  We use the data from a recent, 100 ksec XMM-Newton observation of the Narrow
Line Seyfert 1 galaxy Ark 564 to obtain its time average, X-ray spectrum. The
3-11 keV spectrum is well fitted by a power-law of slope 2.43. We detect a weak
(equivalent width ~80 eV) emission line at ~6.7 keV, which implies emission
from ionized iron. There is no compelling evidence for significant broadening
of the line.We also detect a possible Doppler shifted absorption line at 8.1
keV. At energies lower than 2 keV, the spectrum is dominated by a smooth soft
excess component which can be well fitted either by a two black body components
(kT~0.15 and 0.07 keV) or by a black body plus a relativistically blurred
photoionized disc reflection model. We detect a broad, shallow flux deficit in
the 0.65-0.85 keV band, reminiscent of the iron unresolved transition array
(UTA) features. We do not detect neither a strong absorption edge around 0.7
keV nor an emission line around 1 keV. The soft excess emission is consistent
with being reflected emission from a geometrically flat disc, with solar
abundances, illuminated by an isotropic source. The weakness of the iron line
emission can be explained by relativistic blurring. The UTA feature implies the
presence of warm material with a column density of 2-5*10^{20} cm^{-2}. If the
absorption line at 8.1 keV corresponds to FeXXVI Kalpha, it suggests the
presence of a highly ionized absorbing material with N_H > 10^{23} cm^{-2},
outflowing at a high velocity of ~0.17c.
