  We draw the multimessenger picture of J1048+7143, a flat-spectrum radio
quasar known to show quasi-periodic oscillations in the $\gamma$-ray regime. We
generate the adaptively-binned Fermi Large Area Telescope light curve of this
source above 168 MeV to find three major $\gamma$-ray flares of the source,
such that all three flares consist of two-two sharp sub-flares. Based on radio
interferometric imaging data taken with the Very Large Array, we find that the
kpc-scale jet is directed towards west, while our analysis of $8.6$-GHz very
long baseline interferometry data, mostly taken with the Very Long Baseline
Array, revealed signatures of two pc-scale jets, one pointing towards east, one
pointing towards south. We suggest that the misalignment of the kpc- and
pc-scale jets is a revealing signature of jet precession. We also analyze the
$5$-GHz total flux density curve of J1048+7143 taken with the Nanshan(Ur) and
RATAN-600 single dish radio telescopes and find two complete radio flares,
slightly lagging behind the $\gamma$-ray flares. We model the timing of
$\gamma$-ray flares as signature of the spin-orbit precession in a supermassive
black hole binary, and find that the binary could merge in the next $\sim
60-80$ years. We show that both the Pulsar Timing Arrays and the planned Laser
Interferometer Space Antenna lack sensitivity and frequency coverage to detect
the hypothetical supermassive black hole binary in J1048$+$7143. We argue that
the identification of sources similar to J1048+7143 plays a key role to reveal
periodic high-energy sources in the distant Universe.
