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We present very-long-baseline interferometry (VLBI) observations of acontinuum radio source potentially associated with the fast radio burst sourceFRB 20190520B. Using the European VLBI network (EVN), we find the source to becompact on VLBI scales with an angular size of $<2.3$ mas ($3\sigma$). Thiscorresponds to a transverse physical size of $<9$ pc (at the $z=0.241$ redshiftof the host galaxy), confirming it to be an FRB persistent radio source (PRS)like that associated with the first-known repeater FRB 20121102A. The PRS has aflux density of $201 \pm 34 \rm{\mu Jy}$ at 1.7 GHz and a spectral radioluminosity of $L_{1.7 \rm GHz} = (3.0 \pm 0.5) \times 10^{29}\,\mathrm{ergs^{-1} Hz^{-1}}$ (also similar to the FRB 20121102A PRS). Comparing to previouslower-resolution observations, we find that no flux is resolved out onmilliarcsecond scales. We have refined the PRS position, improving itsprecision by an order of magnitude compared to previous results. We also reportthe detection of a FRB 20190520B burst at 1.4 GHz and find the burst positionto be consistent with the PRS position, at $\lesssim20$ mas. This stronglysupports their direct physical association and the hypothesis that a singlecentral engine powers both the bursts and the PRS. We discuss the model of amagnetar in a wind nebula and present an allowed parameter space for its ageand the radius of the putative nebula powering the observed PRS emission.Alternatively, we find that an accretion-powered 'hypernebula' model also fitsour observational constraints.

Constraints on the persistent radio source associated with FRB 20190520B using the European VLBI Network