Relativistic Plasma as the Dominant Source of the Optical Continuum Emission in the Broad-Line Radio Galaxy 3c 120

Leon-Tavares, J.; Lobanov, A. P.; Chavushyan, V.; Arshakian, T. G.; Doroshenko, V. T.; Сергеев, С. Г.; Efimov, Yu. S.; Назаров, С. В.

doi:10.1088/0004-637x/715/1/355

Cited by 48 publications

(59 citation statements)

References 36 publications

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“…Arshakian et al (2010) found a connection between the variable optical continuum and the subparsecscale jet in 3C 390.3, in addition to a significant correlation (at a confidence level of >99.99%) between the ejected jet components and optical continuum flares and that radio events follow the maxima of optical flares with the mean time delay around ∼36 days. Results obtained in León-Tavares et al (2010) for the broad-line radio galaxy 3C 120, confirm the correlations found in Arshakian et al (2010) and support the idea that the correlation between optical flares and kinematics of the jet may be common to all radio-loud galaxies and quasars. There is therefore, an open question about the origin of QPOs in 3C 390.3.…”

Section: Continuum and Line Light Curves: Possible Quasi-periodical Osupporting

confidence: 77%

Spectral optical monitoring of 3C 390.3 in 1995–2007

Shapovalova¹,

Popovic²,

Буренков³

et al. 2010

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Context. We present the results of the long-term (1995)(1996)(1997)(1998)(1999)(2000)(2001)(2002)(2003)(2004)(2005)(2006)(2007) spectral monitoring of the broad-line radio galaxy 3C 390.3, a well known AGN with double-peaked broad emission lines, usually assumed to be emitted from an accretion disk. Aims. To explore dimensions and structure of the BLR, we analyze the light curves of the broad Hα and Hβ line fluxes and the continuum flux. To detect variations in the BLR, we analyze the Hα and Hβ line profiles, as well as the change in the line profiles during the monitoring period. Methods. We attempt first to find a periodicity in the continuum and Hβ light curves, finding that there is a high probability of measuring quasi-periodical oscillations. Using the line shapes and their characteristics (such as e.g., peak separation and their intensity ratio, or FWHM) of broad Hβ and Hα lines, we discuss the structure of the BLR. We also cross-correlate the continuum flux with Hβ and Hα lines to determine the dimensions of the BLR. Results. During the monitoring period, we found that the broad emission component of the Hα and Hβ lines, and the continuum flux varied by a factor of ≈4−5. We also detected different structure in the line profiles of Hα and Hβ. An additional central component appears to be present and superimposed on the disk emission. In the period of high activity (after 2002), Hβ became broader than Hα and red wing of Hβ was higher than that of Hα. We detected time lags of ∼95 days between the continuum and Hβ flux, and about 120 days between the continuum and Hα flux. Conclusions. Variations in the line profiles, as well as correlation between the line and continuum flux during the monitoring period, are consistent with a disk origin of the broad lines and the possible contribution of some additional region and/or some kind of perturbation in the disk.

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Section: Continuum and Line Light Curves: Possible Quasi-periodical Osupporting

confidence: 77%

Spectral optical monitoring of 3C 390.3 in 1995–2007

Shapovalova¹,

Popovic²,

Буренков³

et al. 2010

A&A

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“…In particular, in the jets of γ-ray blazars, observed at 22 and 43 GHz, stationary features within a distance of 2 pc (projected) from the core are commonly observed (Jorstad et al 2001). Stationary jet features were previously investigated in more detail in the cases of 3C 390.3 (Arshakian et al 2010), a nearby double-peaked radio galaxy at z = 0.0561, and the Seyfert galaxy 3C 120 (z = 0.033; León-Tavares et al 2010). For these two sources, stationary features were found at distances of ∼0.4 pc (3C 390.3) and ∼1.3 pc (3C 120) from the core at 15 GHz.…”

