  XMM-Newton observations aimed at determining for the first time the
broad-band X-ray properties of the faint high galactic latitude Intermediate
Polar UU Col are presented. We performed X-ray timing analysis in different
energy ranges of the EPIC cameras which reveals the dominance of the 863s white
dwarf rotational period. The spin pulse is strongly energy dependent. Weak
variabilities at the beat 935s and at the 3.5hr orbital periods are also
observed, but the orbital modulation is detected only below 0.5keV.
Simultaneous UV and optical photometry shows that the spin pulse is anti-phased
with respect to the hard X-rays. Analysis of the EPIC and RGS spectra reveals
the complexity of the X-ray emission, being composed of a soft 50eV black--body
component and two optically thin emission components at 0.2keV and 11keV
strongly absorbed by dense material with an equivalent hydrogen column density
of 10**(23)cm**(-2) partially (50%) covering the X-ray source. The complex
X-ray and UV/optical temporal behaviour indicates that accretion occurs
predominantly (80%) via a disc with a partial contribution (20%) directly from
the stream. The main accreting pole dominates at high energies whilst the
secondary pole mainly contributes in the soft X-rays and at lower energies. The
bolometric flux ratio of the soft-to-hard X-ray emissions is found to be
consistent with the prediction of the standard accretion shock model. We find
the white dwarf in UU Col accretes at a low rate and possesses a low magnetic
moment. It is therefore unlikely that UU Col will evolve into a moderate field
strength Polar, which leaves the soft X-ray Intermediate Polars a still
enigmatic small group of magnetic Cataclysmic Variables.
