Jet Radiation Properties of 4C +49.22: from the Core to Large-scale Knots

Zhang, Jin; Zhang, Haiming; Yao, Shujie; Guo, Sheng-Chu; Lu, Rui-Jing; Liang, En‐Wei

doi:10.3847/1538-4357/aadd0b

Cited by 5 publications

(4 citation statements)

References 72 publications

(148 reference statements)

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“…As given in Tables 3 and 4, P e jet  of the core is within 3 × 10 42 -10 44 erg s −1 while P e jet  of extended regions are in the range of ∼10 43 -10 44 erg s −1 . It is found that the jet powers of the core and extended regions for the three CSOs are roughly of the same order, and similar results have been reported for a γ-ray-emitting RG 3C 120 (Zargaryan et al 2017) and a blazar 4C +49.22 (Zhang et al 2018). We also estimate the kinetic power (P kin ) of the three CSOs with the radio luminosity at 1.4 GHz of extended regions using Equation (1) in Cavagnolo et al (2010) and obtain 1.4 × 10 44 erg s −1 , 3.0 × 10 42 erg s −1 and 7.3 × 10 43 erg s −1 for PKS 1718-649, NGC 3894 and TXS 0128+554, respectively.…”

Section: Broadband Sed Modeling and γ-Ray Originsupporting

confidence: 80%

Lobe-dominated γ-Ray Emission of Compact Symmetric Objects

Gan,

Zhang,

Yang

et al. 2024

Res. Astron. Astrophys.

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The $\gamma$-ray emitting compact symmetric objects (CSOs) PKS 1718--649, NGC 3894, and TXS 0128+554 are lobe-dominated in the radio emission. In order to investigate their $\gamma$-ray radiation properties, we analyze the $\sim$14-yr Fermi/LAT observation data of the three CSOs. They all show the low luminosity ($10^{41}-10^{43}$ erg s$^{-1}$) and no significant variability in the $\gamma$-ray band. Their $\gamma$-ray average spectra can be well fitted by a power-law function. These properties of $\gamma$-rays are clearly different from the $\gamma$-ray emitting CSOs CTD 135 and PKS 1413+135, for which the $\gamma$-rays are produced by a restarted aligned jet. In the $L_{\gamma}-\Gamma_{\gamma}$ plane, the three CSOs are also located at the region occupied by radio galaxies (RGs) while CTD 135 and PKS 1413+135 display the similar feature to blazars. Together with the similar radio emission property to $\gamma$-ray emitting RGs Cen A and Fornax A, we speculate that the $\gamma$-rays of the three CSOs stem from their extended mini-lobes. The broadband spectral energy distributions of the three CSOs can be well explained by the two-zone leptonic model, where their $\gamma$-rays are produced by the inverse Compton process of the relativistic electrons in extended region. By extrapolating the observed Fermi/LAT spectra to the very high energy band, we find that TXS 0128+554 among the three CSOs may be detected by the Cherenkov Telescope Array in future.

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Section: Broadband Sed Modeling and γ-Ray Originsupporting

confidence: 80%

Lobe-dominated γ-Ray Emission of Compact Symmetric Objects

Gan,

Zhang,

Yang

et al. 2024

Res. Astron. Astrophys.

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“…The time lag of optical V band to γ-ray can be explained by lepton synchrotron-self Compton (LSSC) model. However, there are two tentative radiation models to produce the γ-ray flux, i.e., lepton SSC model (Zhou et al 2014) and proton synchrotron model (Zhang et al 2012(Zhang et al , 2013(Zhang et al , 2018Gao et al 2018) for 3FGL J0449.4−4350. The strong correlations of the two different wavelength band of this source support the LSSC model.…”

Section: Summary and Discussionmentioning

confidence: 99%

The γ-Ray and Optical Variability Analysis of the BL Lac Object 3FGL J0449.4−4350

Yang

Zhang

et al. 2020

PASP

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We have assembled the historical light curves of the BL Lac Object 3FGL J0449.4-4350 at optical and γ-ray bands, the time spanning about 10 years, analyzed the periodic variability of the light curves by using four different methods (Lomb-Scargle periodogram, REDFIT38, Jurkevich and DACF). We detected a marginally possible quasi-periodic oscillation (QPO) of ∼ 450 days. Assuming it originates from the helical motion jet in a supermassive binary black hole (SMBBH) system undergoing major merger, we estimate the primary black hole mass M ∼ 7.7 × 10 9 M . To explore the origin of the γ-ray, we investigated the optical-γ-ray correlations using discrete correlation function (DCF) method, and found that the correlation between the two bands is very significant. This strong correlation tends to imply lepton self-synchro-Compton (LSSC) model to produce the γ-ray.

