INSIGHT-HXMT Observations of the New Black Hole Candidate MAXI J1535−571: Timing Analysis

Huang, Y.; Qu, J. L.; Zhang, Shuang‐Nan; Bu, Q. C.; Chen, Y. P.; Tao, Lian; Zhang, S.; Lu, Fangjun; Li, T. P.; Song, Liming; Xu, Y. P.; Cao, X. L.; Chen, Y.; Liu, C. Z.; Chang, Hsiang-Kuang; Yu, Wenfei; Weng, Shanshan; Hou, X.; Kong, Albert; Xie, Fu-Guo; Zhang, Guangbin; Zhou, Jianfeng; Chang, Zhi; Chen, G.; Chen, L.; Chen, T. X.; Chen, Y. B.; Cui, Wei; Cui, Wei; Deng, J. K.; Dong, Yongwei; Du, Yongzhai; Fu, M. X.; Gao, G. H.; Gao, He; Gao, Min; Ge, M. Y.; Gu, Y. D.; Guan, J.; Güngör, Can; Guo, Chengcheng; Han, Danxiang; Hu, W.; Jia, Haiqiang; Ji, Junhua; Jia, S.; Jiang, Luhua; Jiang, Weichun; Jin, J.; Jin, Yongjie; Li, B.; Li, C. K.; Li, G.; Li, M. S.; Li, W.; Li, Xin; Li, X. B.; Li, X. F.; Li, Y. G.; Li, Z. J.; W., Li, Z.; Liang, X. H.; Liao, J. Y.; Liu, G. Q.; Liu, H. W.; Liu, S. Z.; Liu, X. J.; Liu, Y.; Liu, Y. N.; Lü, Bo; Lu, X. F.; Luo, T.; Ma, Xiang; Meng, Bin; Nang, Y.; Nie, J. Y.; Ou, G.; Sai, N.; Shang, R. C.; Sun, Liang; Tan, Ying; Tao, W. H.; Tuo, Y. L.; Wang, G. F.; Wang, H. Y.; Wang, J.; Wang, W. S.; Wang, Y. S.; Wen, Xiang-Yang; Wu, B. B.; Wu, Mei‐Hwan; Xiao, G. C.; Xiong, S. L.; Xu, He; Yan, Linyin; Yang, Jianping; Yang, S.; Yang, Yi-Jung; Zhang, A. M.; Zhang, C. L.; Zhang, C. M.; Zhang, Faming; Zhang, H. M.; Zhang, J.; Zhang, Q.; Zhang, T.; Zhang, W.; Zhang, W. C.; Zhang, W. Z.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. J.; Zhang, Zhaojian; Zhang, Z. L.; Zhao, H. S.; Zhao, Jianling; Zhao, X. F.; Zheng, S.; Zhu, Yajun; Zou, C. L.

doi:10.3847/1538-4357/aade4c

Cited by 90 publications

(95 citation statements)

References 48 publications

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“…Low-frequency QPOs have been observed in almost all the transient BHBs (e.g. Miyamoto et al 1991;Takizawa et al 1997;Méndez et al 1998;Tomsick & Kaaret 2000;Kalemci et al 2003;Casella et al 2004;Homan et al 2005;Yadav et al 2016;Huang et al 2018;Xu et al 2019), and can be further classified into three categories, dubbed type-A, -B, and -C, based on differences in PDS shape and phase-lag behaviour (Wijnands et al 1999;Remillard et al 2002;Casella et al 2005). In contrast, only nine sources show a handful of high-frequency QPOs (e.g.…”

Section: Introductionmentioning

confidence: 99%

A systematic analysis of the phase lags associated with the type-C quasi-periodic oscillation in GRS 1915+105

Zhang

Méndez

Altamirano

et al. 2020

Monthly Notices of the Royal Astronomical Society

115

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We present a systematic analysis of the phase lags associated with the type-C QPOs in GRS 1915+105 using RXTE data. Our sample comprises of 620 RXTE observations with type-C QPOs ranging from ∼ 0.4 Hz to ∼ 6.3 Hz. Based on our analysis, we confirm that the QPO phase lags decrease with QPO frequency, and change sign from positive to negative at a QPO frequency of ∼ 2 Hz. In addition, we find that the slope of this relation is significantly different between QPOs below and above 2 Hz. The relation between the QPO lags and QPO rms can be well fitted with a broken line: as the QPO lags go from negative to positive, the QPO rms first increases, reaching its maximum at around zero lag, and then decreases. The phase-lag behaviour of the subharmonic of the QPO is similar to that of the QPO fundamental, where the subharmonic lags decrease with subharmonic frequency and change sign from positive to negative at a subharmonic frequency of ∼ 1 Hz; on the contrary, the second harmonic of the QPO shows a quite different phase-lag behaviour, where all the second harmonics show hard lags that remain more or less constant. For both the QPO and its (sub)harmonics, the slope of the lag-energy spectra shows a similar evolution with frequency as the average phase lags. This suggests that the lag-energy spectra drives the average phase lags. We discuss the possibility for the change in lag sign, and the physical origin of the QPO lags.

