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A Hard gamma-ray flare from 3C 279 in 2013 December

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dc.contributor.author Paliya, Vaidehi S
dc.contributor.author Diltz, Chris
dc.contributor.author Bottcher, Markus
dc.contributor.author Stalin, C. S
dc.contributor.author Buckley, David
dc.date.accessioned 2020-11-17T14:19:55Z
dc.date.available 2020-11-17T14:19:55Z
dc.date.issued 2016-01
dc.identifier.citation The Astrophysical Journal, Vol. 817, No. 1, 61 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7141
dc.description Restricted Access © The American Astronomical Society http://dx.doi.org/10.3847/0004-637X/817/1/61 en_US
dc.description.abstract The blazar 3C 279 exhibited twin γ -ray fl ares of similar intensity in 2013 December and 2014 April. In this work, we present a detailed multi-wavelength analysis of the 2013 December fl aring event. Multi-frequency observations reveal the uncorrelated variability patterns with X-ray and optical – UV fl uxes peaking after the γ -ray maximum. The broadband spectral energy distribution ( SED ) at the peak of the γ -ray activity shows a rising γ -ray spectrum but a declining optical – UV fl ux. This observation along with the detection of uncorrelated variability behavior rules out the one-zone leptonic emission scenario. We, therefore, adopt two independent methodologies to explain the SED: a time-dependent lepto-hadronic modeling and a two-zone leptonic radiative modeling approach. In the lepto-hadronic modeling, a distribution of electrons and protons subjected to a randomly orientated magnetic fi eld produces synchrotron radiation. Electron synchrotron is used to explain the IR to UV emission while proton synchrotron emission is used to explain the high-energy γ -ray emission. A combination of both electron synchrotron self-Compton emission and proton synchrotron emission is used to explain the X-ray spectral break seen during the later stage of the fl are. In the two-zone modeling, we assume a large emission region emitting primarily in IR to X-rays and γ -rays to come primarily from a fast-moving compact emission region. We conclude by noting that within a span of four months, 3C 279 has shown the dominance of a variety of radiative processes over each other and this re fl ects the complexity involved in understanding the physical properties of blazar jets in general. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Galaxies: active en_US
dc.subject Galaxies: jets en_US
dc.subject Gamma rays: galaxies en_US
dc.subject Quasars: individual (3C 279) en_US
dc.title A Hard gamma-ray flare from 3C 279 in 2013 December en_US
dc.type Article en_US


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