  Low-luminosity AGNs are perceived to be radio loud and devoid of a ``big blue
bump'', indicating a transition from a radiatively efficient, geometrically
thin, accretion disc in high-luminosity AGNs, to a geometrically thick,
radiatively inefficient accretion flow at low luminosities and accretion rates.
I revisit the issue of the spectral energy distributions (SEDs) of
low-luminosity AGNs using recently published, high-angular-resolution data at
radio, UV, and X-ray wavelengths, for a sample of 13 nearby galaxies with LINER
nuclei. I show that, contrary to common wisdom, low-luminosity AGNs have
significant nonstellar UV flux, and UV/X-ray luminosity ratios similar, on
average, to those of Seyfert 1 nuclei ~10^4 times more luminous. The alpha_ox
index that quantifies this ratio is in the range between -0.8 to -1.4, and is
below the extrapolation to low luminosities of the relation between alpha_ ox
and UV luminosity observed at higher luminosities. In terms of radio loudness,
most of the LINERs are indeed radio loud (or sometimes even ``super radio
loud'') based on their radio/UV luminosity ratios, when compared to the most
luminous quasars. However, the entire distribution of radio loudness has been
shown to shift to higher radio/UV ratios at low AGN luminosities. In the
context of this global shift, some LINERs (the majority) can be considered
radio quiet, and some (from among those with black hole masses >~10^8.5 M_sun)
are radio loud. The SEDs of low-luminosity (~10^40 erg/s) AGNs are thus quite
similar to those of Seyferts up to luminosities of ~10^44erg/s, and there is no
evidence for a sharp change in the SEDs at the lowest luminosities. Thin AGN
accretion discs may therefore persist at low accretion rates, in analogy to
some recent findings for Galactic stellar-mass accreting black holes.
