  We report on XMM-Newton spectroscopy of the low-luminosity active galaxies
(LLAGN) M81 and NGC4579 both of which have known black hole masses and
well-sampled spectral energy distributions (SED). The iron Kalpha line profiles
from both the LLAGN can be described in terms of two components - a narrow line
at 6.4 keV and a moderately broad line (FWHM = 20000 km/s) arising from highly
ionized, He-like or H-like species (E \sim 6.8 keV). We interpret the broad
lines arising from an accretion disk the inner edge of which is restricted to
large radii (r_{in} \sim 100 r_g). However, the Eddington ratio, {L}/{L_{Edd}},
of these sources, is 3 - 4 orders of magnitude lower than that required to
photo-ionize a cold disk to He-like iron. We suggest that the lines can be
explained as collisionally ionized X-ray lines arising from the transition
region between a hot (radiatively inefficient) flow in the inner regions and a
cold disk outside r \sim 100r_g. The accretion flow geometry probed by our
XMM-Newton observations is consistent with the truncated disk models proposed
to explain the SED of LLAGNs.
