  NGC 2419 is the most distant massive globular cluster in the outer Galactic
halo. It is unusual also due to the chemical peculiarities found in its red
giant stars in recent years. We study the stellar population of this unusual
object using spectra obtained at the 1.93-m telescope of the Haute-Provence
Observatory. At variance with commonly used methods of high-resolution
spectroscopy applicable only to bright stars, we employ spectroscopic
information on the integrated light of the cluster. We carry out population
synthesis modeling of medium-resolution spectra using synthetic stellar
atmosphere models based on a theoretical isochrone corresponding accurately to
the observed color-magnitude diagram. We study the influence of non-Local
Thermodynamic Equilibrium for some chemical elements on our results. The
derived age (12.6 Gyr), [Fe/H]=-2.25 dex, helium content Y=0.25, and abundances
of 12 other chemical elements are in a good qualitative agreement with
published high-resolution spectroscopy estimates for red giant members in the
cluster. On the other hand, the derived element abundance, [alpha/Fe]=0.13 dex
(the mean of [O/Fe], [Mg/Fe] and [Ca/Fe]), differs from the published one
([alpha/Fe] =0.4 dex) for selected red giants in the cluster and may be
explained by a large dispersion in the alpha-element abundances recently
discovered in NGC2419. We suggest that studies of the {\it integrated} light in
the cluster using high-resolution spectrographs in different wavelength regions
will help to understand the nature of these chemical anomalies.
