Particle acceleration and magnetic field structure in PKS 2155-304: optical polarimetric observations

被引：16
作者：
Barres de Almeida, U. [1 ]
Ward, M. J. [1 ]
Dominici, T. P. [2 ]
Abraham, Z. [3 ]
Franco, G. A. P. [4 ]
Daniel, M. K. [1 ]
Chadwick, P. M. [1 ]
Boisson, C. [5 ]
机构：
[1] Univ Durham, Dept Phys, Durham DH1 3LE, England
[2] Lab Nacl Astrofis, BR-37504364 Itajuba, Brazil
[3] Univ Sao Paulo, Dept Astron, BR-05508090 Sao Paulo, Brazil
[4] ICEx UFMG, Dept Fis, BR-30123970 Belo Horizonte, MG, Brazil
[5] Observ Paris, F-92190 Meudon, France
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2010年 / 408卷 / 03期
关键词：
polarization; BL Lacertae objects: individual: PKS 2155-304; galaxies: jets; BL LACERTAE OBJECTS; FREQUENCY-DEPENDENT POLARIZATION; ACTIVE GALACTIC NUCLEI; COMPACT RADIO-SOURCES; SYNCHROTRON RADIATION; RELATIVISTIC JETS; VARIABILITY; BLAZARS; PKS-2155-304; MODEL;
D O I：
10.1111/j.1365-2966.2010.17236.x
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
In this paper, we present multiband optical polarimetric observations of the very-high energy blazar PKS 2155-304 made simultaneously with a HESS/Fermi high-energy campaign in 2008, when the source was found to be in a low state. The intense daily coverage of the data set allowed us to study in detail the temporal evolution of the emission, and we found that the particle acceleration time-scales are decoupled from the changes in the polarimetric properties of the source. We present a model in which the optical polarimetric emission originates at the polarized mm-wave core and propose an explanation for the lack of correlation between the photometric and polarimetric fluxes. The optical emission is consistent with an inhomogeneous synchrotron source in which the large-scale field is locally organized by a shock in which particle acceleration takes place. Finally, we use these optical polarimetric observations of PKS 2155-304 at a low state to propose an origin for the quiescent gamma-ray flux of the object, in an attempt to provide clues for the source of its recently established persistent TeV emission.
引用
收藏
页码：1778 / 1787
页数：10
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