THE BRIGHTEST GAMMA-RAY FLARING BLAZAR IN THE SKY:
                    <i>AGILE</i>
                    AND MULTI-WAVELENGTH OBSERVATIONS OF 3C 454.3 DURING 2010 NOVEMBER

Vercellone, S.; Striani, E.; Vittorini, V.; Donnarumma, I.; Pacciani, L.; Pucella, G.; Tavani, M.; Raiteri, C. M.; Villata, M.; Romano, P.; Fiocchi, M.; Bazzano, A.; Bianchin, V.; Ferrigno, C.; Maraschi, L.; Pian, E.; Türler, M.; Ubertini, P.; Bulgarelli, A.; Chen, Andrew; Giuliani, A.; Longo, F.; Barbiellini, G.; Cardillo, M.; Cattaneo, P. W.; Monte, E. Del; Evangelista, Y.; Feroci, M.; Ferrari, A.; Fuschino, F.; Gianotti, F.; Giusti, M.; Lazzarotto, F.; Pellizzoni, A.; Piano, G.; Pilia, M.; Rapisarda, M.; Rappoldi, A.; Sabatini, S.; Soffitta, P.; Trifoglio, M.; Trois, A.; Giommi, P.; Lucarelli, F.; Pittori, C.; Santolamazza, P.; Verrecchia, F.; Agudo, I.; Aller, H. D.; Aller, M. F.; Arkharov, A. A.; Bach, U.; Berdyugin, A.; Borman, G. A.; Chigladze, R. A.; Efimov, Yu. S.; Ефимова, Н. В.; Gómez, J. L.; Gurwell, M. A.; McHardy, I. M.; Joshi, M.; Kimeridze, G. N.; Krajci, Tom; Kurtanidze, O. M.; Kurtanidze, S. O.; Larionov, V. M.; Lindfors, E.; Molina, S. N.; Morozova, D. A.; Назаров, С. В.; Nikolashvili, M. G.; Nilsson, K.; Pasanen, M.; Reinthal, R.; Ros, Javier; Sadun, A. C.; Sakamoto, T.; Sallum, Stephanie; Сергеев, С. Г.; Schwartz, Richard D.; Sigua, L. A.; Sillanpää, A.; Sokolovsky, K. V.; Strelnitski, V.; Takalo, L. O.; Taylor, B.; Walker, G.

doi:10.1088/2041-8205/736/2/l38

Cited by 80 publications

(52 citation statements)

References 34 publications

(46 reference statements)

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“…This increases with respect to the BH the location of the dissipation region during the highest state although by less than a factor of 1.4. A one-zone leptonic model has been used also by Vercellone et al (2010), Pacciani et al (2010), and Vercellone et al (2011) to explain the dynamic behavior of the SEDs during outbursts I and III. The authors employ the synchrotron, SSC, and EC mechanisms, with seed photons for IC scattering provided by the accretion disk and BLR.…”

Section: Discussionmentioning

confidence: 99%

“…The similarity in structure of flare a at optical and γ -ray frequencies implies that the flaring emission at the two wavelengths originates in the same region. The difference between the relative amplitudes of γ -ray versus optical peaks can be explained as the result of differences in relativistic boosting of γ -ray and optical emission, as proposed by Raiteri et al (2011), or by variations in the density of seed photons available for scattering to γ -ray energies, as suggested by Vercellone et al (2011). The latter is additionally supported by existence of orphan optical outbursts, for example, a very sharp spike at ∼10 days before the maximum when the fastest optical variability during outburst III was observed (Table 3) without an obvious counterpart in the γ -ray light curve ( Figure 5, the bottom insert).…”

Section: Optical Outburstsmentioning

confidence: 99%

“…Flare b is distinct during outburst III as well, although it precedes the γ -ray flare b by ∼9 days. Table 3 shows that the minimum timescale of variability is ∼18-24 hr with the optical flux changing by a factor of 1.5-2.5 (see also Raiteri et al 2011;Vercellone et al 2011). Comparison of Tables 1-3 reveals that the timescale of optical variability is different from τ γ and similar to τ X , which is longer by a factor of five than the minimum timescale of the γ -ray flux.…”

Section: Optical Outburstsmentioning

confidence: 99%

“…Villata et al (2007), Raiteri et al (2008), Hagen-Thorn et al (2009), andJorstad et al (2010) have analyzed comprehensive multi-waveband observations of an extraordinary radio to X-ray outburst in 2005, as well as major, but less pronounced, flares over the following two years. After the launch of the Astro-rivelatore Gamma a Immagini LEggero (AGILE) and Fermi Gamma-ray Space Telescope orbiting observatories, 3C 454.3 displayed unprecedentedly bright γ -ray outbursts in late 2009, 2010 April, and late 2010 (Ackermann et al 2010;Abdo et al 2011;Bonnoli et al 2011;Raiteri et al 2011;Vercellone et al 2011;Wehrle et al 2012). During the 2010 event, 3C 454.3 reached the highest γ -ray flux ever detected from a single non-transient cosmic source.…”

Section: Introductionmentioning

confidence: 99%

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A Tight Connection Between Gamma-Ray Outbursts and Parsec-Scale Jet Activity in the Quasar 3c 454.3

Jorstad

Marscher

Smith

et al. 2013

ApJ

164

113

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We analyze the multi-frequency behavior of the quasar 3C 454.3 during three prominent γ -ray outbursts: 2009 Autumn, 2010 Spring, and 2010 Autumn. The data reveal a repeating pattern, including a triple flare structure, in the properties of each γ -ray outburst, which implies similar mechanism(s) and location for all three events. The multi-frequency behavior indicates that the lower frequency events are co-spatial with the γ -ray outbursts, although the γ -ray emission varies on the shortest timescales. We determine that the variability from UV to IR wavelengths during an outburst results from a single synchrotron component whose properties do not change significantly over the different outbursts. Despite a general increase in the degree of optical linear polarization during an outburst, the polarization drops significantly at the peak of the γ -ray event, which suggests that both shocks and turbulent processes are involved. We detect two disturbances (knots) with superluminal apparent speeds in the parsec-scale jet associated with the outbursts in 2009 Autumn and 2010 Autumn. The kinematic properties of the knots can explain the difference in amplitudes of the γ -ray events, while their millimeterwave polarization is related to the optical polarization during the outbursts. We interpret the multi-frequency behavior within models involving either a system of standing conical shocks or magnetic reconnection events located in the parsec-scale millimeter-wave core of the jet. We argue that γ -ray outbursts with variability timescales as short as ∼3 hr can occur on parsec scales if flares take place in localized regions such as turbulent cells.

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Section: Discussionmentioning

confidence: 99%

Section: Optical Outburstsmentioning

confidence: 99%

Section: Optical Outburstsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A Tight Connection Between Gamma-Ray Outbursts and Parsec-Scale Jet Activity in the Quasar 3c 454.3

Jorstad

Marscher

Smith

et al. 2013

ApJ

164

113

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“…The latter two were monitored at γ-ray energies by the AGILE satellite (Donnarumma et al 2009;Vercellone et al 2009). In 2009 December, 3C454.3 became the brightest source in the γ-ray sky, (e.g., Pacciani et al 2010), and an exceptional γ-ray outburst in 2010 November (Abdo et al 2011a) was accompanied by dramatic activity in the quasar across the electromagnetic spectrum (e.g., Vercellone et al 2011;Wehrle et al 2012). All of these high-energy outbursts from 2005 to 2010 were associated with ejections of superluminal knots into the 43GHz parsec-scale jet, KI-KIII , and K09, K10 (Jorstad et al 2013b).…”

mentioning

confidence: 99%

Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz within the VLBA-BU-BLAZAR Program

Jorstad

Marscher

Morozova

et al. 2017

ApJ

331

499

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We analyze the parsec-scale jet kinematics from 2007 June to 2013 January of a sample of γ-ray bright blazars monitored roughly monthly with the Very Long Baseline Array at 43GHz. In a total of 1929 images, we measure apparent speeds of 252 emission knots in 21 quasars, 12 BLLacertae objects (BLLacs), and 3 radio galaxies, ranging from 0.02c to 78c; 21% of the knots are quasi-stationary. Approximately one-third of the moving knots execute non-ballistic motions, with the quasars exhibiting acceleration along the jet within 5pc (projected) of the core, and knots in BLLacs tending to decelerate near the core. Using the apparent speeds of the components and the timescales of variability from their light curves, we derive the physical parameters of 120 superluminal knots, including variability Doppler factors, Lorentz factors, and viewing angles. We estimate the half-opening angle of each jet based on the projected opening angle and scatter of intrinsic viewing angles of knots. We determine characteristic values of the physical parameters for each jet and active galactic nucleus class based on the range of values obtained for individual features. We calculate the intrinsic brightness temperatures of the cores, T b,int core , at all epochs, finding that the radio galaxies usually maintain equipartition conditions in the cores, while ∼30% of T b,int core measurements in the quasars and BLLacs deviate from equipartition values by a factor >10. This probably occurs during transient events connected with active states. In the Appendix, we briefly describe the behavior of each blazar during the period analyzed.

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An optical view of BL Lacertae objects

Falomo

Pian²,

Treves

2014

Astron Astrophys Rev

138

109

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BL Lac objects are active nuclei, hosted in massive elliptical galaxies, the emission of which is dominated by a relativistic jet closely aligned with the line of sight. This implies the existence of a parent population of sources with a misaligned jet, that have been identified with low-power radiogalaxies. The spectrum of BL Lacs, dominated by non-thermal emission over the whole electromagnetic range, together with bright compact radio cores, high luminosities, rapid and large amplitude flux variability at all frequencies and strong polarization make these sources an optimal laboratory for high energy astrophysics. A most distinctive characteristic of the class is the weakness or absence of spectral lines, that historically hindered the identification of their nature and ever thereafter proved to be a hurdle in the determination of their distance. In this paper we review the main observational facts that contribute to the present basic interpretation of this class of active galaxies. We overview the history of the BL Lac objects research field and their population as it emerged from multi-wavelength surveys. The properties of the flux variability and polarization, compared with those at radio, X-ray and gamma-ray frequencies, are summarized together with the present knowledge of the host galaxies, their environments, and central black hole masses. We focus this review on the optical observations, that played a crucial role in the early phase of BL Lacs studies, and, in spite of extensive radio, X-ray, and recently gamma-ray observations, could represent the future major contribution to the unveiling of the origin of these sources. In particular they could provide a firm conclusion on the long debated issue of the cosmic evolution of this class of active galactic nuclei and on the connection between formation of supermassive black holes and relativistic jets.

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THE BRIGHTEST GAMMA-RAY FLARING BLAZAR IN THE SKY: AGILE AND MULTI-WAVELENGTH OBSERVATIONS OF 3C 454.3 DURING 2010 NOVEMBER

Cited by 80 publications

References 34 publications

A Tight Connection Between Gamma-Ray Outbursts and Parsec-Scale Jet Activity in the Quasar 3c 454.3

A Tight Connection Between Gamma-Ray Outbursts and Parsec-Scale Jet Activity in the Quasar 3c 454.3

Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz within the VLBA-BU-BLAZAR Program

An optical view of BL Lacertae objects

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