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“…The consistency between the X-ray spectrum and the extrapolation of the radio-optical synchrotron emission indicates the same synchrotron radiation origin of X-ray emission (Sambruna et al 2007;Zhang et al 2010Zhang et al , 2018b. But for most substructures, the hard spectra in the X-ray band require a new radiation component different from the low energy band, and then the inverse Compton (IC) scattering process is suggested to explain the X-ray emission (e.g., Kataoka & Stawarz 2005;Zhang et al 2010Zhang et al , 2018b, i.e., the synchrotron-self-Compton (SSC, Stawarz et al 2007) model and the IC scattering of the cosmic microwave background (IC/CMB, Georganopoulos & Kazanas 2003;Abdo et al 2010;McKeough et al 2016;Wu et al 2017;Zhang et al 2018a;Guo et al 2018) model. The X-ray emission may be produced by the synchrotron radiation of the second electron population different from the radio-optical emission (e.g., Zhang et al 2009;Zargaryan et al 2017;Sun et al 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Comparing with the variability of the core radiation, the emission of substructures in large-scale jets almost does not show any variation, which is also used to estimate the origin of the γ-ray emission (e.g.,Zhang et al 2018a;Guo et al 2018;Meyer et al 2019). …”

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confidence: 99%

Leptonic or Hadronic Emission: The X-Ray Radiation Mechanism of Large-scale Jet Knots in 3C 273

Wang

Zhang

Sun

et al. 2020

ApJ

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A comprehensively theoretical analysis on the broadband spectral energy distributions (SEDs) of large-scale jet knots in 3C 273 is presented for revealing their X-ray radiation mechanism. We show that these SEDs cannot be explained with a single electron population model when the Doppler boosting effect is either considered or not. By adding a more energetic electron (the leptonic model) or proton (the hadronic model) population, the SEDs of all knots are well represented. In the leptonic model, the electron population that contributes the X-ray emission is more energetic than the one responsible for the radio-optical emission by almost two orders of magnitude; the derived equipartition magnetic field strengths (B eq ) are ∼ 0.1 mG. In the hadronic model, the protons with energy of ∼ 20 PeV are required to interpret the observed X-rays; the B eq values are several mG, larger than that in the leptonic model. Based on the fact that no resolved substructures are observed in these knots and the fast cooling-time of the high-energy electrons is difficult to explain the observed X-ray morphologies, we argue that two distinct electron populations accelerated in these knots are unreasonable and their X-ray emission would be attributed to the proton synchrotron radiation accelerated in these knots. In case of these knots have relativistic motion towards the observer, the super-Eddington issue of the hadronic model could be avoided. Multiwavelength polarimetry and the γ-ray observations with high resolution may be helpful to discriminate these models.In this scenario, the synchrotron, SSC, and IC/CMB radiations of a single electron population are used to reproduce the broadband SEDs of knots. The radiating electrons are assumed to have the number distribution as Equation (1). The minimum and maximum energies of electrons are taken as E e,min =1 MeV and E e,max =510 TeV, which are respectively corresponding to γ e ∼ 2 and γ e ∼ 10 9 , where γ e is the Lorenz factor of electrons. In case of the knots do not have the relativistic motions, i.e., δ = Γ = 1, the IC component would be dominated by the SSC process since the energy density of the synchrotron radiation photon field (U syn ) is higher than U ′ CMB . A magnetic field strength (B) lower than the equipartition value (B eq ) is also needed (e.g.

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Jet Radiation Properties of 4C +49.22: from the Core to Large-scale Knots

Cited by 5 publications

References 72 publications

Lobe-dominated γ-Ray Emission of Compact Symmetric Objects

Lobe-dominated γ-Ray Emission of Compact Symmetric Objects

The γ-Ray and Optical Variability Analysis of the BL Lac Object 3FGL J0449.4−4350

Leptonic or Hadronic Emission: The X-Ray Radiation Mechanism of Large-scale Jet Knots in 3C 273

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