Flaring γ-Ray Emission from High Redshift BlazarsReportar como inadecuado

Flaring γ-Ray Emission from High Redshift Blazars

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INAF - Istituto di Radioastronomia, Via Gobetti 101, Bologna I-40129, Italy


Dipartimento di Fisica e Astronomia, Universitá degli Studi di Bologna, Viale Berti Pichat, 6-2, Bologna I-40127, Italy


U.S. Naval Research Laboratory, Code 7653, 4555 Overlook Ave SW, Washington, DC 20375-5352, USA


Author to whom correspondence should be addressed.

Academic Editors: Jose L. Gómez, Alan P. Marscher and Svetlana G. Jorstad

Abstract High redshift blazars are among the most powerful objects in the Universe. Although they represent a significant fraction of the extragalactic hard X-ray sky, they are not commonly detected in γ-rays. High redshift z > 2 objects represent < 10 per cent of the active galactic nuclei AGN population observed by Fermi so far, and γ-ray flaring activity from these sources is even more uncommon. The characterization of the radio-to-γ-ray properties of high redshift blazars represents a powerful tool for the study of the energetics of such extreme objects and the Extragalactic Background Light. This contribution will present results of multi-band campaigns, from radio to γ-rays, on PKS 0836+710, PKS 2149−306, and TXS 0536+145. The latter is the highest redshift detection of a flaring γ-ray blazar so far. At the peaks of their respective flares these sources reached an apparent isotropic gamma-ray luminosity of about 10 50 erg·s − 1 , which is comparable with the luminosity observed from the most powerful blazars. The physical properties derived from the multi-wavelength observations of these sources are then compared with those shown by the high redshift population. View Full-Text

Keywords: galaxies: active; gamma-rays: general; radiation mechanisms: non-thermal galaxies: active; gamma-rays: general; radiation mechanisms: non-thermal

Autor: Monica Orienti 1,* , Filippo D’Ammando 1,2, Marcello Giroletti 1, Justin Finke 3 and Daniele Dallacasa 1,2

Fuente: http://mdpi.com/


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