<i>FERMI</i>LARGE AREA TELESCOPE OBSERVATIONS OF MISALIGNED ACTIVE GALACTIC NUCLEI

Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, Luca; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, Pascal; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Celotti, A.; Charles, E.; Chekhtman, A.; Chen, Andrew; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Conrad, J.; Davis, David; Dermer, C. D.; Angelis, A. De; Palma, F. de; Silva, E. Do Couto E; Drell, P. S.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fortin, P.; Frailis, M.; Fukazawa, Yasushi; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grandi, P.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Landé, J.; Latronico, L.; Lee, S.-H.; Lemoine‐Goumard, M.; Garde, M. Llena; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Malaguti, G.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Migliori, G.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godó, M.; Nestoras, I.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J.; Parent, D.; Pelassa, V.; Pepé, M.; Peršić, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reyes, Luis; Roth, M.; Sadrozinski, H. F-W.; Sánchez, David; Sander, A.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, Takaaki; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Torresi, E.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.

doi:10.1088/0004-637x/720/1/912

Cited by 165 publications

(244 citation statements)

References 60 publications

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“…In leptonic models, γ-ray radiation from blazars is mostly explained by Compton scattering of low-energy synchrotron photons by the same relativistic electrons in the jets producing the synchrotron emission at lower frequencies (e.g., Bloom & Marscher, 1996); in hadronic models, the high-energy emission is dominated by relativistic protons (e.g., Böttcher, 2010). Besides the blazars, there are dozens of misaligned AGN detected by the Fermi (e.g., Abdo et al, 2010a;Ackermann et al, 2015). The sample size is still small, though they constitute a very interesting class of γ-ray emitters.…”

Section: Introductionmentioning

confidence: 99%

Radio properties of the γ ‐ray emitting CSO candidate 2234+282

Cui

Gabányi

et al. 2016

Astron Nachr

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Most of the γ-ray emitting active galactic nuclei (AGN) are blazars, although there is still a small fraction of non-blazar AGN in the Fermi/LAT catalog. Among these misaligned γ-ray-emitting AGN, a few can be classified as Compact Symmetric Objects (CSOs). In contrast to blazars in which γ-ray emission is generally thought to originate from highly beamed relativistic jets, the source of γ-ray emission in unbeamed CSOs remains an open question. The rarity of the γ-ray emitting CSOs is a mystery as well. Here we present the radio properties of the γ-ray CSO candidate 2234+282.

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Section: Introductionmentioning

confidence: 99%

Radio properties of the γ ‐ray emitting CSO candidate 2234+282

Cui

Gabányi

et al. 2016

Astron Nachr

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“…The majority among those associated with radio sources possess relatively large core dominance (Abdo et al 2010), indicating that their viewing angle is probably not large. Assuming θ < 20 • , if Γ < 10, PS01 deviation is no more than a factor of ∼6 (at E > mc 2 ).…”

Section: Discussionmentioning

confidence: 99%

Hadronic beam models for quasars and microquasars

Torres

Reimer

2011

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Context. Most of the hadronic jet models for quasars (QSOs) and microquasars (MQs) found in the literature represent beams of particles (e.g. protons). These particles interact with the matter in the stellar wind of the companion star in the system or with crossing clouds, generating γ-rays via proton-proton processes. Aims. Our aim is to derive the particle distribution in the jet as seen by the observer, so that the γ-ray and neutrino yields can be properly computed. Methods. We use relativistic invariants to obtain the transformed expressions in the cases of both a power law and power law with a cutoff particle distribution in the beam. We compare them with previous expressions used earlier in the literature. Results. We show that formerly used expressions for the particle distributions in the beam as seen by the observer are in error, with the differences being strongly dependent on the viewing angle. For example, for Γ = 10 (Γ is the Lorentz factor of the blob) and angles larger than ∼20 • , the calculation used earlier entails an overprediction (order of magnitude or more) of the proton spectra for E > Γmc 2 , whereas it always overpredicts (two orders of magnitude) the proton spectrum at lower energies, for all the viewing angles. Conclusions. All the results for photon and neutrino fluxes in hadronic models are affected in beams that have made use of the earlier calculation. Given that correct γ-ray fluxes will in almost any case be significantly diminished in comparison with published results and that the time of observations in Cherenkov facilities grows with the square of the flux-reduction factor in a statistically limited result, the possibility of observing hadronic beams is undermined.

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“…In addition to those, new classes of non-blazar γ-ray bright AGN have been discovered by the LAT. The elusive class of γ-ray detected misaligned radio-loud AGN has grown to a size of 29 sources (Abdo et al 2010e;Ackermann et al 2015). Apart from three radio galaxies (Cen A, Cen B, and Pic A), the source PKS B 0625-354 is in the TANAMI sample.…”

Section: High-energy Emission Of Blazars and Other Classes Of Agnmentioning

confidence: 99%

TANAMI: Multiwavelength and multimessenger observations of active galaxies

2015

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Extragalactic jets launched from the immediate vicinity of supermassive black holes in radio-loud active galactic nuclei (AGN) are key objects in modern astronomy and astroparticle physics. AGN jets carry a fraction of the total gravitational energy released during the accretion of matter onto supermassive black holes and are prime suspects as possible sources of ultrahigh-energy cosmic rays and the recently detected extraterrestrial neutrinos at PeV energies. TANAMI (Tracking Active galactic Nuclei with Austral Milliarcsecond Interferometry) is a multiwavelength program monitoring AGN jets of the southern sky. It combines high-resolution imaging and spectral monitoring at radio wavelengths with higher-frequency observations at IR, optical/UV, X-ray, and γ-ray energies. We review recent results of the TANAMI program, highlighting AGN candidate neutrino-emitters in the error circles of the IceCube PeV neutrino events.

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FERMILARGE AREA TELESCOPE OBSERVATIONS OF MISALIGNED ACTIVE GALACTIC NUCLEI

Cited by 165 publications

References 60 publications

Radio properties of the γ ‐ray emitting CSO candidate 2234+282

Radio properties of the γ ‐ray emitting CSO candidate 2234+282

Hadronic beam models for quasars and microquasars

TANAMI: Multiwavelength and multimessenger observations of active galaxies

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