首页|Analysis of Bright Source Hardness Ratios in the 4yr Insight-HXMT Galactic Plane Scanning Survey Catalog

Analysis of Bright Source Hardness Ratios in the 4yr Insight-HXMT Galactic Plane Scanning Survey Catalog

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We conduct a statistical analysis of the hardness ratio(HR)for bright sources in the 4 yr Galactic Plane Scanning Survey catalog of Insight-HXMT.Depending on the stable(variable)flux Fs(Fv)or spectrum Ss(Sv)of each source,the bright sources are classified into three groups:Fv&Sv,Fv&Ss,and Fs&Ss.Our study of the HR characteristics in different types of sources reveals that accretion-powered neutron star(NS)low-mass X-ray binaries(LMXBs)exhibit softer energy spectra than NS high-mass X-ray binaries(HMXBs),but harder energy spectra than black hole binaries in most cases.This difference is probably due to their different magnetic field strengths.Additionally,Fv&Sv LMXBs tend to be harder than Fv&Ss LMXBs below 7 keV,while the opposite is true for HMXBs.Our results suggest that LMXBs may dominate unclassified sources,and NS binaries are likely to be the primary type of X-ray binaries with ambiguous compact stars.By comparing the HR of transient sources in their outburst and low-flux states,it is found that the averaged HR of four sources in the two states are roughly comparable within uncertainties.We also investigate the spatial properties of the three groups and find that Fv&Sv sources are mainly located in the longitude of-20°＜l＜9°,Fv&Ss sources cross the Galactic Plane,and Fs&Ss sources are predominantly concentrated in 19°＜l＜42°.In addition,analyzing the HR spatial distributions shows the absorption of soft X-rays(primarily below 2 keV)in the Galactic Plane.

catalogssurveysmethods:data analysisX-rays:general

Chen Wang、Jin-Yuan Liao、Ju Guan、Yuan Liu、Cheng-Kui Li、Na Sai、Jing Jin、Shuang-Nan Zhang

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Key Laboratory of Space Astronomy and Technology,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China

University of Chinese Academy of Sciences,Beijing 100049,China

Key Laboratory of Particle Astrophysics,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China

Department of Astronomy,School of Physics and Technology,Wuhan University,Wuhan 430072,China

WHU-NAOC Joint Center for Astronomy,Wuhan University,Wuhan 430072,China

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China National Space Administration(CNSA)中国科学院项目国家自然科学基金国家自然科学基金国家自然科学基金国家自然科学基金国家自然科学基金国家自然科学基金国家自然科学基金中国科学院青年创新促进会项目国家重点研发计划international partnership program of the Chinese Academy of Sciences

12333007U1838202U1838201U1838107U1838113U1838113U203810220180142021YFA0718500113111KYSB20190020

2024

10.1088/1674-4527/ad18a3

天文和天体物理学研究
中国科学院国家天文台

天文和天体物理学研究

CSTPCD
影响因子：0.406
ISSN：1674-4527
年,卷(期)：2024.24(2)
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