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

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

doi:10.1016/j.jheap.2020.02.005

Cited by 11 publications

(8 citation statements)

References 15 publications

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“…However, sometimes the LE data require extra selection, because the data at 1−6 keV band are vulnerable to contamination of particle events. The details are described in Sai et al (2020). The backgrounds of HE and ME are characterized by the fluctuations that come from the modulation of the geomagnetic field (Li et al 2009;Xie et al 2015), and a polynomial fit is sufficient enough to estimate them (Nang et al 2020).…”

Section: Data Reductionmentioning

confidence: 99%

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The Long-term Monitoring Results of Insight-HXMT in the First 4 yr Galactic Plane Scanning Survey

Wang

Liao

Guan

et al. 2023

ApJS

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The first X-ray source catalog of the Insight-HXMT Galactic Plane (∣b∣ < 10°) Scanning Survey (GPSS) is presented based on the data accumulated from 2017 June to 2021 August. The 4 yr limit sensitivities at main energy bands can reach 8.2 × 10−12 erg s−1 cm2 (2−6 keV), 4.21 × 10−11 erg s−1 cm2 (7−40 keV), and 2.78 × 10−11 erg s−1 cm2 (25−100 keV). More than 1300 sources have been monitored at a wide band (1−100 keV), of which 223 sources have a signal-to-noise ratio greater than 5. We combined the GPSS data of Insight-HXMT and MAXI and found it feasible to obtain more complete long-term light curves from their scanning results. The flux variabilities at different energy bands of the 223 bright sources are analyzed based on the excess variances. It is found that the fluxes of X-ray binaries are more active than those of supernova remnants and isolated pulsars. Different types of binaries, e.g., low-mass X-ray binaries (LMXBs), high-mass X-ray binaries (HMXBs), neutron star binaries, and black hole binaries, also distinctively show different regularities. In addition, the relations between the hardness ratio (HR) and excess variances, and HR and source types are analyzed. It is obvious that the HRs of HMXBs tend to be harder than those of LMXBs and HMXBs tend to be more active than those of LMXBs.

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Section: Data Reductionmentioning

confidence: 99%

“…After the scanning data are screened, we fit the corresponding light curves with steps 3−7 illustrated in Figure 4. The details are described in Sai et al (2020), and we outline the processes as follows: 3. Distinguish bright and faint sources based on the fluxes and signal-to-noise ratios (S/N).…”

Section: Light-curve Fittingmentioning

confidence: 99%

The Long-term Monitoring Results of Insight-HXMT in the First 4 yr Galactic Plane Scanning Survey

Wang

Liao

Guan

et al. 2023

ApJS

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“…The three light curves for the three boxes will then be fitted jointly. The analysis process of the Insight-HXMTʼs scanning data has the following three main steps, and the details are described in Sai et al (2020).…”

Section: Data Reduction and Basic Analysis Of The Scanning Observationmentioning

confidence: 99%

“…Before the end of 2019 April, the whole Galactic plane was divided into 22 scanned areas with a radius of 10°. For each scanned area, the progressive-scanning mode (Sai et al 2020) is performed with a scanning speed of 0°.06 s −1 and a scanning interval (the angular distance between two adjacent scanning rows) of 0°.8. From the end of 2019 April to now, in order to scan more densely while the duration of one scanning observation is not changed much, the whole Galactic plane is redivided into 50 scanned areas with a radius of 7°, and the scanning interval is changed to 0°.4.…”

Section: Introductionmentioning

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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“…For gamma-ray burst observation, the background is usually taken from preand post-burst (Luo et al, 2020). For scanning observation, the background is derived from the scanning light curves with sources subtracted (Sai et al, 2020). However, the background estimation of the pointing observation is much more complicated, since the traditional on-off mode of BeppoSAX /PDS (Frontera et al, 1997a,b) and RXTE /HEXTE (Rothschild et al, 1998) for observation of the background was not adopted in the design of Insight-HXMT.…”

Section: Introductionmentioning

confidence: 99%

Five-year in-orbit background of Insight-HXMT

Liao¹,

Zhang²,

Zhang³

et al. 2023

Preprint

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We present the five-year in-orbit background evolution of Insight-HXMT since the launch, as well as the effects of the background model in data analysis. Methods: The backgrounds of the three main payloads, i.e., Low-Energy Telescope, Medium-Energy Telescope and High-Energy Telescope, are described, respectively. The evolution of the background over time is obtained by simply comparing the background in every year during the in-orbit operation of Insight-HXMT. Results: The major observational characteristics of the Insight-HXMT in-orbit background are presented, including the

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

Cited by 11 publications

References 15 publications

The Long-term Monitoring Results of Insight-HXMT in the First 4 yr Galactic Plane Scanning Survey

The Long-term Monitoring Results of Insight-HXMT in the First 4 yr Galactic Plane Scanning Survey

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

Five-year in-orbit background of Insight-HXMT

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