Long-term multi-wavelength study of temporal and spectral properties of 3C 279

Tolamatti, A.; Ghosal, B.; Singh, Krishna Kumar; Bhattacharyya, Subir; Bhatt, N.; Yadav, K. K.; Chandra, P.; Das, Mousumi; Tickoo, A. K.; Rannot, R. C.; Kothari, M.; Gaur, K.K.; Goyal, A.; Kumar, Naveen; Marandi, P.; Agarwal, Nikita; Godambe, S.; Mankuzhiyil, N.; Sarkar, Debdeep; Sharma, M.; Chouhan, N.; Borwankar, C.; Dhar, V. K.; Koul, M. K.; Venugopal, K.; Kotwal, S.; Godiyal, S.

doi:10.1016/j.astropartphys.2022.102687

Cited by 6 publications

(11 citation statements)

References 76 publications

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“…Our results in Table 1 indicate that a log-parabola model is enough to fit the spectra and no significant cut-off at GeV energies is observed during the flaring state, suggesting the dissipation region is outside the BLR and the energy dissipation may be due to the IC process of scattering the DT infrared photons. This result is consistent with the one suggested by Tolamatti et al (2022).…”

Section: The Location Of the Dissipation Regionsupporting

confidence: 94%

“…Shukla & Mannheim (2020) analyzed the minute timescale peak-in-peak variability and proposed that the particle acceleration is due to relativistic magnetic reconnection. However, the magnetic reconnection mechanism for the particle acceleration has been questioned for the reason of a low magnetization (Hu et al 2020(Hu et al , 2021Tolamatti et al 2022), and the shock-in-jet model for the particle acceleration is considered for the 2018 flare (Tolamatti et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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Variability and Spectral Behavior of Gamma-Ray Flares of 3C 279

Wang¹,

Fan²,

Xiao³

et al. 2022

PASP

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3C 279 showed enhanced flux variations in Fermi-LAT γ-ray observations from 2018 January to June. We present a detailed Fermi-LAT analysis to investigate the variability and spectral behaviors of 3C 279 during the γ-ray flares in 2018. In this work, we analyzed the γ-ray spectra and found that the spectra in either the flaring or quiescent states do not show any clear breaks (or cutoffs). This indicates that the dissipation region is outside the broad-line region, and the energy dissipation may be due to the inverse Compton process of scattering the dust torus infrared photons, this result is also consistent with that in Tolamatti et al. An external inverse Compton scattering of dusty torus (DT) photons is employed to calculate the broadband spectral energy distribution (SED). This model was further supported by the fact that we found flare decay timescale was consistent with the cooling time of relativistic electrons through DT photons. During the SED modeling, a relatively harder spectrum for the electron energy distribution is found and suggests these electrons may not be accelerated by the shock that happened in the dissipation region. Besides, the magnetic reconnection is also ruled out due to a low magnetization ratio. Thus, we suggest an injection of higher-energy electrons from outside the blob and raising the flare.

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Section: The Location Of the Dissipation Regionsupporting

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Variability and Spectral Behavior of Gamma-Ray Flares of 3C 279

Wang¹,

Fan²,

Xiao³

et al. 2022

PASP

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“…Based on the sharp peak profiles, we notice 4FGL J0303.4-2407 and 4FGL J0739.2+0137 show fast-rising and slowly decaying subflares. This asymmetry can be related to the particle acceleration mechanism in the jet, a fast rise could result from an effective particle acceleration at the shock front and slow decay may be interpreted as the weakening of the shock (Sokolov et al 2004;Tolamatti et al 2022) or from the injection of energetic particles on a shorter timescale than the cooling process timescales (Acharyya et al 2021). 4FGL J1751.5+0938 shows a slowly rising and fast-decaying subflare, which may be associated with an efficient cooling process.…”

Section: Connection With the Tev Bandmentioning

confidence: 99%

“…Based on these observations, significant progress has been made in blazar studies, e.g., the classification that depends on the synchrotron peak frequency (Abdo et al 2010a;Fan et al 2016;Yang et al 2022), the blazar sequence (Fan et al 2017;Ghisellini et al 2017;Ouyang et al 2023), and the blazar central engine (Paliya et al 2021;Xiao et al 2022a). More studies focus on individual sources, study the properties of flares or outbursts, and put constraints on the blazar emission mechanism, such as the flare of 3C 279 (Shukla & Mannheim 2020;Wang et al 2022a;Tolamatti et al 2022), the neutrino TXS 0506+056 (IceCube Collaboration et al 2018b), variability and spectral properties for 3C 279, Ton 599, and PKS 1222+216 (Adams et al 2022), and the light-curve study of PKS 1510+089 (Prince et al 2017) to obtain information on blazar emission variability, periodicity, and spectrum. Long-coverage observations on different timescales and spectral analysis can be carried out by taking advantage of the all-sky monitoring capabilities of Fermi-LAT.…”

