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Active galactic nuclei (AGN) accreting at rates close to the Eddington limitcan host radiatively driven mildly relativistic outflows. Some of these X-rayabsorbing but powerful outflows may produce strong shocks resulting in asignificant non-thermal emission. This outflow-driven radio emission may bedetectable in the radio-quiet quasar PDS 456 since it has a bolometricluminosity reaching the Eddington limit and a relativistic wide-aperture X-rayoutflow with a kinetic power high enough to quench the star formation in itshost galaxy. To investigate this possibility, we performed very-long-baselineinterferometric (VLBI) observations of the quasar with the European VLBINetwork (EVN) at 5 GHz. The EVN image with the full resolution reveals twofaint and diffuse radio components with a projected separation of about 20 pcand an average brightness temperature of around two million Kelvin. In relationto the optical sub-mas-accuracy position measured by the Gaia mission, the twocomponents are very likely on opposite sides of an undetected radio core. TheVLBI structure at the deca-pc scale can thus be either a young jet or abidirectional radio-emitting outflow, launched in the vicinity of a stronglyaccreting central engine. Two diffuse components at the hecto-pc scale, likelythe relic radio emission from the past AGN activity, are tentatively detectedon each side in the low-resolution EVN image.

A radio structure resolved at the deca-parsec scale in radio-quiet quasar PDS 456 with an extremely powerful X-ray outflow