  It is well known that the bright and remote Galactic globular cluster NGC2419
has a very peculiar structure. In particular its half-light radius is
significantly larger than that of ordinary globular clusters of similar
luminosity, being as large as that of the brightest nuclei of dwarf elliptical
galaxies. In this context it is particularly worth to check the reliability of
the existing surface brightness profiles for this cluster and of the available
estimates of its structural parameters. Combining different datasets I derive
the surface brightness profile going from the cluster center out to ~ 480
arcsec, i.e. ~25 core radii. (Abridged). The newly obtained surface brightness
profile 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=0.32
arcmin, mu_V(0)=19.55 and C=1.35. Also new independent estimates of the total
integrated 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 structure
of NGC2419 is now reliably constrained by (at least) two fully independent
observational profiles that are in good agreement one with the other. Also the
overall agreement between structural parameters independently obtained by
different authors is quite satisfying.