Section: Discussionmentioning

confidence: 99%

Relativistic outflow drivesγ-ray emission in 3C 345

Schinzel

Lobanov

Taylor

et al. 2012

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Aims. On the basis of the first 20 months of Fermi-LAT data and optical monitoring, the quasar 3C 345 has been identified as a γ-ray emitter. We investigate whether there is a connection between the γ-ray and optical variability of 3C 345 and the properties of its parsec-scale radio emission. Methods. We combined the Fermi-LAT data of 3C 345, covering an energy range of 0.1-300 GeV, with 32 Very Long Baseline Array observations of the object made at 43.2 GHz in the period of January 2008-March 2010.Results. The VLBA data reveal the morphology and kinematics of the flow on scales of up to ≈5 milliarcseconds (deprojected linear distances of 380 parsecs). The brightness temperature, T b (r), measured along the jet first decreases with distance ∝r −(0.95 ± 0.69) and later exhibits a break at ≈0.3 milliarcseconds (mas), with T b (r) ∝ r −(4.11 ± 0.85) at larger separations. Variations in the γ-ray, optical, and parsec-scale radio emission display a similar long-term trend that persists during the entire VLBA monitoring period. The γ-ray and optical variations on shorter timescales are related to structural changes in the jet on scales of ≈0.3 mas (≈23 parsecs, deprojected), with the γ-ray and optical flares possibly being related to the evolution of four distinct superluminal components identified in the flow. Conclusions. The observations indicate that both the quiescent and flaring components of the γ-ray emission are produced in a region of the jet that extends up to ∼23 pc. This region may correspond to the Compton-loss dominated zone of the flow and its large extent may favor the synchrotron self-Compton mechanism for γ-ray production in the relativistic jet of the quasar 3C 345.

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“…This correlation was confirmed for another radio galaxy, 3C 120 (León-Tavares et al 2010), suggesting that this link is common for all radio-loud galaxies and radio-loud quasars. The link between optical continuum variability and kinematics of the parsec-scale jet is interpreted in terms of optical flares generated at subparsec-scales in the innermost part of a relativistic jet (Arshakian et al 2010;León-Tavares et al 2010) rather than in the accretion disk. This suggests that the bulk of optical continuum emission is non-thermal and Doppler-boosted.…”

Section: Optical Continuum Luminosity and Properties Of The Jet For Mmentioning

confidence: 99%

“…We should expect that in quasars Table 3 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/520/A62 the emission from both the central engine (thermal?) and the jet (non-thermal) contribute to the total power, whereas in radio galaxies the bulk of the optical continuum emission may be attributed to the relativistic jet rather than the central engine hidden by the torus (e.g., Arshakian et al 2010;León-Tavares et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Radio-optical scrutiny of compact AGN: correlations between properties of pc-scale jets and optical nuclear emission

Arshakian¹,

Torrealba

Chavushyan

et al. 2010

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Aims. We study the correlations between the VLBA (Very Long Baseline Array) radio emission at 15 GHz, extended emission at 151 MHz, and optical nuclear emission at 5100 Å for a complete sample of 135 compact jets. Methods. We use the partial Kendall's tau correlation analysis to check the link between radio properties of parsec-scale jets and optical nuclear luminosities of host active galactic nuclei (AGN). Results. We find a significant positive correlation for 99 quasars between optical nuclear luminosities and total radio (VLBA) luminosities of unresolved cores at 15 GHz originated at milliarcseconds scales. For 18 BL Lacs, the optical continuum emission correlates with the radio emission of the jet at 15 GHz. We suggest that the radio and optical emission are beamed and originate in the innermost part of the sub-parsec-scale jet in quasars. Analysis of the relation between the apparent speed of the jet and the optical nuclear luminosity at 5100 Å supports the relativistic beaming model for the optical emission generated in the jet, and allows the peak values of the intrinsic optical luminosity of the jet and its Lorentz factor to be estimated for the populations of quasars (2 × 10 20 W Hz −1 and γ = 52), BL Lacs (9 × 10 21 W Hz −1 and γ = 20), and radio galaxies (1.5 × 10 21 W Hz −1 and γ = 9). The radio-loudness of quasars (the ratio of 15 GHz flux density and optical nuclear flux at 5100 Å) is found to increase at high redshifts, which is interpreted as progressively higher Doppler factors in radio regime compared to those in optical. A strong positive correlation is found between the intrinsic kinetic power of the jet (measured from the flux density at 151 MHz) and the apparent luminosities of the total and the unresolved core emission of the jet at 15 GHz. This correlation is interpreted in terms of an intrinsically more luminous parsec-scale jet producing more luminous extended structure, which is detectable at low radio frequencies, 151 MHz. A possibility that the low frequency radio emission is relativistically beamed in superluminal sources and therefore correlates with radio luminosity of the jet at 15 GHz cannot be ruled out. Monitoring of superluminal AGN in a wide range of frequencies is required to check the contribution of each effect.

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Relativistic Plasma as the Dominant Source of the Optical Continuum Emission in the Broad-Line Radio Galaxy 3c 120

Cited by 48 publications

References 36 publications

Spectral optical monitoring of 3C 390.3 in 1995–2007

Spectral optical monitoring of 3C 390.3 in 1995–2007

Relativistic outflow drivesγ-ray emission in 3C 345

Radio-optical scrutiny of compact AGN: correlations between properties of pc-scale jets and optical nuclear emission

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