2009ApJ...696..328H


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.06CET19:08:25

2009ApJ...696..328H - Astrophys. J., 696, 328-347 (2009/May-1)

Full polarization spectra of 3C 279.

HOMAN D.C., LISTER M.L., ALLER H.D., ALLER M.F. and WARDLE J.F.C.

Abstract (from CDS):

We report the results of parsec-scale, multifrequency Very Long Baseline Array observations of the core region of 3C 279 in Stokes I, linear polarization, and circular polarization. These full polarization spectra are modeled by radiative transfer simulations to constrain the magnetic field and particle properties of the parsec-scale jet in 3C 279. We find that the polarization properties of the core region, including the amount of linear polarization, the amount and sign of Faraday rotation, and the amount and sign of circular polarization can be explained by a consistent physical picture. The base of the jet, component D, is modeled as an inhomogeneous Blandford-Königl style conical jet dominated by a vector-ordered poloidal magnetic field along the jet axis, and we estimate its net magnetic flux. This poloidal field is responsible for the linear and circular polarization from this inhomogeneous component. Farther down the jet, the magnetic field in two homogeneous features is dominated by local shocks and a smaller fraction of vector-ordered poloidal field remains along the jet axis. This remaining poloidal field provides internal Faraday rotation which drives Faraday conversion of linear polarization into circular polarization from these components. In this picture, we find the jet to be kinetically dominated by protons with the radiating particles being dominated by electrons at an approximate fraction of ≳75%, still allowing the potential for a significant admixture of positrons. Based on the amounts of Faraday conversion deduced for the homogeneous components, we find a plausible range for the lower cutoff in the relativistic particle energy spectrum to be 5 ≲ γl≲ 35. The physical picture described here is not unique if the observed Faraday rotation and depolarization occur in screens external to the jet; however, we find the joint explanation of linear and circular polarization observations from a single set of magnetic fields and particle properties internal to the jet to be compelling evidence for this picture.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: individual: 3C 279 - galaxies: jets - radiation mechanisms: non-thermal - radio continuum: galaxies

Simbad objects: 8

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Number of rows : 8

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3467 3
2 QSO B0607-157 QSO 06 09 40.9477650070 -15 42 40.649794982   18.47 18.0 19.90   ~ 282 1
3 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5251 1
4 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2641 2
5 QSO B1519-273 BLL 15 22 37.67598872 -27 30 10.7854174   18.72 18.5 17.42   ~ 252 1
6 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11077 0
7 ICRF J182931.7+484446 Sy1 18 29 31.7812801678 +48 44 46.158815781   17.05 16.81 16.860   ~ 619 1
8 NAME BL Lac BLL 22 02 43.2913773726 +42 16 39.978417860   15.66 14.72     ~ 1976 1

    Equat.    Gal    SGal    Ecl

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2019.12.06-19:08:25

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