2016/01/26 by R. T. Coogan, Rosemary T. Coogan, A. M. Brown +3
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Emission spectrum #Fermi Gamma-ray Space Telescope #Flare #Flux (metallurgy) #Galaxy #Physics #Quasar #Radio Astronomy Observations and Technology #Spectral line #Spectral shape analysis #Spitzer Space Telescope #Supermassive black hole #Telescope #astro-ph.GA #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stw199
Accepted for publication in MNRAS, 12 pages, 8 figures, 3 tables
arxiv created 2016/01/26 · openalex publication_date 2016/03/07 · arxiv updated 2016/03/23 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In 2014 May–July, the flat spectrum radio quasar 3C 454.3 exhibited strong flaring behaviour. Observations with the Large Area Telescope detector on-board the Fermi Gamma-ray Space Telescope captured the γ-ray flux at energies 0.1 ≤ Eγ ≤ 300 GeV increasing fivefold during this period, with two distinct peaks in emission. The γ-ray emission is analysed in detail, in order to study the emission characteristics and put constraints on the location of the emission region. We explore variability in the spectral shape of 3C 454.3, search for evidence of a spectral cutoff, quantify the significance of very high energy emission and investigate whether or not an energy-dependence of the emitting electron cooling exists. γ-ray intrinsic doubling time-scales as small as τint = 0.68 ± 0.01 h at a significance of >5σ are found, providing evidence of a compact emission region. Significant Eγ, emitted ≥ 35 GeV and Eγ, emitted ≥ 50 GeV emission are also observed. The location of the emission region can be constrained to r ≥ 1.3 × |R_\rm BLR^\rm out|, a location outside the broad-line region. The spectral variation of 3C 454.3 also suggests that these flares may be originating further downstream of the supermassive black hole than the emission before and after the flares.