Volume 604, August 2017
|Number of page(s)||9|
|Published online||22 August 2017|
Probing the innermost regions of AGN jets and their magnetic fields with RadioAstron
II. Observations of 3C 273 at minimum activity⋆
1 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
2 INAF–Istituto di Radioastronomia, via Piero Gobetti, 101, 40129 Bologna, Italy
3 INAF–Istituto di Astrofisica e Planetologia Spaziali, via Fosso del Cavaliere, 100, 00133 Rome, Italy
4 Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
5 Institut für Experimentalphysik, Universität Hamburg, Luruper Chaussee 149, 22 761 Hamburg, Germany
6 Astro Space Center of Lebedev Physical Institute, Profsoyuznaya 84/32, 117997 Moscow, Russia
7 IAASARS, National Observatory of Athens, Vas. Pavlou & I. Metaxa, 15236 Penteli, Greece
8 Sternberg Astronomical Institute, Moscow State University, Universitetskii pr. 13, 119992 Moscow, Russia
9 Institute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA
10 Astronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, Russia
11 Deutsches GeoForschungsZentrum GFZ, Telegrafenberg, 14473 Potsdam, Germany
12 Aalto University Metsähovi Radio Observatory, Metsähovintie 114, 02540 Kylmälä, Finland
13 Aalto University Department of Electronics and Nanoengineering, PL 15500, 00076 Aalto, Finland
14 Korea Astronomy and Space Science Institute, 776 Daedeok-daero, Yuseong-gu, 34055 Daejeon, Republic of Korea
15 Korea University of Science and Technology, 217 Gajeong-ro, Yuseong-gu, 34113 Daejeon, Republic of Korea
16 Observatori Astronómic, Universitat de València, Parc Científic, C. Catedrático José Beltrán 2, 46980 Paterna, València, Spain
17 Departament d’Astronomia i Astrofísica, Universitat de València, 46100 Burjassot, València, Spain
18 Moscow Institute of Physics and Technology, Dolgoprundy, Institutsky per., 9, Moscow region, 141700, Russia
Received: 22 May 2017
Accepted: 27 June 2017
Context. RadioAstron is a 10 m orbiting radio telescope mounted on the Spektr-R satellite, launched in 2011, performing Space Very Long Baseline Interferometry (SVLBI) observations supported by a global ground array of radio telescopes. With an apogee of ~350 000 km, it is offering for the first time the possibility to perform μas-resolution imaging in the cm-band.
Aims. The RadioAstron active galactic nuclei (AGN) polarization Key Science Project (KSP) aims at exploiting the unprecedented angular resolution provided by RadioAstron to study jet launching/collimation and magnetic-field configuration in AGN jets. The targets of our KSP are some of the most powerful blazars in the sky.
Methods. We present observations at 22 GHz of 3C 273, performed in 2014, designed to reach a maximum baseline of approximately nine Earth diameters. Reaching an angular resolution of 0.3 mas, we study a particularly low-activity state of the source, and estimate the nuclear region brightness temperature, comparing with the extreme one detected one year before during the RadioAstron early science period. We also make use of the VLBA-BU-BLAZAR survey data, at 43 GHz, to study the kinematics of the jet in a ~1.5-yr time window.
Results. We find that the nuclear brightness temperature is two orders of magnitude lower than the exceptionally high value detected in 2013 with RadioAstron at the same frequency (1.4 × 1013 K, source-frame), and even one order of magnitude lower than the equipartition value. The kinematics analysis at 43 GHz shows that a new component was ejected ~2 months after the 2013 epoch, visible also in our 22 GHz map presented here. Consequently this was located upstream of the core during the brightness temperature peak. Fermi-LAT observations for the period 2010−2014 do not show any γ-ray flare in conjunction with the passage of the new component by the core at 43 GHz.
Conclusions. These observations confirm that the previously detected extreme brightness temperature in 3C 273, exceeding the inverse Compton limit, is a short-lived phenomenon caused by a temporary departure from equipartition. Thus, the availability of interferometric baselines capable of providing μas angular resolution does not systematically imply measured brightness temperatures over the known physical limits for astrophysical sources.
Key words: galaxies: active / galaxies: jets / galaxies: magnetic fields
The reduced image (FITS file) is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/604/A111
© ESO, 2017
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.