  PSO J334.2028+1.4075 (PSO J334) is a luminous quasar located at redshift
z=2.06. The source gained attention when periodic flux density variations were
discovered in its optical light curve. These variations were initially
interpreted as the variability due to the orbital motion of a supermassive
black hole binary (SMBHB) residing in a single circumbinary accretion disk.
However, subsequent multiwavelength observations provided evidence against the
binary hypothesis as no optical periodicity was found on extended time
baselines. On the other hand, detailed radio analysis with the Karl G. Jansky
Very Large Array (VLA) and the Very Long Baseline Array (VLBA) revealed a
lobe-dominated quasar at kpc scales, and possibly a precessing jet, which could
retain PSO J334 as a binary SMBH candidate. We aim to study both the large- and
small-scale radio structures in PSO J334 to provide additional evidence for or
against the binary scenario. We observed the source at 1.7 GHz with the
European Very Long Baseline Interferometry Network (EVN), and at 1.5 and 6.2
GHz with the VLA, at frequencies that complement the previous radio
interferometric study. Our images reveal a single component at parsec scales
slightly resolved in the southeast-northwest direction and a lobe-dominated
quasar at kiloparsec scales with a complex structure. The source morphology and
polarization in our VLA maps suggest that the jet is interacting with dense
clumps of the ambient medium. While we also observe a misalignment between the
inner jet and the outer lobes, we suggest that this is due to the restarted
nature of the radio jet activity and the possible presence of a warped
accretion disk rather than due to the perturbing effects of a companion SMBH.
Our analysis suggests that PSO J334 is most likely a jetted AGN with a single
SMBH, and there is no clear evidence of a binary SMBH system in its central
engine.
