TY - JOUR
T1 - The comptonizing medium of the black hole X-ray binary MAXI J1535−571 through type-C quasi-periodic oscillations
AU - Rawat, Divya
AU - Méndez, Mariano
AU - García, Federico
AU - Altamirano, Diego
AU - Karpouzas, Konstantinos
AU - Zhang, Liang
AU - Alabarta, Kevin
AU - Belloni, Tomaso M.
AU - Jain, Pankaj
AU - Bellavita, Candela
N1 - 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.
PY - 2023/3/1
Y1 - 2023/3/1
N2 - 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.
AB - 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.
KW - accretion, accretion discs
KW - black hole physics
KW - methods: observationa
KW - software: data analysis
KW - X-rays: binaries
KW - X-rays: individual: MAXI J1535−571
UR - http://www.scopus.com/inward/record.url?scp=85150326573&partnerID=8YFLogxK
U2 - 10.1093/mnras/stad126
DO - 10.1093/mnras/stad126
M3 - Article
AN - SCOPUS:85150326573
SN - 0035-8711
VL - 520
SP - 113
EP - 128
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -