MAGIC Observations and multiwavelength properties of the quasar 3C 279 in 2007 and 2009

Aleksić, J.; Antonelli, L. A.; Antoranz, P.; Backes, Michael; Barrio, J. A.; Bastieri, D.; González, J. Becerra; Bednarek, W.; Berdyugin, A.; Berger, K.; Bernardini, E.; Biland, A.; Blanch, O.; Böck, R.; Boller, A.; Bonnoli, G.; Tridon, D. Borla; Braun, I.; Bretz, T.; Cañellas, A.; Carmona, E.; Carosi, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Cossio, L.; Covino, S.; Dazzi, F.; Angelis, A. De; Pozo, E. De Cea del; Lotto, B. De; Mendez, C. Delgado; Ortega, A. Diago; Doert, M.; Domínguez, A.; Prester, D. Dominis; Dorner, D.; Doro, M.; Elsäesser, D.; Ferenc, D.; Fonseca, M. V.; Font, L.; Fruck, C.; López, R. J. García; Garczarczyk, M.; Garrido, Daniel; Giavitto, G.; Godinović, N.; Hadasch, D.; Häfner, D.; Herrero, A.; Hildebrand, D.; Hose, J.; Hrupec, Dario; Huber, Bernhard A.; Jogler, T.; Klepser, S.; Krähenbühl, T.; Krause, J.; Barbera, A. La; Lelas, D.; Leonardo, E.; Lindfors, E.; Lombardi, S.; López, M.; Lorenz, E.; Majumdar, P.; Makariev, M.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Meucci, M.; Miranda, J. M.; Mirzoyan, R.; Miyamoto, H.; Moldón, J.; Moralejo, A.; Nieto, D.; Nilsson, K.; Orito, R.; Oya, I.; Paoletti, R.; Pardo, Sharon; Paredes, J. M.; Partini, S.; Pasanen, M.; Pauß, F.; Pérez-Torres, M. A.; Peršić, M.; Peruzzo, L.; Pilia, M.; Pochon, J.; Prada, Francisco; Moroni, P. G. Prada; Prandini, E.; Puljak, I.; Reichardt, I.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Rügamer, S.; Rüger, Michael; Saggion, A.; Saito, Koji; Saito, Takayuki; Salvati, M.; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schweizer, T.; Shayduk, M.; Shore, S. N.; Sillanpää, A.; Sitarek, J.; Sobczyńska, D.; Spanier, F.; Spiro, S.; Stamerra, A.; Steinke, B.; Storz, J.; Strah, N.; Surić, T.; Takalo, L. O.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Thom, M.; Tibolla, O.; Torres, D. F.; Treves, A.; Vankov, H.; Vogler, P.; Wagner, R. M.; Weitzel, Q.; Zabalza, V.; Zandanel, F.; Zanin, R.

doi:10.1051/0004-6361/201116497

Cited by 78 publications

(51 citation statements)

References 72 publications

(76 reference statements)

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“…All of our models are generally in agreement with these bounds across all wavelengths. While our fiducial model does slightly exceed the bounds set by Albert et al (2008) in the optical, we do not find a conflict with the standard ≥ 1.5 bound in Table 2, and we are within 1σ agreement with the harder spectrum observed by Aleksić et al (2011b).…”

Section: Constraints From Gamma-ray Observationssupporting

confidence: 78%

Semi-analytic modelling of the extragalactic background light and consequences for extragalactic gamma-ray spectra

Gilmore

Somerville

Primack

et al. 2012

Monthly Notices of the Royal Astronomical Society

483

582

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Attenuation of high-energy gamma-rays by pair production with ultraviolet, optical and infrared (IR) extragalactic background light (EBL) photons provides a link between the history of galaxy formation and high-energy astrophysics. We present results from our latest semi-analytic models (SAMs), which employ the main ingredients thought to be important to galaxy formation and evolution, as well as an improved model for reprocessing of starlight by dust to mid- and far-IR wavelengths. These SAMs are based upon a Λ cold dark matter hierarchical structural formation scenario, and are successful in reproducing a large variety of observational constraints such as number counts, luminosity and mass functions and colour bimodality. Our fiducial model is based upon a Wilkinson Microwave Anisotropy Probe 5-year cosmology, and treats dust emission using empirical templates. This model predicts a background flux considerably lower than optical and near-IR measurements that rely on subtraction of zodiacal and galactic foregrounds, and near the lower bounds set by number counts of resolvable sources at a large number of wavelengths. We also show the results of varying cosmological parameters and dust attenuation model used in our SAM. For each EBL prediction, we show how the optical depth due to electron-positron pair production is affected by redshift and gamma-ray energy, and the effect of gamma-ray absorption on the spectra of a variety of extragalactic sources. We conclude with a discussion of the implications of our work, comparisons to other models and key measurements of the EBL and a discussion of how the burgeoning science of gamma-ray astronomy will continue to help constrain cosmology. The low EBL flux predicted by our fiducial model suggests an optimistic future for further studies of distant gamma-ray sources.Ministerio de Educación y Ciencia FIS2008-04189Fondo Europeo de Desarrollo Regional CSD2007-00042Junta de Andalucía P07-FQM-0289

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Section: Constraints From Gamma-ray Observationssupporting

confidence: 78%

Semi-analytic modelling of the extragalactic background light and consequences for extragalactic gamma-ray spectra

