Insight-HXMT Observations of Swift J0243.6+6124 during Its 2017–2018 Outburst

Zhang, Y.; Ge, M. Y.; Song, Liming; Zhang, Shuang‐Nan; Qu, J. L.; Zhang, Shu; Doroshenko, V.; Tao, Lian; Ji, Long; Güngör, Can; Santangelo, A.; Shi, Chang-Sheng; Chang, Zhi; Chen, Gang; Chen, Li; Chen, Tianxiang; Chen, Yong; Chen, Yibao; Cui, Wei; Cui, Weiwei; Deng, J. K.; Dong, Yongwei; Du, Yifeng; Fu, M. X.; Gao, G. H.; Gao, He; Gao, Min; Gu, Y. D.; Guan, J.; Guo, Chengcheng; Han, Danxiang; Hu, W.; Huang, Y.; Jia, Haiqiang; Jia, S. M.; Jiang, Luhua; Jiang, Weichun; Jin, Jing; Jin, Yongjie; Li, Bing; Li, Cheng-Kui; Li, Gang; Li, Mao-Shun; Li, Wei; Li, Xian; Li, Xiaobo; Li, Xufang; Li, Yanguo; Li, Zijian; Li, Zhengwei; Liang, X. H.; Liao, J. Y.; Liu, Cong‐Zhan; Liu, Guoqing; Liu, Hongwei; Liu, ShaoZhen; Liu, Xiaojing; Liu, Yuan; Liu, YiNong; Lü, Bo; Lu, X. F.; Luo, T.; Ma, Xiang; Meng, Bin; Nang, Y.; Nie, J. Y.; Ou, G.; Sai, N.; Sun, Liang; Tan, Ying; Tao, W. H.; Tuo, You-Li; Wang, Guofeng; Wang, Huan‐Yu; Wang, Juan; Wang, Wenshuai; Wang, Yusa; Wen, Xiang-Yang; Wu, B. Y.; Wu, Mei‐Hwan; Xiao, G. C.; Xiong, S. L.; Xu, He; Xu, Yupeng; Yan, Linyin; Yang, Jiawei; Yang, S.; Yang, Yanji; Zhang, Aimei; Zhang, Chunlei; Zhang, Chengmo; Zhang, Fan; Zhang, Hongmei; Zhang, Juan; Zhang, Tong; Zhang, Wei; Zhang, WanChang; Zhang, Wenzhao; Zhang, Yi; Zhang, Yifei; Yongjie, Zhang; Zhang, Zhao; Zhang, Ziliang; Zhao, H. S.; Zhao, Jianling; Zhao, Xiaofan; Zheng, S.; Zhu, Yajun; Zhu, Yuxuan; Zou, C. L.

doi:10.3847/1538-4357/ab22b1

Cited by 34 publications

(13 citation statements)

References 29 publications

(41 reference statements)

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“…There are several different reported values for the distance to this source in the literature: 2.5 ± 0.5 kpc (Bikmaev et al 2017) and ∼ 5 kpc (Reig et al 2020), both based on optical photometric observations, a lower limit of 5 kpc set by van den Eijnden et al (2018), ∼ 6 kpc based on two accretion torque models (Zhang et al 2019), and 5.5 +0.4 −0.3 kpc given in Gaia DR3 catalog (Gaia Collaboration et al 2016;. If the distance of the source is assumed for 5 kpc, its peak luminosity is estimated as 1 × 10 39 erg s −1 (0.1-10 keV).…”

Section: Introductionmentioning

confidence: 92%

Multiwavelength observations of Swift J0243.6+6124 from 2017 to 2022

Liu

Yan

Reig

et al. 2022

A&A

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Context. Swift J0243.6+6124 is a high-mass X-ray binary that went into a giant X-ray outburst in 2017. During this event, the X-ray luminosity reached the highest value ever measured in a galactic Be/X-ray binary. Aims. Our aim is to study the long-term variability of Swift J0243.6+6124 after the 2017 major X-ray outburst. Methods. We have obtained optical spectroscopy and photometry data during four years after the event. The long-term photometric light curve and the equivalent widths of the Hα and He I λ6678 lines were used to monitor the state of the Be star's circumstellar disk. The Hα line profiles show evidence for V / R variability that was accounted for by fitting the Hα spectral line profile with two Gaussian functions. We divided our data into three phases according to the intensity of the X-ray, optical, and infrared emission. Results. Phase I covers the rise and decay of the giant X-ray outburst that took place in October-November 2017. We interpret phase II as the dissipation of the Be star's equatorial disk and phase III as its recovery. The timescale of a complete formation and dissipation process is about 1250 days. The epoch when the dissipation process stopped and the reformation period began is estimated to be around MJD 58530. We find a delay of ∼ 100 -200 days between the minimum of the optical or infrared intensity and the strength of the Hα line after the X-ray outburst, which may indicate that the dissipation of the disk begins from the inner parts. The motion of the density perturbation inside the disk is prograde, with a V / R quasi-period of about four years. The source shows a positive correlation in the (B − V) color index versus V-band magnitude diagram, which implies that the system is seen at a small or moderate inclination angle. Conclusions. Despite the super-Eddington X-ray luminosity during the outburst, the subsequent pattern of long-term optical and IR variability of Swift J0243.6+6124 is typical of Be/X-ray binaries.

