Please use this identifier to cite or link to this item:
|Title:||The structure and emission model of the relativistic jet in the quasar 3C279 inferred from radio to high-energy γ-ray observations in 2008-2010||Authors:||Hayashida, M.
RAITERI, Claudia Maria
BUEMI, CARLA SIMONA
DI PAOLA, Andrea
UMANA, Grazia Maria Gloria
|Issue Date:||2012||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||754||Issue:||2||First Page:||114||Abstract:||We present time-resolved broadband observations of the quasar 3C279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. While investigating the previously reported γ-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears to be delayed with respect to the γ-ray emission by about 10days. X-ray observations reveal a pair of "isolated" flares separated by 90 days, with only weak γ-ray/optical counterparts. The spectral structure measured by Spitzer reveals a synchrotron component peaking in the mid-infrared band with a sharp break at the far-infrared band during the γ-ray flare, while the peak appears in the millimeter (mm)/submillimeter (sub-mm) band in the low state. Selected spectral energy distributions are fitted with leptonic models including Comptonization of external radiation produced in a dusty torus or the broad-line region. Adopting the interpretation of the polarization swing involving propagation of the emitting region along a curved trajectory, we can explain the evolution of the broadband spectra during the γ-ray flaring event by a shift of its location from 1pc to 4pc from the central black hole. On the other hand, if the γ-ray flare is generated instead at sub-pc distance from the central black hole, the far-infrared break can be explained by synchrotron self-absorption. We also model the low spectral state, dominated by the mm/sub-mm peaking synchrotron component, and suggest that the corresponding inverse-Compton component explains the steady X-ray emission. © 2012. The American Astronomical Society. All rights reserved..||URI:||http://hdl.handle.net/20.500.12386/32899||URL:||https://iopscience.iop.org/article/10.1088/0004-637X/754/2/114
|Appears in Collections:||1.01 Articoli in rivista|
Show full item record
Files in This Item:
checked on Dec 7, 2023
checked on Dec 7, 2023
Items in DSpace are published in Open Access, unless otherwise indicated.