In-orbit calibration to the point-spread function of Insight-HXMT

Nang, Y.; Liao, J. Y.; Sai, N.; Wang, Chen; Guan, J.; Li, Cheng-Kui; Guo, Chengcheng; Liu, Yuan; Jin, Jing; Li, Xiaobo; Zhang, Shu; Zhang, Shuang‐Nan

doi:10.1016/j.jheap.2020.01.002

Cited by 15 publications

(13 citation statements)

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“…Insight-HXMT monitored the entire outburst completely and the longterm light curve in three energy ranges are shown in Figure 15 (a). In addition to Swift 0243+6124, the longterm light curve of Vela X-1 (HMXB/NS), GX 349+2 (LMXB/NS), Cyg X-1 (HMXB/BH) are also shown in Figure 15 From Nang et al (2020), the systematic errors in flux estimation are 1.8%, 1.6% and 2.7% for LE, ME and HE (Table 4), which may be caused by various factors, such as the small uncertainty of the Energy-Channel relation and the weak long-term evolution of the PSF. As the spectral characteristic of the Crab is generally stable, the long-term light curves of the Crab can be used to obtain the systematic errors of the estimated flux of the scanning observations.…”

Section: Resultsmentioning

confidence: 99%

“…From Nang et al (2020), the systematic errors in flux estimation are 1.8%, 1.6% and 2.7% for LE, ME and HE (Table 4), which may be caused by various factors, such as the small uncertainty of the Energy-Channel relation and the weak long-term evolution of the PSF. As the spectral characteristic of the Crab is generally stable, the long-term light curves of the Crab can be used to obtain the systematic errors of the estimated flux of the scanning observations.…”

Section: Resultsmentioning

confidence: 99%

“…All the collimators of the three telescopes have rectangular FOVs (Figure 1) with different sizes of FOV and orientations, and can be described by the geometric PSF model as equation 1. The in-orbit calibration of the geometrical PSF with rotation correction and parabolic correction are performed by Nang et al (2020), and the light curve fitting is done with the calibrated PSF in order to obtain more accurate analysis results.…”

Section: As Shown Inmentioning

confidence: 99%

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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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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: As Shown Inmentioning

confidence: 99%

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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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“…Instead of calibrating the FOV of each detector, the FOV of a whole box is calibrated. The details of the PSF and the effective area calibration are presented in Nang et al (2020) and , respectively. Because the FOV orientations of the three boxes are different, the light curves of the three boxes will be different and will be generated separately.…”

Section: Data Reduction and Basic Analysis Of The Scanning Observationmentioning

confidence: 99%

The Diffuse X-Ray Background of the Insight-HXMT/LE Telescope in the Galactic Plane

Jin

Liao

Wang

et al. 2022

ApJS

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Accurately estimating of diffuse X-ray background (DXB) is essential for the investigation of sources in the Galactic plane observed with Insight-HXMT/LE, which is a collimated telescope in the soft X-ray energy band with a relatively large field of view. In the high-Galactic-latitude region, DXB is dominated by the cosmic X-ray background, which is almost uniform, but DXB in the Galactic plane region is more complex due to the Galactic H i absorption and the contribution of the Galactic ridge X-ray emission. This study, as a part of background estimation of LE, focuses on estimating the contribution of DXB in the Galactic plane to Insight-HXMT/LE observations. We calculate DXB confined in a region of 0° < l < 360° and ∣b∣ < 10°, where l and b denote Galactic longitude and latitude, respectively, with the first 3 yr of Galactic-plane-scanning survey data of Insight-HXMT/LE. The Galactic plane is divided into 360 × 20 small pixels (1° × 1° per pixel), and a DXB spectrum is obtained for each pixel. An indirect method is developed for the pixels of the bright source regions, which brings a systematic error of ∼10%. The systematic error brought by the satellite attitude is ∼7% on average for all the pixels in the Galactic plane. The LE DXB spectrum obtained in this study is consistent with that reported by RXTE’s Proportional Counter Array.

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“…Section 6 describes the systematic errors of the three instruments onboard Insight-HXMT which can be used in the spectral fitting. The response of the collimators, or the Point Spread Function (PSF) of Insight-HXMT is described else where [7]. The absolute timing accuracy of Insight-HXMT is about 50 us from the time of arrival (TOA) of the Crab Pulsar compared with observations of other telescopes, which has also been described else where [8].…”

Section: Introductionmentioning

confidence: 99%

In-flight calibration of the Insight-Hard X-ray Modulation Telescope

Tan

Yang

et al. 2020

Preprint

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We present the calibration of the Insight-Hard X-ray Modulation Telescope (Insight-HXMT) X-ray satellite, which can be used to perform timing and spectral studies of bright X-ray sources. Insight-HXMT carries three main payloads onboard: the High Energy X-ray telescope (HE), the Medium Energy X-ray telescope (ME) and the low Energy X-ray telescope (LE). In orbit, the radioactive sources, activated lines, the fluorescence lines and celestial sources are used to calibrate the energy scale and energy resolution of the payloads. The Crab nebular is adopted as the primary effective area calibrator and empirical functions are constructed to modify the simulated effective areas of the three payloads respectively. The systematic errors of HE, compared to the model of the Crab nebular, are less than 2% in 28-120 keV and 2%-10% above 120 keV. The systematic errors of ME are less than 1.5% in 10-35 keV. The systematic errors of LE are less than 1% in 1-7 keV except the Si K-edge (1.839 keV, up to 1.5%) and less than 2% in 7-10 keV.

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In-orbit calibration to the point-spread function of Insight-HXMT

Cited by 15 publications

References 10 publications

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

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

The Diffuse X-Ray Background of the Insight-HXMT/LE Telescope in the Galactic Plane

In-flight calibration of the Insight-Hard X-ray Modulation Telescope

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