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Section: Introductionmentioning

confidence: 92%

Multiwavelength observations of Swift J0243.6+6124 from 2017 to 2022

Liu

Yan

Reig

et al. 2022

A&A

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“…Since the spectral characteristic varies over time, the long-term light curves of the sources of the three telescopes are different with each other. Swift J0243.6+6124 is an X-ray binary consisting of a neutron star and a Be star, and it had a strong outburst during 2017 to 2018 (Kouroubatzakis et al 2017;Zhang et al 2019). Insight-HXMT monitored the entire outburst completely and the longterm light curve in three energy ranges are shown in Figure 15 (a).…”

Section: Resultsmentioning

confidence: 99%

Methodology and performance of the two-year galactic plane scanning survey of Insight-HXMT

Sai

Liao

et al. 2020

Journal of High Energy Astrophysics

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The Galactic plane scanning survey is one of the main scientific objectives of the Hard X-ray Modulation Telescope (known as Insight-HXMT ). During the two-year operation of Insight-HXMT, more than 1000 scanning observations have been performed and the whole Galactic plane (0 • < l < 360 • , −10 • < b < 10 • ) has been covered completely. We summarize the Galactic plane scanning survey of Insight-HXMT for two years, including the characteristics of the scanning data, the data analysis process and the preliminary results of the Low-Energy telescope, the Medium-Energy telescope and the High-Energy telescope. With the light curve PSF fitting method, the fluxes of the known sources in the scanned area as well as the flux errors are obtained for each scanning observation. From the relationships of SNRs and fluxes, the 5σ sensitivities of three telescopes of Insight-HXMT are estimated as ∼ 7.6 × 10 −11 erg cm −2 s −1 (3 mCrab, 1 − 6 keV), ∼ 4.0 × 10 −10 erg cm −2 s −1 (20 mCrab, 7 − 40 keV) and ∼ 2.6 × 10 −10 erg cm −2 s −1 (18 mCrab, 25 − 100 keV) for an individual scanning observation of 2 − 3 hours, respectively. Up to September 2019, more than 800 X-ray sources with various types are monitored by the three telescopes and their long-term light curves with three energy bands are obtained to make further scientific analyses.

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“…The Insight-HXMT has launched in 2017 and LE works well since then. The on-orbit performance of LE meets the requirements of the design [2, 21,[23][24][25] and several science results [26][27][28][29] have already been obtained.…”

Section: Discussionmentioning

confidence: 99%

The Low Energy X-ray telescope (LE) onboard the Insight-HXMT astronomy satellite

Chen

Cui

et al. 2020

Sci. China Phys. Mech. Astron.

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The low energy (LE) X-ray telescope is one of the three main instruments of the Insight-Hard X-ray Modulation Telescope (Insight-HXMT). It is equipped with Swept Charge Device (SCD) sensor arrays with a total geometrical area of 384 cm 2 and an energy band from 0.7 keV to 13 keV. In order to evaluate the particle induced X-ray background and the cosmic X-ray background simultaneously, LE adopts collimators to define four types of Field Of Views (FOVs), i.e., 1.6° × 6°, 4° × 6°, 50~60 o × 2~6 o and the blocked ones which block the X-ray by an aluminum cover. LE is constituted of three detector boxes (LEDs) and an electric control box (LEB) and achieves a good energy resolution of 140 eV@5.9 keV, an excellent time resolution of 0.98 ms, as well as an extremely low pileup (<1%@18000 cts/s). Detailed performance tests and calibration on the ground have been performed, including energy-channel relation, energy response, detection efficiency and time response.

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Insight-HXMT Observations of Swift J0243.6+6124 during Its 2017–2018 Outburst

Cited by 34 publications

References 29 publications

Multiwavelength observations of Swift J0243.6+6124 from 2017 to 2022

Multiwavelength observations of Swift J0243.6+6124 from 2017 to 2022

Methodology and performance of the two-year galactic plane scanning survey of Insight-HXMT

The Low Energy X-ray telescope (LE) onboard the Insight-HXMT astronomy satellite

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