  Fluorine is a fairly good tracer of formation histories of multiple stellar
populations in globular clusters as already revealed by several studies. Large
variations in fluorine abundance in red giant stars of the globular cluster M22
have been recently reported by two different groups. Futhermore, one of these
studies claims that the abundance of fluorine is anti-correlated with sodium
abundances in this cluster, leading to strong conclusions on the chemical
history of M22. To validate this important finding, we re-examine the F
abundance determinations of some of the previously studied stars. We have thus
reanalysed some high-resolution VLT/CRIRES spectra of RGB stars found in M22 in
order to re-estimate their fluorine abundance from the spectral synthesis of
the HF line at 2.336microns. Unlike what has been previously estimated, we show
that only upper limits or doubtful fluorine abundances with large uncertainties
in M22 RGB stars can be derived. This is probably caused by an incorrect
identification of continuum fluctuations as the HF signature combined with a
wrong correction of the stellar radial velocity. Such continuum fluctuations
could be the consequences of telluric residuals that are still present in the
analysed spectra. Therefore, no definitive conclusions on the chemical
pollution caused by the M22 first stellar generation can presently be drawn
from the fluorine content of this cluster.
