron self-absorption (SSA). By fitting the radio spectrum with a SSA model and using the LBA size measurement, we determined various physical parameters of the jet knot (identified in ATCA data), including the jet opening angle (= $4.5\pm1.2^{\circ}$) and the magnetic field strength (= $104^{+80}_{-78}$ mG). Our fitted magnetic field strength agrees reasonably well with that inferred from the standard equipartition approach, suggesting the jet knot to be close to equipartition. Our study highlights the capabilities of the Australian suite of radio telescopes to jointly probe radio jets in black hole X-ray binaries (BH-XRBs) via simultaneous observations over a broad frequency range, and with differing angular resolutions. This suite allows us to determine the physical properties of XRB jets. Finally, our study emphasizes the potential contributions that can be made by the low-frequency part of the Square Kilometre Array (SKA-Low) in the study of BH-XRBs. This article has been accepted for publication in PASA. This article has 16 pages, 7 figures and 1 table |
| Databáze: | OpenAIRE |
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