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Section: Introductionmentioning

confidence: 99%

A systematic analysis of the phase lags associated with the type-C quasi-periodic oscillation in GRS 1915+105

Zhang

Méndez

Altamirano

et al. 2020

Monthly Notices of the Royal Astronomical Society

115

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“…The exposure is about 520 ks for observation P0101297 and P0101322. The data reduction for PSR B0540-69 observations is done by HXMTDAS software v2.0 and the data processing is described in Chen et al (2018), Huang et al (2018) and Tuo et al (2019).…”

Section: Data Reductionmentioning

confidence: 99%

The braking index of PSR B0540−69 and the associated pulsar wind nebula emission after spin-down rate transition

Wang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In Dec. 2011 PSR B0540-69 experienced a spin-down rate transition (SRT), after which the spin-down power of the pulsar increased by " 36%. About 1000 days after the SRT, the X-ray luminosity of the associated pulsar wind nebula (PWN) was found to brighten by 32˘8%. After the SRT, the braking index n of PSR B0540-69 changes from n " 2.12 to n " 0.03 and then keeps this value for about five years before rising to n " 0.9 in the following years. We find that most of the current models have difficulties in explaining the measured braking index. One exceptive model of the braking index evolution is the increasing dipole magnetic field of PSR B0540-69. We suggest that the field increase may result from some instabilities within the pulsar core that enhance the poloidal component at the price of toroidal component of the magnetic field. The increasing dipole magnetic field will result in the X-ray brightening of the PWN. We fit the PWN X-ray light curve by two models: one assumes a constant magnetic field within the PWN during the brightening and the other assumes an enhanced magnetic field proportional to the energy density of the PWN. It appears that the two models fit the data well, though the later model seems to fit the data a bit better. This provides marginal observational evidence that magnetic field in the PWN is generated by the termination shock. Future high-quality and high-cadence data are required to draw a solid conclusion.

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“…The criteria for filtering the data of the three main instruments are: (1) pointing offset angle < 0.05 • ; (2) elevation angle > 6 • ; (3) value of the geomagnetic cutoff rigidity > 6 [16]. Since LE detectors are much more sensitive to bright earth, we set the bright earth elevation angle (DYE ELV) > 40 • which is higher than that of ME/HE (DYE ELV > 0 • ).…”

Section: Data Reductionmentioning

confidence: 99%

“…The background lightcurves are generated by the latest background software. The count rate of blind FoV detectors are used to extract the background by a rough proportional correction B = N * C b when generating the net lightcurves, where B stands for background count rate of the selected data, C b stands for the rate of blind FoV detectors and N for the proportional coefficient [16]. We chose only the small FoV detectors for LE/ME because the background of large FoV detectors is much higher.…”

Section: Data Reductionmentioning

confidence: 99%

Timing analysis of Swift J1658.2–4242's outburst in 2018 with Insight-HXMT, NICER and AstroSat

Xiao

et al. 2019

Journal of High Energy Astrophysics

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We present the observational results from a detailed timing analysis of the black hole candidate Swift J1658.2-4242 during its 2018 outburst with the observations of Hard X-ray Modulation Telescope (Insight-HXMT), Neutron Star Interior Composition Explorer (NICER) and AstroSat in 0.1-250 keV. The evolution of intensity, hardness and integrated fractional root mean square (rms) observed by Insight-HXMT and NICER are presented in this paper. Type-C quasi-periodic oscillations (QPOs) observed by NICER (0.8-3.5 Hz) and Insight-HXMT (1-1.6 Hz) are also reported in this work. The features of the QPOs are analysed with an energy range of 0.5-50 keV. The relations between QPO frequency and other characteristics such as intensity, hardness and QPO rms are carefully studied. The timing and spectral properties indicate that Swift J1658.2-4242 is a black hole binary system. Besides, the rms spectra of the source calculated from the simultaneous observation of Insight-HXMT, NICER and AstroSat support the Lense-Thirring origin of the QPOs. The relation between QPO phase lag and the centroid frequency * Corresponding author.Email addresses: xiaogc@ihep.ac.cn (Guangcheng Xiao), gemy@ihep.ac.cn (Mingyu Ge) of Swift J1658.2-4242 reveals a near zero constant when < 4 Hz and a soft phase lag at 6.68 Hz. This independence follows the same trend as the high inclination galactic black hole binaries such as MAXI J1659-152.

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INSIGHT-HXMT Observations of the New Black Hole Candidate MAXI J1535−571: Timing Analysis

Cited by 90 publications

References 48 publications

A systematic analysis of the phase lags associated with the type-C quasi-periodic oscillation in GRS 1915+105

A systematic analysis of the phase lags associated with the type-C quasi-periodic oscillation in GRS 1915+105

The braking index of PSR B0540−69 and the associated pulsar wind nebula emission after spin-down rate transition

Timing analysis of Swift J1658.2–4242's outburst in 2018 with Insight-HXMT, NICER and AstroSat

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