首页|Probing the Gamma-Ray Emission Region of Five TeV Flat Spectrum Radio Quasars

Probing the Gamma-Ray Emission Region of Five TeV Flat Spectrum Radio Quasars

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The location of γ-ray emission of blazars remains a contested topic,inspiring the development of numerous investigative techniques to address this issue.In this work,we analyzed Fermi γ-ray light curves in the GeV and MeV bands,employing the discrete cross-correlation function method to discern time lags between the two bands.For 4C+21.35,Ton 599,B2 1420+32,and PKS 1510-089,we identified a time lag spanning several days,while for PKS 1441+25,the time lag was not statistically found.The results imply that the soft photons necessary for inverse Compton scattering predominantly originate from the dusty torus in the first four sources,whereas for PKS 1441+25,they seem to be sourced mainly from the broad-line region.Further analysis of the opacity(τγγ)and the GeV spectra study supports the conclusion that the location of the dissipation region must be beyond the BLR to avoid significant absorption.Notably,for PKS 1441+25,the emission region is also posited to lie outside yet proximate to the BLR.The parameters of describing the emission region were obtained by fitting broadband spectral energy distribution with contemporaneous observation data.Our findings suggest that for the five TeV FSRQs,during TeV flaring events,the jet appears to maintain an equilibrium between the energy density of the magnetic field and that of the particles for all investigated sources,with the exceptions of 4C+21.35 and PKS 1441+25.In terms of the overall jet power,particle energy is the dominant contributor,and the observed blazar radiation cannot be solely attributed to the magnetic field,except in the case of 4C+21.35.Consequently,magnetic reconnection is unlikely to be the primary mechanism behind particle acceleration in these systems.

galaxies:activegamma-rays:galaxiesgalaxies:jets

Hu-Bing Xiao、Hai-Tao Cao、Rui Xue、Jin-Ting Cai、Ge-Ge Wang、Marina Manganaro、Shao-Hua Zhang、Zhi-Hao Ouyang、Li-Ping Fu、Jun-Hui Fan

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Shanghai Key Lab for Astrophysics,Shanghai Normal University,Shanghai 200234,China

School of Information Engineering,Guangzhou Panyu Polytechnic,Guangzhou 511483,China

Department of Physics,Zhejiang Normal University,Jinhua 321004,China

College of Mathematics and Physics,Guangxi Minzu University,Nanning 530006,China

Key Laboratory of Cosmology and Astrophysics(Liaoning),College of Sciences,Northeastern University,Shenyang 110819,China

Department of Physics,University of Rijeka,Rijeka 51000,Croatia

Center for Astrophysics,Guangzhou University,Guangzhou 510006,China

Key Laboratory for Astronomical Observation and Technology of Guangzhou,Guangzhou 510006,China

Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province,Guangzhou 510006,China

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National Natural Science Foundation of China(NSFC)Shanghai Science and Technology Fundscience research grants from the China Manned Space ProjectNational Natural Science Foundation of China(NSFC)National Natural Science Foundation of China(NSFC)National Natural Science Foundation of China(NSFC)National Key Research and Development Program of ChinaShanghai Science and Technology FundProgram for Professor of Special Appointment(Eastern Scholar)at Shanghai Institutions of Higher Learningthe Shuguang ProgramShanghai Education Development Foundation and Shanghai Municipal Education CommissionNational Natural Science Foundation of China(NSFC)National Natural Science Foundation of China(NSFC)Scientific and Technological Cooperation ProjectsPeople's Republic of ChinaRepublic of Bulgaria,the science research grants from the China Manned Space ProjectBulgarian National Science Fund of the Ministry of Education and ScienceBulgarian National Science Fund of the Ministry of Education and ScienceBulgarian National Science Fund of the Ministry of Education and Science

1220303422YF14315001220304311933002121730262022YFC28073032301050390023SG39U20312011173300120202023CMS-CSST-2021-A06KP-06-H38/42019KP-06-KITAJ/22020KP-06-H68/42022

2024

10.1088/1674-4527/ad420e

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(6)