  We here report on the multiwavelength study which led us to the
identification of X-ray source IGR J16194-2810 as a new Symbiotic X-ray Binary
(SyXB), that is, a rare type of Low Mass X-ray Binary (LMXB) composed of a
M-type giant and a compact object. Using the accurate X-ray position allowed by
Swift/XRT data, we pinpointed the optical counterpart, a M2 III star. Besides,
the combined use of the spectral information afforded by XRT and INTEGRAL/IBIS
shows that the 0.5-200 keV spectrum of this source can be described with an
absorbed Comptonization model, usually found in LMXBs and, in particular, in
SyXBs. No long-term (days to months) periodicities are detected in the IBIS
data. The time coverage afforded by XRT reveals shot-noise variability typical
of accreting Galactic X-ray sources, but is not good enough to explore the
presence of X-ray short-term (seconds to hours) oscillations in detail. By
using the above information, we infer important parameters for this source such
as its distance (about 3.7 kpc) and X-ray luminosity (about 1.4e35 erg/s in the
0.5-200 keV band), and we give a description for this system (typical of SyXBs)
in which a compact object (possibly a neutron star) accretes from the wind of
its M-type giant companion. We also draw some comparisons between IGR
J16194-2810 and other sources belonging to this subclass, finding that this
object resembles SyXBs 4U 1700+24 and 4U 1954+31.
