2021A&A...648A..82P


Query : 2021A&A...648A..82P

2021A&A...648A..82P - Astronomy and Astrophysics, volume 648A, 82-82 (2021/4-1)

Probing the innermost regions of AGN jets and their magnetic fields with RadioAstron. IV. The quasar 3C 345 at 18 cm: Magnetic field structure and brightness temperature.

POTZL F.M., LOBANOV A.P., ROS E., GOMEZ J.L., BRUNI G., BACH U., FUENTES A., GURVITS L.I., JAUNCEY D.L., KOVALEV Y.Y., KRAVCHENKO E.V., LISAKOV M.M., SAVOLAINEN T., SOKOLOVSKY K.V. and ZENSUS J.A.

Abstract (from CDS):


Context. Supermassive black holes in the centres of radio-loud active galactic nuclei (AGN) can produce collimated relativistic outflows (jets). Magnetic fields are thought to play a key role in the formation and collimation of these jets, but the details are much debated.
Aims. We study the innermost jet morphology and magnetic field strength in the AGN 3C 345 with an unprecedented resolution using images obtained within the framework of the key science programme on AGN polarisation of the Space VLBI mission RadioAstron.
Methods. We observed the flat spectrum radio quasar 3C 345 at 1.6GHz on 2016 March 30 with RadioAstron and 18 ground-based radio telescopes in full polarisation mode.
Results. Our images, in both total intensity and linear polarisation, reveal a complex jet structure at 300 µas angular resolution, corresponding to a projected linear scale of about 2pc or a few thousand gravitational radii. We identify the synchrotron self-absorbed core at the jet base and find the brightest feature in the jet 1.5mas downstream of the core. Several polarised components appear in the Space VLBI images that cannot be seen from ground array-only images. Except for the core, the electric vector position angles follow the local jet direction, suggesting a magnetic field perpendicular to the jet. This indicates the presence of plane perpendicular shocks in these regions. Additionally, we infer a minimum brightness temperature at the largest (u, v)-distances of 1.1x1012K in the source frame, which is above the inverse Compton limit and an order of magnitude larger than the equipartition value. This indicates locally efficient injection or re-acceleration of particles in the jet to counter the inverse Compton cooling or the geometry of the jet creates significant changes in the Doppler factor, which has to be >11 to explain the high brightness temperatures.

Abstract Copyright: © F. M. Pötzl et al. 2021

Journal keyword(s): radio continuum: galaxies - galaxies: active - galaxies: jets - galaxies: magnetic fields - quasars: individual: 3C 345

VizieR on-line data: <Available at CDS (J/A+A/648/A82): list.dat fits/*>

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 - 2024
#notes
1 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 4017 3
2 7C 064253.00+445430.00 QSO 06 46 32.02599653 +44 51 16.5901185   19.57 18.49 18.64   ~ 348 1
3 8C 0716+714 BLL 07 21 53.4482942664 +71 20 36.363846516   15.5 15.50 14.27   ~ 1303 1
4 QSO J0854+2006 BLL 08 54 48.8749846272 +20 06 30.639583620   15.91 15.43 15.56   ~ 2344 1
5 Ton 599 Sy1 11 59 31.83391383 +29 14 43.8268224   14.80 14.41 17.652 13.39 ~ 927 1
6 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 5811 1
7 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7221 3
8 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4351 2
9 NAME Her B Sy1 16 42 58.80997043 +39 48 36.9939552   16.81 16.59 16.84   ~ 1729 2
10 QSO B2136+1410 QSO 21 39 01.30926630 +14 23 35.9921774     18.90 18.22   ~ 248 1
11 NAME BL Lac BLL 22 02 43.2913536816 +42 16 39.979416792   15.66 14.72     ~ 2265 1

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