Origin of multiwavelength emission from flaring high redshift blazar PKS 0537-286

被引：7

作者：

Sahakyan, N. ^{[1
,2
,3
]}

Harutyunyan, G. ^{[1
,4
]}

Israyelyan, D. ^{[1
]}

机构：

[1] ICRANet Armenia, Marshall Baghramian Ave 24a, Yerevan 0019, Armenia

[2] ICRANet, Pzza Repubbl 10, I-65122 Pescara, Italy

[3] Sapienza Univ Roma, Dipartimento Fis, ICRA, Ple Aldo Moro 5, I-00185 Rome, Italy

[4] Byurakan Astrophys Observ, Byurakan 0213, Aragatsotn Reg, Armenia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 521卷 / 01期

关键词：

galaxies: active; galaxies: jets; quasars: individual: PKS 0537-286; gamma-rays: galaxies; GAMMA-RAY VARIABILITY; HIGH-ENERGY NEUTRINO; LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; BL-LAC OBJECTS; X-RAY; TXS 0506+056; FERMI-LAT; PARTICLE-ACCELERATION; LIGHT CURVES;

D O I：

10.1093/mnras/stad517

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The high redhsift blazars powered by supermassive black holes with masses exceeding 10(9) M-circle dot have the highest jet power and luminosity and are important probes to test the physics of relativistic jets at the early epochs of the Universe. We present a multifrequency spectral and temporal study of high redshift blazar PKS 0537-286 by analysing data from Fermi-LAT, NuSTAR Swift XRT, and UVOT. Although the time averaged gamma-ray spectrum of the source is relatively soft (indicating the high-energy emission peak is below the GeV range), several prominent flares were observed when the spectrum hardened and the luminosity increased above 10(49) erg s(-1). The X-ray emission of the source varies in different observations and is characterized by a hard spectrum <= 1.38 with a luminosity of >10(47) erg s(-1). The broad-band spectral energy distribution in the quiescent and flaring periods was modelled within a one-zone leptonic scenario assuming different locations of the emission region and considering both internal (synchrotron radiation) and external (from the disc, broad-line region, and dusty torus) photon fields for the inverse Compton scattering. The modelling shows that the most optimistic scenario, from the energy requirement point of view, is when the jet energy dissipation occurs within the broad-line region. The comparison of the model parameters obtained for the quiescent and flaring periods suggests that the flaring activities are most likely caused by the hardening of the emitting electron spectral index and shifting of the cut-off energy to higher values.

引用

页码：1013 / 1022

页数：10

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