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It is well known that the bright and remote Galactic globular cluster NGC2419has a very peculiar structure. In particular its half-light radius issignificantly larger than that of ordinary globular clusters of similarluminosity, being as large as that of the brightest nuclei of dwarf ellipticalgalaxies. In this context it is particularly worth to check the reliability ofthe existing surface brightness profiles for this cluster and of the availableestimates of its structural parameters. Combining different datasets I derivethe surface brightness profile going from the cluster center out to ~ 480arcsec, i.e. ~25 core radii. (Abridged). The newly obtained surface brightnessprofile is in excellent agreement with that provided by Trager, King &Djorgovski for r>= 4 arcsec; it is best fitted by a King model having r_c=0.32arcmin, mu_V(0)=19.55 and C=1.35. Also new independent estimates of the totalintegrated V magnitude (V_t=10.47 +/- 0.07) and of the half-light radius(r_h=0.96 arcmin +/- 0.2 arcmin) have been obtained. (Abridged). The structureof NGC2419 is now reliably constrained by (at least) two fully independentobservational profiles that are in good agreement one with the other. Also theoverall agreement between structural parameters independently obtained bydifferent authors is quite satisfying.

The surface brightness profile of the remote cluster NGC 2419