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Abridged - Stars with ZAMS masses between 140 and $260 M_\odot$ are thoughtto explode as pair-instability supernovae (PISNe). During their thermonuclearrunaway, PISNe can produce up to several tens of solar masses of radioactivenickel, resulting in luminous transients similar to some superluminoussupernovae (SLSNe). Yet, no unambiguous PISN has been discovered so far.SN2018ibb is a H-poor SLSN at $z=0.166$ that evolves extremely slowly comparedto the hundreds of known SLSNe. Between mid 2018 and early 2022, we monitoredits photometric and spectroscopic evolution from the UV to the NIR with 2-10mclass telescopes. SN2018ibb radiated $>3\times10^{51} \rm erg$ during itsevolution, and its bolometric light curve reached $>2\times10^{44} \rmerg\,s^{-1}$ at peak. The long-lasting rise of $>93$ rest-frame days implies along diffusion time, which requires a very high total ejected mass. The PISNmechanism naturally provides both the energy source ($^{56}$Ni) and the longdiffusion time. Theoretical models of PISNe make clear predictions for theirphotometric and spectroscopic properties. SN2018ibb complies with most tests onthe light curves, nebular spectra and host galaxy, potentially all tests withthe interpretation we propose. Both the light curve and the spectra require25-44 $M_\odot$ of freshly nucleosynthesised $^{56}$Ni, pointing to theexplosion of a metal-poor star with a He-core mass of 120-130 $M_\odot$ at thetime of death. This interpretation is also supported by the tentative detectionof [Co II]$\lambda$1.025$\mu$m, which has never been observed in any other PISNcandidate or SLSN before. Powering by a central engine, such as a magnetar or ablack hole, can be excluded with high confidence. This makes SN2018ibb by farthe best candidate for being a PISN, to date.

1100 days in the life of the supernova 2018ibb -- The best pair-instability supernova candidate, to date