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The bright X-ray jet in RGB J1512+020A: evidence for a third radiative component?

Presentation #401.04 in the session Active Galactic Nuclei II.

Published onJul 01, 2023
The bright X-ray jet in RGB J1512+020A: evidence for a third radiative component?

The radiative processes responsible of the high-energy emission of extragalactic jets remain after many years still a puzzle. X-ray observations at sub-arcsecond resolution have allowed us to probe the structure of extragalactic jets and investigate the sites, knots and hotspots, where efficient particle acceleration takes place. Recent studies of jets at low- and high-redshift return a complex picture, suggesting that different processes could be at work and their relevance determined by the physical parameters of each jet. Significant progress in the last years has been made by improving the quality of the data in terms of multi-wavelength coverage, angular resolution and sensitivity, leading to meaningful comparison with state-of-art RMHD simulations.

We present an X-ray and multi-wavelength study of a powerful, relativistic jet in the radio quasar RGB J1512+020A. The jet is among the brightest X-ray jets at low redshift (z<0.5) and has a relatively high jet-to-core X-ray flux ratio (~0.26), similar to high-z jets. Its main features are characterized by large X-ray-to-radio luminosity ratios (LX/Lr up to ~50) in comparison with knots and hotspots of other known jets. For two of the jet’s components, archival ALMA data have unveiled a turnover of the radio synchrotron spectrum at ~460 GHz. This implies that the optical emission visible in DECaLS images is either due to the same radiative component responsible for the X-ray emission or to a third radiative component of unknown nature. We discuss the different radiative scenarios and their implications for the jet physics.

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