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We present amultiwavelength study of IC 1531 (z=0.02564), an extragalactic radio source associated with the γ -ray object 3FGL J0009.9-3206 and classified as a blazar of uncertain type in the Third Fermi-Large Area Telescope AGN catalog (3LAC). A core-jet structure, visible in radio and X-rays, is enclosed within a ~220 kpc wide radio structure. The morphology and spectral characteristics of the kiloparsec jet in radio and X-rays are typical of Fanaroff-Riley type I galaxies. The analysis of the radio data and optical spectrum and different diagnostic methods based on the optical, infrared, and γ -ray luminosities also support a classification as a low-power RG seen at moderate angles (θ = 10°-20°). In the framework of leptonic models, the high-energy peak of the non-thermal nuclear spectral energy distribution can be explained in terms of synchrotron-self-Compton emission from a jet seen at θ ~ 15°. Similarly to other misaligned AGNs detected by Fermi, the required bulk motion is lower (Γ = 4) than the values inferred in BL Lac objects, confirming that, because of the de-boosting of emission from the highly relativistic blazar region, these nearby systems are valuable targets to probe the existence of multiple sites of production of the most energetic emission in the jets.© 2018 The Author(s). ; The research leading to these results has received funding from the European Union's Horizon 2020 Programme under AHEAD project (grant agreement n. 654215). Partial support to this work was provided by the NASA grant AR4-15009X. GM acknowledges the financial support from the UnivEarthS Labex program of Sorbonne Paris Cite (ANR10LABX0023 and ANR11IDEX000502). We thank the anonymous referee for comments and suggestions that helped us to improve the manuscript. TB acknowledges financial contribution from the agreement ASI-INAF n. 2017-14-H.0. MAPT acknowledges support from the Spanish MINECO through grants AYA2012-38491-C02-02 and AYA2015-63939-C2-1-P. AS was supported by NASA contract NAS8-03060 (Chandra X-ray Center). ET acknowledges financial support from ASI-INAF grant 2015-023-R.O. We acknowledge financial support from PRIN INAF 2016. This work has used data supplied by the UK Swift Science Data Centre at the University of Leicester and archival data from the VLA. The NRAO a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

© 2015. The American Astronomical Society. All rights reserved. We present the analysis of the radio jet evolution of the radio galaxy 3C 120 during a period of prolonged γ-ray activity detected by the Fermi satellite between 2012 December and 2014 October. We find a clear connection between the γ-ray and radio emission, such that every period of γ-ray activity is accompanied by the flaring of the millimeter very long baseline interferometry (VLBI) core and subsequent ejection of a new superluminal component. However, not all ejections of components are associated with γ-ray events detectable by Fermi. Clear γ-ray detections are obtained only when components are moving in a direction closer to our line of sight. This suggests that the observed γ-ray emission depends not only on the interaction of moving components with the millimeter VLBI core, but also on their orientation with respect to the observer. Timing of the γ-ray detections and ejection of superluminal components locate the γ-ray production to within ∼0.13 pc from the millimeter VLBI core, which was previously estimated to lie about 0.24 pc from the central black hole. This corresponds to about twice the estimated extension of the broad line region, limiting the external photon field and therefore suggesting synchrotron self Compton as the most probable mechanism for the production of the γ-ray emission. Alternatively, the interaction of components with the jet sheath can provide the necessary photon field to produced the observed γ-rays by Compton scattering. ; his research has been supported by the Spanish Ministry of Science and Innovation grants AYA2010-14844, and AYA2013-40825 P, and by the Regional Government of Andalucia (Spain) grant P09-FQM-4784. This research was partly supported by the Russian Foundation for Basic Research grant 13-02-12103 and by the Academy of Finland project 274477. ; Peer Reviewed