Gilmore

Somerville

Primack

et al. 2012

Monthly Notices of the Royal Astronomical Society

483

582

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“…3C 279 presents variable emission throughout the entire electromagnetic spectrum on several timescales, showing some periods of low activity and others in which intense flares are observed (Maraschi et al 1994;Wehrle et al 1998;Hartman et al 2001a;Larionov et al 2008;Chatterjee et al 2008;Collmar et al 2010;Abdo et al 2010;Aleksić et al 2011; A&A proofs: manuscript no. 35170corr Hayashida et al 2012;Rani et al 2017;Patiño-Álvarez et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength analysis of brightness variations of 3C 279: probing the relativistic jet structure and its evolution

Beaklini

Dominici

Abraham

et al. 2019

A&A

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Aims. We studied the correlation between brightness and polarization variations in 3C 279 at different wavelengths, over time intervals long enough to cover the time lags due to opacity effects. We used these correlations together with VLBI images to constrain the radio and high energy source position. Methods. We made 7 mm radio continuum and R-band polarimetric observations of 3C 279 between 2009 and 2014. The radio observations were performed at the Itapetinga Radio Observatory, while the polarimetric data were obtained at Pico dos Dias Observatory, both in Brazil. We compared our observations with the γ-ray Fermi/LAT and R-band SMARTS light curves. Results. We found a good correlation between 7 mm and R-band light curves, with a delay of 170 ± 30 days in radio, but no correlation with the γ rays. However, a group of several γ-ray flares in April 2011 could be associated with the start of the 7 mm strong activity observed at the end of 2011.We also detected an increase in R-band polarization degree and rotation of the polarization angle simultaneous with these flares. Contemporaneous VLBI images at the same radio frequency show two new strong components close to the core, ejected in directions very different from that of the jet. Conclusions. The good correlation between radio and R-band variability suggests that their origin is synchrotron radiation. The lack of correlation with γ-rays produced by the Inverse Compton process on some occasions could be due to the lack of low energy photons in the jet direction or to absorption of the high energy photons by the broad line region clouds. The variability of the polarization parameters during flares can be easily explained by the combination of the jet polarization parameters and those of newly formed jet components.

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“…Additionally, the detection in TeV γ -rays of a few FSRQs, including a recent confirmation for PKS 1510−089 (Cortina et al 2012) (others are 3C 279, Albert et al 2008Aleksić et al 2011aand PKS 1222+216, Aleksić et al 2011b, challenges traditional EC scenarios because jet-emitted TeV photons would be readily lost by photon-photon pair production with the copious soft photons surrounding the jet. These findings have thus stimulated a renewed interest in the possibility that even for some of these powerful jets in systems with luminous accretion disc and broad-line emission, the γ -ray emission may be predominantly by SSC (for analysis on 3C 279 see e.g.…”

Section: Pure Sscmentioning

confidence: 99%

Time-dependent simulations of emission from the FSRQ PKS 1510−089: multiwavelength variability of external Compton and synchrotron self-Compton models

Chen

Fossati

Böttcher

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present results of modelling the broad‐band spectral energy distribution (SED) and multiwavelength variability of the bright flat spectrum radio quasars PKS 1510−089 with our time‐dependent multizone Monte Carlo/Fokker–Planck code. As the primary source of seed photons for inverse Compton scattering, we consider radiation from the broad‐line region (BLR), from the hot dust of the molecular torus and the local synchrotron radiation [synchrotron self‐Compton (SSC)]. We evaluate the viability of different Compton models by comparing simulated multiwavelength light curves and SEDs with one of the best observed flares by PKS 1510−089, in 2009 March. The time dependence of our code and its correct handling of light travel time effects allow us to fully take into account the effect of the finite size of the active region, and in turn to fully exploit the information carried by time‐resolved observed SEDs that are becoming increasingly available since the launch of Fermi. We confirm that the spectrum adopted for the external radiation field has an important impact on the modelling of the SED, in particular for the lower energy end of the Compton component which is observed in the X‐ray band, which in turn is one of the most critical bands to assess the differences between external Compton and SSC emission. In the context of the scenario presented in this paper, where the flaring is caused by the increase of the number of relativistic electrons ascribed to the effect of the interaction of a portion of the jet (blob) with a shock, we cannot firmly discriminate the three main scenarios for γ‐ray emission. However, results show clearly the differences produced by a more realistic treatment of the emitting source in the shape of SEDs and their time variability over relevant, observable time‐scales, and demonstrate the crucial importance of time‐dependent multizone models to advance our understanding of the physics of these sources, by taking full advantage of the wealth of information offered by the high‐quality data of current multiwavelength campaigns.

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MAGIC Observations and multiwavelength properties of the quasar 3C 279 in 2007 and 2009

Cited by 78 publications

References 72 publications

Semi-analytic modelling of the extragalactic background light and consequences for extragalactic gamma-ray spectra

Semi-analytic modelling of the extragalactic background light and consequences for extragalactic gamma-ray spectra

Multiwavelength analysis of brightness variations of 3C 279: probing the relativistic jet structure and its evolution

Time-dependent simulations of emission from the FSRQ PKS 1510−089: multiwavelength variability of external Compton and synchrotron self-Compton models

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