2019A&A...627A..89B


Query : 2019A&A...627A..89B

2019A&A...627A..89B - Astronomy and Astrophysics, volume 627A, 89-89 (2019/7-1)

The TeV-emitting radio galaxy 3C 264. VLBI kinematics and SED modeling.

BOCCARDI B., MIGLIORI G., GRANDI P., TORRESI E., MERTENS F., KARAMANAVIS V., ANGIONI R. and VIGNALI C.

Abstract (from CDS):

Context. In March 2018, the detection by VERITAS of very-high-energy emission (VHE > 100 GeV) from 3C 264 was reported. This is the sixth, and second most distant, radio galaxy ever detected in the TeV regime. Aims. In this article we present a radio and X-ray analysis of the jet in 3C 264. We determine the main physical parameters of the parsec-scale flow and explore the implications of the inferred kinematic structure for radiative models of this γ-ray emitting jet. Methods. The radio data set is comprised of VLBI observations at 15GHz from the MOJAVE program, and covers a time period of about two years. Through a segmented wavelet decomposition method (WISE code), we estimated the apparent displacement of individual plasma features; we then performed a pixel-based analysis of the stacked image to determine the jet shape. The X-ray data set includes all available observations from the Chandra, XMM, and Swift satellites, and is used, together with archival data in the other bands, to build the spectral energy distribution (SED). Results. Proper motion is mostly detected along the edges of the flow, which appears strongly limb brightened. The apparent speeds increase as a function of distance from the core up to a maximum of ∼11.5c. This constrains the jet viewing angle to assume relatively small values (θ≤10°). In the acceleration region, extending up to a de-projected distance of ∼4.8x104 Schwarzschild radii (∼11pc), the jet is collimating (r∝z0.40±0.04), as predicted for a magnetically-driven plasma flow. By assuming that the core region is indeed magnetically dominated (UB/Ue>1), the SED and the jet power can be well reproduced in the framework of leptonic models, provided that the high-energy component is associated to a second emitting region. The possibility that this region is located at the end of the acceleration zone, either in the jet layer or in the spine, is explored in the modeling.

Abstract Copyright: © B. Boccardi et al. 2019

Journal keyword(s): galaxies: active - galaxies: jets - instrumentation: high angular resolution - X-rays: individuals: 3C 264 - radiation mechanisms: non-thermal

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 IC 310 rG 03 16 42.9787569912 +41 19 29.615579544   14.3       ~ 267 2
2 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 3937 3
3 QSO B0625-354 BLL 06 27 06.7286533392 -35 29 15.363665088   14.93       ~ 176 1
4 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 1063 1
5 3C 264.0 QSO 11 45 05.00904503 +19 36 22.7409909   14.98 13.97     ~ 585 2
6 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7020 3
7 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4399 3
8 4C 38.41 QSO 16 35 15.49297809 +38 08 04.5005995   18.14 17.97 17.25   ~ 830 1
9 7C 165211.80+395026.00 BLL 16 53 52.21668403 +39 45 36.6088754 14.09 14.15 13.29 8.26   ~ 2108 2
10 NAME Cyg A Sy2 19 59 28.35656837 +40 44 02.0972325   16.22 15.10     ~ 2321 2
11 4C 11.69 QSO 22 32 36.40890093 +11 43 50.9040592   17.75 17.33     ~ 1090 2

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2023.09.27-18:12:57

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