Section: Introductionmentioning

confidence: 99%

GeV Variability Properties of TeV Blazars Detected by Fermi-LAT

Wang,

Xiao,

Fan

et al. 2024

ApJS

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Variability is a prominent observational feature of blazars. The high-energy radiation mechanism of jets has always been important but is still unclear. In this work, we performed a detailed analysis using Fermi-LAT data across 15 yr and obtained GeV light-curve information for 78 TeV blazars detected by Fermi. We provided annual GeV fluxes and corresponding spectral indices for the 78 TeV blazars and thorough monthly GeV fluxes for a subsample of 41 bright blazars. Our results suggest a strong correlation between the γ-ray photon index and log L γ for the flat spectrum radio quasars (FSRQs) and high-energy peaked BL Lacs. Fourteen sources in our sample show significant GeV outbursts/flares above the relatively stable, low-flux light curve, with six of them showing a clear sharp peak profile in their 5 day binned light curves. We quantified the variability utilizing the fractional variability parameter F var, and found that the flux of the FSRQs showed significantly stronger variability than that of the BL Lacs. The 41 bright blazars in this work are best fit by a log-normal flux distribution. We checked the spectral behavior and found 11 out of the 14 sources show a bluer-when-brighter trend, suggesting this spectral behavior for these TeV blazars at the GeV band arises from the mechanism in which the synchrotron-self Compton process dominates the GeV emission. Our research offers a systematic analysis of the GeV variability properties of TeV blazars and serves as a helpful resource for further associated blazar studies.

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“…The variability timescales shed lights on the emission size and even constrain the central black hole masses. Many TBLs are detected during their flare state of the γ-ray (Punch et al 1992;Quinn et al 1996;Catanese et al 1998;Chadwick et al 1999;Shukla & Mannheim 2020;Tolamatti et al 2022;Wang et al 2022). The variability in different wavelength can be used to investigate the emission mechanism.…”

Section: Luminosity Versus Luminositymentioning

confidence: 99%

Comparison Between TeV and Non-TeV Fermi-detected BL Lacertae Objects

Liang,

Zeng,

Chen

et al. 2023

PASP

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In this paper, we compiled a sample of 410 Fermi-detected BL Lacs, including 42 TeV-detected BL Lacs (TBLs) and 368 non-TeV-detected BL Lacs (non-TBLs) with corresponding mid-infrared (mid-IR), TeV and Fermi γ-ray data, and calculated some important parameters including monochromatic luminosities (mid-IR, GeV and TeV bands) and mid-IR spectral indices. Based on those parameters, we discussed the relationship between the mid-IR and the TeV bands and that between the mid-IR and the GeV bands. Main conclusions are drawn as follows: (1) In the color–color and color–magnitude diagrams, our sample forms a WISE-Gamma Strip in the [3.4]–[4.6]–[12] μm color–color diagram, and TBLs occupy the brighter region than the non-TBLs for the similar color-index in the color-magnititue diagram; (2) The mid-IR luminosity of the TBLs is on average higher than that of non-TBLs, while the average mid-IR spectral index of TBLs is smaller than the non-TBLs, suggesting that TBLs are brighter and hold a more flat spectrum than do the non-TBLs in the mid-IR band. Besides, HBLs have a more flat mid-IR spectrum than LBLs and IBLs; (3) The mid-IR luminosity is positively correlated with the GeV luminosity and the intrinsic TeV luminosity. A positive correlation exists between the mid-IR spectral index and the observed TeV spectral index, which is consistent with the expectations of the synchrotron self-Compton mechanism. We suggest that the HBLs with extreme relativistic electrons might scatter the mid-IR photons up to the TeV band.

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Long-term multi-wavelength study of temporal and spectral properties of 3C 279

Cited by 6 publications

References 76 publications

Variability and Spectral Behavior of Gamma-Ray Flares of 3C 279

Variability and Spectral Behavior of Gamma-Ray Flares of 3C 279

GeV Variability Properties of TeV Blazars Detected by Fermi-LAT

Comparison Between TeV and Non-TeV Fermi-detected BL Lacertae Objects

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