The comptonizing medium of the black-hole X-ray binary MAXI~J1535$-$571 through type-C quasi-periodic oscillations
The comptonizing medium of the black-hole X-ray binary MAXI~J1535$-$571 through type-C quasi-periodic oscillations
We present a detailed spectral and temporal analysis of the black hole candidate MAXI J1535−571 using NICER observations in 2017 September and October. We focus specifically on observations in the hard-intermediate state when the source shows type-C quasi-periodic oscillations (QPOs). We fitted the time-averaged spectrum of the source and the rms and phase-lag spectra of the QPO with a one-component time-dependent Comptonization model. We found that the corona contracts from ∼104–3× 10 3 km as the QPO frequency increases from ∼ 1.8–9.0 Hz. The fits suggest that the system would consist of two coronas, a small one that dominates the time-averaged spectrum and a larger one, possibly the jet, that dominates the rms and lag spectra of the QPO. We found a significant break in the relation between the spectral parameters of the source and the properties of the QPO, including its lag spectra, with QPO frequency. The change in the relations happens when the QPO frequency crosses a critical frequency ν c ≈ 3.0 Hz. Interestingly, the QPO reaches this critical frequency simultaneously as the radio emission from the jet in this source is quenched.
X-rays: binaries, X-rays: individual: MAXI J1535-571, accretion, accretion discs, black hole physics, methods: observationa, software: data analysis, accretion, accretion discs, X-rays: individual: MAXI J1535−571
113-128
Rawat, Divya
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Méndez, Mariano
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García, Federico
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Altamirano, Diego
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Karpouzas, Konstantinos
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Zhang, Liang
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Alabarta, Kevin
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Belloni, Tomaso M.
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Jain, Pankaj
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Bellavita, Candela
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1 March 2023
Rawat, Divya
7c84e7db-d7ce-41be-b574-2c5d18fe2f59
Méndez, Mariano
5cc6f759-dae2-488a-9cc2-cff89f4eca72
García, Federico
7c0fed66-dda4-4333-b38c-175f570820ce
Altamirano, Diego
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Karpouzas, Konstantinos
d796fbbc-2dbb-4244-8c06-ad6466a9abc0
Zhang, Liang
216ccbc3-5449-42f1-83af-4303376c07b4
Alabarta, Kevin
8c164ccd-de85-4b2b-870b-7471ff95423b
Belloni, Tomaso M.
2658fa71-5f5a-4f0c-86b7-3b9e3a80f28b
Jain, Pankaj
17d489fa-21fa-4f8f-9eec-baea121d40c6
Bellavita, Candela
244e2625-59a8-4b89-ab4b-877cc2c213c8
Rawat, Divya, Méndez, Mariano, García, Federico, Altamirano, Diego, Karpouzas, Konstantinos, Zhang, Liang, Alabarta, Kevin, Belloni, Tomaso M., Jain, Pankaj and Bellavita, Candela
(2023)
The comptonizing medium of the black-hole X-ray binary MAXI~J1535$-$571 through type-C quasi-periodic oscillations.
Monthly Notices of the Royal Astronomical Society, 520 (1), .
(doi:10.1093/mnras/stad126).
Abstract
We present a detailed spectral and temporal analysis of the black hole candidate MAXI J1535−571 using NICER observations in 2017 September and October. We focus specifically on observations in the hard-intermediate state when the source shows type-C quasi-periodic oscillations (QPOs). We fitted the time-averaged spectrum of the source and the rms and phase-lag spectra of the QPO with a one-component time-dependent Comptonization model. We found that the corona contracts from ∼104–3× 10 3 km as the QPO frequency increases from ∼ 1.8–9.0 Hz. The fits suggest that the system would consist of two coronas, a small one that dominates the time-averaged spectrum and a larger one, possibly the jet, that dominates the rms and lag spectra of the QPO. We found a significant break in the relation between the spectral parameters of the source and the properties of the QPO, including its lag spectra, with QPO frequency. The change in the relations happens when the QPO frequency crosses a critical frequency ν c ≈ 3.0 Hz. Interestingly, the QPO reaches this critical frequency simultaneously as the radio emission from the jet in this source is quenched.
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2301.04418v1
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stad126
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Accepted/In Press date: 10 January 2023
e-pub ahead of print date: 12 January 2023
Published date: 1 March 2023
Additional Information:
Funding Information:
This research is part of a project proposed for the Committee on Space Research (COSPAR) Panel on Capacity Building (PCB) fellowship program. We would like to thank the referee for constructive comments that helped improve this paper. DR would like to thank COSPAR, Indian Space Research Organization (ISRO), and Professor Diego Altamirano for jointly funding the academic visit to the University of Southampton. MM, FG, and KK acknowledge support from the research programme Athena with project number 184.034.002, which is (partly) financed by the Dutch Research Council (NWO). FG acknowledges support from PIP 0102 and PIP 0113 (CONICET). FG is a CONICET researcher. This work received financial support from PICT-2017-2865 (ANPCyT). KA acknowledges support from a UGC-UKIERI Phase 3 Thematic Partnership (UGC-UKIERI-2017-18-006; PI: P. Gandhi). TMB acknowledges financial contribution from PRIN INAF 2019 n.15. CB is a fellow of Consejo Interuniversitario Nacional (CIN).
Funding Information:
This research is part of a project proposed for the Committee on Space Research (COSPAR) Panel on Capacity Building (PCB) fellowship program. We would like to thank the referee for constructive comments that helped improve this paper. DR would like to thank COSPAR, Indian Space Research Organization (ISRO), and Professor Diego Altamirano for jointly funding the academic visit to the University of Southampton. MM, FG, and KK acknowledge support from the research programme Athena with project number 184.034.002, which is (partly) financed by the Dutch Research Council (NWO). FG acknowledges support from PIP 0102 and PIP 0113 (CONICET). FG is a CONICET researcher. This work received financial support from PICT-2017-2865 (ANPCyT). KA acknowledges support from a UGC-UKIERI Phase 3 Thematic Partnership (UGC-UKIERI-2017-18-006; PI: P. Gandhi). TMB acknowledges financial contribution from PRIN INAF 2019 n.15. CB is a fellow of Consejo Interuniversitario Nacional (CIN).
Publisher Copyright:
© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
Keywords:
X-rays: binaries, X-rays: individual: MAXI J1535-571, accretion, accretion discs, black hole physics, methods: observationa, software: data analysis, accretion, accretion discs, X-rays: individual: MAXI J1535−571
Identifiers
Local EPrints ID: 475683
URI: http://eprints.soton.ac.uk/id/eprint/475683
ISSN: 1365-2966
PURE UUID: 2fb0a90e-e74e-49c1-b855-d738cca4ea7c
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Date deposited: 24 Mar 2023 17:36
Last modified: 17 Mar 2024 03:34
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Contributors
Author:
Divya Rawat
Author:
Mariano Méndez
Author:
Federico García
Author:
Liang Zhang
Author:
Kevin Alabarta
Author:
Tomaso M. Belloni
Author:
Pankaj Jain
Author:
Candela Bellavita
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