FLARE-LIKE VARIABILITY OF THE Mg II λ2800 EMISSION LINE IN THE γ-RAY BLAZAR 3C 454.3

Chavushyan, V.; Patiño-Álvarez, V.; Valtaoja, E.; Arshakian, T. G.; Tornikoski, M.; Lobanov, A. P.; Carramiñana, A.; Carrasco, L.; Lähteenmäki, A.

doi:10.1088/2041-8205/763/2/l36

Cited by 93 publications

(110 citation statements)

References 45 publications

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“…In the case of 3C 454.3, a powerful γ-ray FSRQ, a significant increase of the broad Mg II λ2798 has been reported in response to γ-ray flaring activity, suggesting a close spatial connection [41]. Some rest frame optical lines like Hβ and Hγ, though variable, are consistent with longer time scales with respect to the characteristic flaring time [42].…”

Section: Optical Spectra From Agns With Jetsmentioning

confidence: 85%

“…Variability of emission lines, corresponding to γ-ray flaring activity and ejection of super-luminal components from radio cores has been reported, suggesting that the non-thermal radiation of the jet might contribute to the ionization of the BLR or even produce a BLR-like structure at large distances from the AGN centre [41]. A more extensive investigation of the broad lines, however, indicates that the contribution can at most only partially account for the observed line fluxes, which still are affected by the thermal ionizing radiation of the accretion field [42].…”

Section: Discussionmentioning

confidence: 99%

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Relativistic plasmas in AGN jets

et al. 2017

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Abstract. Relativistic jets of plasma are a key ingredient of many types of Active Galactic Nuclei (AGN). Today we know that AGNs are powered by the accretion of inter stellar material into the gravitational field of a Super Massive Black Hole and that this process can release as much power as a whole galaxy, like the Milky Way, from a region that is comparable to the Solar System in size. Depending on the properties of the central energy source, a large fraction of this power can be involved in the acceleration of magnetized plasmas at relativistic speeds, to form large scale jets. The presence of jets affects the spectrum of AGNs through the emission of synchrotron radiation and Inverse Compton scattering of low energy photons, thus leading to a prominent non-thermal spectrum, some times extending from radio frequencies all the way up to γ-ray energies. Here we review some characteristic processes of radiation emission in AGN jets, which lead to the emission of photons in the radio, optical, X-ray and γ-ray bands, and we present the results of a spectroscopic campaign of optical counterparts. We discuss our observations and their connection with γ-ray properties in a scenario that traces the role of relativistic jets in different classes of AGNs, detected both in the local as well as in the remote Universe.PACS. 52.25.Os Emission, absorption and scattering of electromagnetic radiation -52.27.Ny Relativistic plasmas -98.54.Cm Active and peculiar galaxies and related systems (including BL Lacertae objects, blazars, Seyfert galaxies, Markarian galaxies, and active galactic nuclei) -98.70.Rz γ-ray sources; γ-ray bursts

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Section: Optical Spectra From Agns With Jetsmentioning

confidence: 85%

Section: Discussionmentioning

confidence: 99%

Relativistic plasmas in AGN jets

et al. 2017

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“…Relatively slow sections of the jet, e.g., a Mach disk, might provide ample seed photons, but the SEDs are better fit by a thermal spectrum of seed photons. One possible solution, supported by reported variations in emission lines from 3C 454.3 during its late-2010 mega-outburst [31,45], is that stray broad emission-line clouds are located near the parsec-scale jet and are illuminated by beamed UV photons from the jet. This could provide a variable source of seed photons (as the Mach disk does in the TEMZ model), thus affecting the γ-ray variations.…”

Section: Discussionmentioning

confidence: 99%

Multi-waveband Behavior of Blazars

Marscher

2013

EPJ Web of Conferences

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Abstract. The author reviews recent progress toward understanding blazars that multi-waveband monitoring observations have advanced. The primary techniques include the compilation of multi-waveband light curves, multi-epoch VLBI images at radio wavelengths, plots of linear polarization vs. time at radio through optical wavelengths, and spectral energy distributions (SEDs). Correlations and the coincidence or lag of events across wavebands and in the images indicate where the events take place relative to the "core" that lies 0.5 pc from the central engine. Rotations of the polarization electric vector suggest a helical geometry of the magnetic field upstream of the millimeter-wave core, while rapid fluctuations in degree and position angle of polarization imply that the jet plasma is turbulent in and downstream of the core. The author is developing a numerical model that simulates the emission from such turbulence as it interacts with a conical standing shock in the core region.

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“…At the same time, it is important to realize that these three conventional sources might not be the complete answer to the question of correlation between γ-ray and radio events at pc scales that we are currently facing. In that case, tinkering with the possibility of new sources of seed photon fields or getting creative with the existing ones [see, e.g., 17,18,20] should be and needs to be explored. In addition to the position of the emission region along the jet axis, another factor that plays an important role in deciding the range of the location of γ-ray emission is the duration over which the shocks stay inside the system.…”

Section: Discussionmentioning

confidence: 99%

Constraining the location of gamma-ray emission in blazar jets

Joshi

Marscher

Böttcher

2013

EPJ Web of Conferences

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Abstract.The location of γ-ray emission in blazar jets has remained elusive as wetry to understand jet emission despite the extensive multiwavelength campaigns and vigorous theoretical efforts to understand the multiwavelength spectra. The synergy between multiwavelength campaigns and VLBA studies has resulted in correlation between the majority of γ-ray events and disturbances propagating down the parsec-scale jet. This implies that the γ-ray emission might originate beyond the broad line region (BLR), perhaps on scales comparable to the size of the dusty torus. On the other hand, external Compton models in which γ-ray emission is limited to sites inside the BLR have been used to explain the high-energy emission of many blazars. Thus, comprehending the time-dependent impact of all the three external components of seed photon field, namely the accretion disk, the BLR, and the dusty torus, on the evolution of the spectral energy distribution (SED) can be used as an important tool for connecting the origin of γ-ray emission of a flare to its multiwavelength properties. Here, we use a multi-zone time-dependent leptonic jet model, with radiation feedback, to address this aspect of blazar jet emission. We let the system evolve to beyond the BLR and within the dusty torus. We explore the effects of varying the contribution of the disk, the BLR, and the dusty torus on the resultant seed photon field and their manifestation on the simulated SED of a typical blazar to gain insight on the location of the γ-ray emission region.

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FLARE-LIKE VARIABILITY OF THE Mg II λ2800 EMISSION LINE IN THE γ-RAY BLAZAR 3C 454.3

Cited by 93 publications

References 45 publications

Relativistic plasmas in AGN jets

Relativistic plasmas in AGN jets

Multi-waveband Behavior of Blazars

Constraining the location of gamma-ray emission in blazar jets

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