Relativistic outflow drives γ-ray emission in 3C 345

被引：65

作者：

Schinzel, F. K. ^{[1
]}

Lobanov, A. P. ^{[1
]}

Taylor, G. B. ^{[2
]}

Jorstad, S. G. ^{[3
,4
]}

Marscher, A. P. ^{[3
]}

Zensus, J. A. ^{[1
]}

机构：

[1] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[2] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA

[3] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA

[4] St Petersburg State Univ, St Petersburg, Russia

来源：

ASTRONOMY & ASTROPHYSICS | 2012年 / 537卷

基金：

美国国家科学基金会;

关键词：

galaxies: jets; galaxies: active; radio continuum: galaxies; gamma rays: galaxies; Galaxy: nucleus; galaxies: individual: 3C 345; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; PARSEC-SCALE JET; BROAD-LINE REGION; POLARIMETRIC OBSERVATIONS; OPTICAL CONTINUUM; VLBI OBSERVATIONS; HIGH-FREQUENCIES; QUASAR; 3C-345; RADIO-SOURCES;

D O I：

10.1051/0004-6361/201117705

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. On the basis of the first 20 months of Fermi-LAT data and optical monitoring, the quasar 3C 345 has been identified as a gamma-ray emitter. We investigate whether there is a connection between the gamma-ray and optical variability of 3C 345 and the properties of its parsec-scale radio emission. Methods. We combined the Fermi-LAT data of 3C 345, covering an energy range of 0.1-300 GeV, with 32 Very Long Baseline Array observations of the object made at 43.2 GHz in the period of January 2008-March 2010. Results. The VLBA data reveal the morphology and kinematics of the flow on scales of up to approximate to 5 milliarcseconds (deprojected linear distances of 380 parsecs). The brightness temperature, T-b(r), measured along the jet first decreases with distance proportional to r(-(0.95+/-0.69)) and later exhibits a break at approximate to 0.3 milliarcseconds (mas), with T-b(r) proportional to r(-(4.11+/-0.85)) at larger separations. Variations in the gamma-ray, optical, and parsec-scale radio emission display a similar long-term trend that persists during the entire VLBA monitoring period. The gamma-ray and optical variations on shorter timescales are related to structural changes in the jet on scales of approximate to 0.3 mas (approximate to 23 parsecs, deprojected), with the gamma-ray and optical flares possibly being related to the evolution of four distinct superluminal components identified in the flow. Conclusions. The observations indicate that both the quiescent and flaring components of the gamma-ray emission are produced in a region of the jet that extends up to similar to 23 pc. This region may correspond to the Compton-loss dominated zone of the flow and its large extent may favor the synchrotron self-Compton mechanism for gamma-ray production in the relativistic jet of the quasar 3C 345.

引用

页数：9

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